System1Orbit1Begin Later observations did not indicate that there was any need to change these elements. (W.E. Harper, Publ. Dom. Astrophys. Obs., 6, 208, 1935). System1Orbit1End System2Orbit1Begin The orbit was assumed to be circular, and the orbital elements are based on measures of two lines of He II seen in absorption. The velocities show a large scatter, and Hutchings offers several alternative solutions based on different emission lines and different numbers of plates. The system resembles some X-ray binaries and may contain a collapsed component. The primary generates a strong stellar wind, and it is unclear how far any of the spectral lines represent the true orbital velocity of the star. P.S. Conti and J.-M. Vreux (Astrophys. J., 228, 220, 1979) do not confirm the period found by Hutchings and question whether the star's velocity is genuinely variable. System2Orbit1End System3Orbit1Begin The new elements, based on photoelectric velocity measurements, should certainly be preferred over those originally determined by W.H. Christie (Astrophys. J., 77, 310, 1933), especially since the new observations lead to an improved value of the period. The agreement between the two values of K is acceptable. Beavers and Salzer applied the test devised by Lucy & Sweeney to the eccentricity and concluded that, although small, it is genuine. The star varies in light by about 0.2 m in V in a way that suggests it is an eclipsing variable. (R.D. Lines & D.S. Hall, Inf. Bull. Var. Stars, No. 2013, 1981). The shape of the light curve suggests that at least one component is distorted -- unusual in a system of such long period. Attempts to detect the secondary spectrum have so far failed. System3Orbit1End System4Orbit1Begin Earlier investigations by R.H. Baker (Publ. Allegheny Obs., 1, 22, 1908), H. Ludendorff (Astron. Nachr., 178, 23, 1908), O. Kohl (Astron. Nachr., 262, 472, 1937), W.J. Luyten, O. Struve and W.W. Morgan (Publ. Yerkes Obs., 7, Pt. IV, 1, 1939) and J.A. Pearce (Publ. Am. Astron. Soc., 9, 16, 1936) gave a range in K from 27 km/s to 34 km/s. Aikman obtained new, high-dispersion observations of this mercury-manganese star; the orbital elements given are based on his new observations and the older ones. No new elements have been published since, but K.D. Rakos, H. Jenker and J. Wood (Astron. Astrophys. Supp., 43, 209, 1981) find evidence for light variations in the ultraviolet with a period of about 0.96d and velocity variations (measured from three Si II lines near lambda = 1300 A) of up to 10 km/s in a period of about 0.13 day. S.J. Adelman and D.M. Pyper (Astron. Astrophys., 118, 313, 1983) also suspect some light variations at visual and near ultraviolet wavelengths. Considering these results, and a possibility that V0 may be varying, we believe that the assessment given for this orbit in the Seventh Catalogue may have been optimistic. (Note also a misprint in Aikman's paper where 9.6 km/s is given as the most recent value of V0 rather than -9.6 km/s) Petrie's (II) value of Delta m = 1.35m is probably affected by the lambda 4479 component of the Mg II line and is an underestimate. The star is the brighter component of A.D.S. 94; the companion is 11.4m at 75". System4Orbit1End System5Orbit1Begin The orbital elements are described as `preliminary' by Hube and Gulliver themselves. Curchod and Hauck classify the metallic-lined spectrum as A3 from the K line and F0 from the metal lines. Hube and Gulliver suggest that a search for eclipses might be worthwhile. System5Orbit1End System6Orbit1Begin The new results by Andersen et al. represent a major advance in our understanding of this system. The velocity-curve of the secondary component (the K star) is now well determined by photoelectric measurements -- much better so than the d quality suggests. The value of V0 is derived from measures of the secondary component, which also leaves little doubt that the true orbit is circular (the epoch is the time of primary minimum and the period is variable). Earlier work by O. Struve (Astrophys. J., 99, 89, 1944) and by C.J. van Houten (Astron. Astrophys., 97, 46, 1981) is now superseded. Andersen's own determination of K2 from spectrograms (Publ. Astron. Soc. Pacific, 85, 191, 1973) is surprisingly closely confirmed. There is now general agreement that the A-type spectrum is that of a shell, not that of the hotter star, whose true spectral type was estimated from UV observations to be B7 (M. Plavec, J.L. Weiland and R.H. Koch, Astrophys. J., 256, 206, 1982). Andersen et al. have also analyzed the photometric observations, particularly those of C.-Y. Shao (Astron. J., 72, 480, 1967). They find an orbital inclination of about 79deg and a light ratio in V (K star brighter) of 1.7. The system appears to be semi-detached. E.F. Guinan, S. Tomcyzk and D.J. Turnshek (Publ. Astron. Soc. Pacific, 95, 364, 1983) confirm that the H-alpha emission comes from a region larger than either star. The faint companion (V = 11.68m) about 17" away appears not to be physically related to the binary system. System6Orbit1End System7Orbit1Begin This is a cataclysmic variable of the Z Cam type. Even the period is uncertain -- an alternative value of 0.149 day is quite possible -- and the elements must be considered provisional, although K1 and V0 would be approximately the same whichever period is chosen. Co-adding individual spectra gives a somewhat lower value of K1 (92 km/s) and an appreciably better fit to the velocity-curve. A circular orbit was assumed. System7Orbit1End System8Orbit1Begin This is the first complete investigation of the system since the original one by J.A. Pearce (Mon. Not. Roy. Astron. Soc., 92, 877, 1932) although O. Struve and M. Rudkjobing (Astrophys. J., 108, 537, 1948) and J. Sahade (Publ. Goethe Link Obs., No. 69, 1967) questioned the visibility of the secondary spectrum seen by Pearce. In consequence, the very high masses found for this star by the last-named investigator have long been doubted. Hutchings and Bernard base their analysis on only eleven spectrograms, but since these are well distributed around the orbital period and the results for the primary spectrum agree well with Pearce's, we can probably assume that the orbit of the brighter component is well known. They believe that Pearce measured lines of Fe II in the neighbourhood of the K line and misidentified these as the secondary component of that line. They find possible traces of a weak secondary component in the helium lines which indicate a mass-ratio near unity and a magnitude difference (in the photographic region of the spectrum) of about 1.5mag. Corresponding minimum masses are around 15 MSol for each component. The epoch is T0. The secondary may be of earlier spectral type and still close to the main sequence. There is evidence for a stellar wind associated with the primary star. System8Orbit1End System9Orbit1Begin The spectral type is A2 from the K line and F2 from the metallic lines. System9Orbit1End System10Orbit1Begin An earlier investigation by E. MacCormack (Astrophys. J., 80, 120, 1934) gives elements in good agreement with Cester's except for a small eccentricity. The light-curve obtained by N.L. Magalashvili and Ya.I. Kumsishvili (Bulletin Abastumani Obs., No. 22, 3, 1958) shows a displaced secondary minimum which suggests an appreciable eccentricity of the orbit. K.J. Johnston (Astrophys. J., 176, 455, 1971) has confirmed Cester's suggestion that the light variation is due solely to the ellipticities of the two nearly identical components. He found i=38 deg and suggested there might be rapid apsidal rotation. New spectroscopic observations are being obtained by C.T. Bolton to test this possibility. The epoch given in the Catalogue is T0. The star is the brighter component of A.D.S. 191; companion 7.8m at 12". Reference: B.Cester, Trieste Contr.,, No. 291, 1959 System10Orbit1End System11Orbit1Begin System11Orbit1End System12Orbit1Begin Earlier investigations were made by W.S. Adams and G. Stromberg (Astrophys. J., 47, 329, 1918), J.A. Pearce (Publ. Dom. Astrophys. Obs., 3, 275, 1926), and O. Struve and H.G. Horak (Astrophys. J., 110, 447, 1949). All available observations have also been discussed by G. Mannino (Asiago Contr., No. 103, 1959) and A. Krancj (Publ. Bologna Univ. Obs., 7, No. 14, 1960). An excellent three-colour (UBV) light-curve was obtained by R.H. Koch (Astron. J., 65, 127, 1960). These and an earlier light-curve obtained by F.B. Wood (Astrophys. J., 108, 28, 1948) were analyzed by J.B. Hutchings and G. Hill (Astrophys. J., 167, 137, 1971) by their method of light-curve synthesis. They found the orbital inclination to be 56 deg, the eclipses being grazing and most of the light variation being the result of distortion of the stars. Abhyankar finds evidence for different mean velocities for each component, raising the question how far the velocities derived for the secondary star can be assumed to result from its orbital motion. If the secondary spectrum does arise from the secondary star then the system does not conform to the mass-luminosity relation. Petrie(II) found Delta m = 0.78, a greater difference than would be expected if the mass-ratio is 0.85, as found by Abhyankar. Hutchings and Hill confirm this value of the mass-ratio (they find 0.81) and speculate that the system is close to a rapid phase of mass transfer. The orbit of the primary is well determined in Abhyankar's work, although his value of K1 is different from those found earlier. He believes there is some evidence for apsidal rotation with a period of about 70 years. System12Orbit1End System13Orbit1Begin Light-curves in B and V have been published by R.M. Williamon, T.F. Collins and K.-Y. Chen (Astron. Astrophys. Supp., 34, 207, 1978). The epoch is the time of primary minimum. Hilditch and King were unable to satisfy the light-curves with the same value of the mass-ratio as obtained from the velocity-curves; the light-curves give q=0.27. Subject to uncertainties arising from this, Hilditch and King find the masses, radii and luminosities of the two stars to be, respectively: 1.9 MSol and 0.7 MSol ; 2.1 RSol and 1.3 RSol ; and 8.95 LSol and 3.47 LSol. The orbital inclination is close to 80 deg. Different luminosity ratios would be found at the two quadratures from the relative intensity of the spectra. System13Orbit1End System14Orbit1Begin Although the observations are spread over an interval of nearly sixty years, no evidence for apsidal motion has been detected. The original paper gives spectrophotometric information and an estimate of rotational velocities (75 km/s). The study serves as an example of what can be learned when old plates are measured by modern cross-correlation methods. System14Orbit1End System15Orbit1Begin It is, perhaps, surprising that this relatively bright, short-period system has not attracted more attention from spectroscopists. Plaskett's discussion remains the only complete one. Luyten rediscussed the observations and derived a small eccentricity: photometric observations, however, reveal that any displacement of the secondary minimum is very small. Observations by J. Sahade and O. Struve (Astrophys. J., 102, 480, 1945) agree with Plaskett's curve but show a distinct rotational disturbance. Those investigators could not confirm Plaskett's detection of the secondary spectrum (K2=150 km/s) -- hardly surprising since modern photometry indicates a light-ratio in V of about 0.05 (K. W lodarczyk, Acta Astron., 34, 47, 1984). Plaskett's zero of phase is based on a time of primary minimum given by R.J. McDiarmid (Princeton Obs. Contr., No. 7, 1924). The value given in the Catalogue is one-quarter of a period later and corresponds to the time of maximum positive velocity. There is evidence, however, that the period changes (A.C. de Landtsheer, Astron. Astrophys. Supp., 52, 213, 1983). De Landtsheer also presents an infrared light-curve in that paper. In addition, with P.S. Mulder (Astron. Astrophys., 127, 297, 1983) he reports on IUE observations of the system, which failed to show any trace of circumstellar matter. A discussion of the system's possible evolution has been published by J.P. de Greve, A.C. de Landtsheer and W. Packet (Astron. Astrophys., 142, 367, 1985). W lodarczyk (op.cit.) finds i=80 deg, in good agreement with earlier discussions of the light-curve (C.M. Huffer & Z. Kopal, Astrophys. J., 114, 297, 1951 and J. Papousek, Bull. Astron. Inst. Csl, 25, 152, 1974). The spectral type given for the secondary component is derived from W lodarczyk's solution. System15Orbit1End System16Orbit1Begin Original observations and elements by G.H. Tidy (Publ. David Dunlap Obs., 1, 191, 1940). Tanner showed that the period adopted by Tidy was incorrect. The epoch is T0 as defined by Sterne. Lucy & Sweeney regard the orbit as circular. System16Orbit1End System17Orbit1Begin Period uncertain by up to one day. Epoch is arbitrary zero of phase. Star is brighter component of A.D.S. 328: companion 8.0m at 0.2", but star appeared single in 1953 (I.D.S.). System17Orbit1End System18Orbit1Begin Secondary spectrum seen and measured with difficulty. System18Orbit1End System19Orbit1Begin Hube calls attention to the large mass-function and suggests that the system may prove to be eclipsing. Earlier reports of variability, however, have not been confirmed. Some authors have classified the star as an Si Ap star, but Hube finds no evidence of peculiarity. J. Zverko (Bull. Astron. Inst. Csl, 30, 372, 1979) published an abundance analysis and concluded that silicon is slightly overabundant. System19Orbit1End System20Orbit1Begin System20Orbit1End System21Orbit1Begin Residuals are small, but maximum of velocity-curve is not well defined. H.L. Alden (Publ. Am. Astron. Soc., 9, 31, 1937) gives an astrometric orbit, i=110.4 deg, a=0.068", omega=3 deg. System21Orbit1End System22Orbit1Begin The orbit is based exclusively on photoelectric measurements of radial velocity, although earlier photographic measurements revealed the variability (R.E. Wilson and A.H. Joy, Astrophys. J., 111, 221, 1950; J.F. Heard, Publ. David Dunlap Obs., 2, 105, 1956). A circular orbit was adopted after an application of Bassett's test (Observatory, 98, 122, 1978) showed the small eccentricity to be statistically insignificant. The epoch is T0. Griffin suggests that the star may be fainter than the H.D. magnitude given in the Catalogue. System22Orbit1End System23Orbit1Begin System23Orbit1End System24Orbit1Begin This Cepheid variable is also a spectroscopic binary and a member of the cluster N.G.C. 129. System24Orbit1End System25Orbit1Begin This is another supergiant member of the cluster N.G.C. 129. System25Orbit1End System26Orbit1Begin Star is 1' S.E. of B.D. +61 deg 113. Period is accurately known from light-curve. I.M. Levitt (Flower Reprint, No. 76, 1949) found from visual observations i=67 deg and the light-ratio to be about 0.75. System26Orbit1End System27Orbit1Begin 13 Cet (A.D.S. 490) is a well-known triple system. Luyten estimates V0 for the whole system is 11.0 km/s. Earlier investigations are by J.S. Paraskevopoulos (Astrophys. J., 52, 110, 1920) and A. Pogo (Astrophys. J., 68, 116, 1938). A visual orbit for the long-period system (P=6.91y) was derived by Aitken (Publ. Lick Obs., 12, 5, 1914) and rediscussed by Luyten in the paper cited in the Catalogue. The long-period system has not been included in the Catalogue since there seems to have been no direct spectroscopic determination of K, the semiamplitude of the spectroscopic binary about the centre of mass of the whole system. There are discrepancies in the orbital elements from epoch to epoch, probably indicating that the two orbital motions have not yet been completely disentangled, although there may also be physical perturbations. The set of elements given here refers to the interval 1923-28. G. Gatewood and S. Sofia (Publ. Astron. Soc. Pacific, 88, 50, 1976) find that the astrometric data suggest that the principal components of the system are overluminous for their masses. System27Orbit1End System28Orbit1Begin System28Orbit1End System29Orbit1Begin This is a mercury-manganese star for which Stickland and Weatherby give a `possible orbital solution'. A periodicity of about 400 d in the velocity had previously been suggested by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976). System29Orbit1End System30Orbit1Begin This star was used as a reference star in the Cambridge photoelectric velocity measurements and therefore, as explained by McClure et al., some orbits derived from such observations may be affected. It is difficult to classify the orbit. The scatter of observations at a given phase is often greater than the total range of variation, but the large number of observations permits a fairly precise determination of K1. In view of the long (and correspondingly uncertain) period, a conservative assessment seems appropriate. System30Orbit1End System31Orbit1Begin Brighter component of A.D.S. 513, companion 9.0 mag at 36". Other investigations by F.C. Jordan (Publ. Allegheny Obs., 2, 45, 1910) and W.J. Luyten, O. Struve and W.W. Morgan (Publ. Yerkes Obs., 7, Pt. IV, 254, 1939). The elements of the primary orbit found by these authors agree well, and they must be considered well determined. Only Pearce observed the secondary spectrum. Petrie(II) found Delta m=3.17. Luyten, Struve and Morgan revised the period to 143.621d. System31Orbit1End System32Orbit1Begin The Durchmusterung number is from the C.P.D. Radial velocities for this early-type near-contact system have been determined by cross-correlation and the primary curve is well covered although the r.m.s. error is 8.5 km/s. The epoch is a time of primary minimum, but the period is decreasing and a quadratic term (9.04E-4 d) must be included in the ephemeris. Hilditch and King have combined their spectroscopic observations with photoelectric light-curves observed by J.V. Clausen and B. Groenbech (Astron. Astrophys. Supp., 28, 389, 1977) to obtain masses of 1.6 MSol and 0.7 MSol, radii of 1.6 RSol and 1.0 RSol and luminosities of 5.6 LSol and 0.36 LSol. The orbital inclination is close to 81 deg. The secondary spectral type is estimated from the effective temperature quoted by Hilditch and King. System32Orbit1End System33Orbit1Begin Residuals from velocity-curve are small, but curve is based on only eleven observations. On basis of assigned spectral types, Delta m approx 0.6. Epoch is T0. Star is listed in I.D.S.: companion 8.6m at 330". System33Orbit1End System34Orbit1Begin Bakos gives a period of 15,000 days, which can be only an approximate value. The observational data for this low-amplitude binary are taken from several different observatories, and a homogeneous series of observations would be very helpful in confirming the orbital elements. The star is the brighter component of A.D.S. 548: companion is 12m at 28" separation. System34Orbit1End System35Orbit1Begin The velocities are determined by cross-correlation. Emission is seen at H and K, varying approximately in phase with the more massive component. The epoch is the time of primary minimum, when the less massive star is eclipsed. An unfiltered photoelectric light-curve has been observed by D.H. Bradstreet (Astron. J., 86, 98, 1981) who finds i=81 deg and that the brighter (but marginally cooler) component gives 60 percent of the light. System35Orbit1End System36Orbit1Begin The variation of the velocity of this star seems to be established, but with only one observation on the descending branch of the velocity-curve, the period must be uncertain. System36Orbit1End System37Orbit1Begin Orbital elements have previously been published by E.A. Vitrichenko (Soviet Astron. J., 11, 898, 1968 and Izv. Krym. Astrofiz. Obs., 39, 63, 1969). The new elements are preferred because they are based on more, better distributed observations. The main difference is the somewhat larger value of K2 found by Vitrichenko. Gies and Bolton suggest that the secondary is cooler than the primary and overluminous for its mass -- they estimate the visual magnitude difference between the two components to be close to zero. Vitrichenko observed a light variation of about 0.2m in V, consistent with the star being an ellipsoidal variable. The epoch is the time of inferior conjunction of the bright star. System37Orbit1End System38Orbit1Begin This system resembles YY Gem, although no eclipses have been detected. Both components have emission of variable intensity in the H and K lines of their spectra. At least one of the stars is a flare star and a BY Dra variable. A model for the system containing a spotty star is proposed by Bopp and Fekel. The epoch is the time of conjunction with the velocity of the primary star increasing: the orbit was assumed circular. The star varies by about 0.06m in V. System38Orbit1End System39Orbit1Begin Earlier investigations by W.E. Harper (Publ. Dom. Astrophys. Obs., 4, 135, 1917) revised in Publ. Dom. Astrophys. Obs., 6, 107, 1935, and by Luyten, based on Harper's material. Agreement with new elements is fairly good. Harper found e=0.01; Mannino and Grubissich find e approx 0.005. Values of K found by Harper are each about 3 km/s less than values in the Catalogue. Epoch is T0. A further discussion of the system was made by A. Krancj (Publ. Bologna Univ. Obs., 7, No. 11, 1959). Petrie(I) found Delta m=0.25. System39Orbit1End System40Orbit1Begin Earlier investigations by J. Lunt (Cape Annals, 10, Pt. 7, 38G, 1924) and by Neubauer himself (Publ. Astron. Soc. Pacific, 41, 371, 1929). Neubauer's later results agree much better with Lunt's than do his 1929 results. A small systematic difference exists between the Lick and Cape measures. From the Cape measures alone, V0=+13.6 km/s. System40Orbit1End System41Orbit1Begin Detection of the secondary component with a Reticon, combined with high-precision measures of the primary, bring the spectroscopic observations of this system to the high standard that photometric observations set long ago. The new elements for the primary star agree well with those found by C.L. Perry and S.N. Stone (Publ. Astron. Soc. Pacific, 78, 5, 1966) and the results from the original study by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 3, 248, 1926) agree within their uncertainties. The new observations lead to a circular orbit (e=0.000+/-0.003); the epoch is the time of primary minimum. Lacy has rediscussed the excellent light-curve by G.E. Kron (Lick Obs. Bull., 19, 59, 1939) and finds i=88.3deg, masses of 2.31 MSol and 1.35 MSol, radii of 2.53 RSol and 1.35 RSol and Delta m bol=2.9. A.C. de Landtsheer and P.S. Mulder (Astron. Astrophys., 127, 297, 1983) report from IUE observations that iron is overabundant by a factor of six in this system. De Landtsheer and J.P. de Greve (Astron. Astrophys., 135, 397, 1984) discuss the possible evolution of the system. Star is brighter component of A.D.S. 624: companion is 9.7m at 36". System41Orbit1End System42Orbit1Begin The first suggestion that this symbiotic star might be a spectroscopic binary with P approx 470 d was made by S.E. Smith (Astrophys. J., 237, 831, 1980). The value of the period was assumed by Oliversen et al. A circular orbit was assumed and phases were computed from the time of maximum equivalent width of the H-alpha emission, J.D. 2,443,200.5. Different methods of reduction lead to rather different values of K1, which quantity is, therefore, uncertain. R.E. Stencel (Astrophys. J., 281, L75, 1984) finds evidence from IUE observations for an eclipse of the hotter star by the cooler. Early reports of large variable magnetic fields in this system (H.W. Babcock, Publ. Astron. Soc. Pacific, 62, 277, 1950) are not confirmed by more recent observations (M.H. Slovak, Astrophys. J., 262, 282, 1982). The system is also discussed by M.R. Garcia (Astron. J., 91, 1400, 1986). System42Orbit1End System43Orbit1Begin The scatter of observations about the mean curve is large, and the possibility of other orbital periods should be investigated. Star is brighter component of A.D.S. 622: companion 11.2m at 33" appears to share the proper motion of the primary. System43Orbit1End System44Orbit1Begin System44Orbit1End System45Orbit1Begin Earlier investigations by J.B. Cannon (Publ. Dom. Astrophys. Obs., 2, 143, 1915), H.S. Jones (Cape Annals, 10, Pt. 8, 35, 1928) and Luyten (based on both these sets). Except for systematic differences in the Ottawa observations all investigators agree well. E.M. Hendry (Publ. Astron. Soc. Pacific, 92, 825, 1980) found that new observations required no modifications to Gratton's elements. The spectrum displays (possibly variable, see Hendry, loc. cit.) Ca II emission. A small light variation was interpreted by C.M. Huffer (Publ. Washburn Obs., 15, 29, 1928) as a combination of ellipticity effects and shallow eclipses. A UBV light-curve has been published by T.S. Belyakina, V.I. Burnashev and V.M. Zhilin (Izv. Krym. Astrofiz. Obs., 56, 16, 1977) who find a range of 0.2m in V and a period of 17.7673d. The epoch is the time of inferior conjunction of the visible star. Several faint companions are listed in I.D.S., but their physical connection is doubtful. System45Orbit1End System46Orbit1Begin The elements given in the Catalogue were published only shortly after those by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976). Since Nadal et al. use more observations and discuss the system more thoroughly, their results are preferred. The agreement is quite good, but there are some systematic departures of Abt's and Levy's observations from those obtained at Haute Provence. Nadal et al. argue for the existence of a third body causing supposed changes in K, omega and V0. Only the last-named are significant, however, and -- despite attempts to connect all observations to the `Lick System' -- may be the result of systematic errors between observatories. By Petrie's method, Nadal et al. find Delta m=0.18 in the photographic region of the spectrum. Two faint companions listed in I.D.S. are regarded by both sets of investigators as probably optical. System46Orbit1End System47Orbit1Begin Abt and Levy combined their new observations with those obtained by F.C. Jordan (Publ. Allegheny Obs., 1, 191, 1910) and offer these new improved elements. Petrie(I) found Delta m=0.76. System47Orbit1End System48Orbit1Begin Popper notes that the hydrogen lines strengthen with respect to the metallic lines during primary eclipse, but this effect cannot be caused by the secondary spectrum which should be that of a cooler star. There is also an apparent rotational disturbance in the velocities although the lines of the spectrum are quite sharp. All lines except lambda 4481 Mg II, which gives a higher value for K1, appear double near the time of primary minimum. The magnitude given in the Catalogue is derived from a single observation. The epoch is the time of primary minimum, and the orbit was assumed circular. System48Orbit1End System49Orbit1Begin The primary component of this two-spectra binary is a newly discovered mercury-manganese star. The velocities of the secondary component were used only to determine K2. More recent observations show some systematic departures from the orbital elements given here. Reference: F.C.Fekel,,,, (Unpublished) System49Orbit1End System50Orbit1Begin Petrie(II) found Delta m=0.29. The orbit should probably be assumed circular. According to I.D.S., there is an 11.5m companion at 133.4". System50Orbit1End System51Orbit1Begin Reference: G.A.Shajn, Pulkovo Circ.,, No. 21; 31, 1937 System51Orbit1End System52Orbit1Begin Earlier spectroscopic observations are discussed by E.F. Carpenter (Astrophys. J., 72, 205, 1930), Z. Kopal (Harvard Obs. Bull., No. 914, 1950) and R.H. Hardie (Astrophys. J., 112, 542, 1950). The complexity of the spectrum, arising from the presence of circumstellar matter in the system, probably ensures that the orbital elements will never be known with high accuracy. The epoch is the time of primary minimum; the period is variable and increasing. The value of K2 comes from the discussion of Reticon observations by J. Tomkin (Astrophys. J., 244, 546, 1981). It agrees closely with the value obtained by Batten and is certainly more reliable. Eruptive events observed in 1974 and since (A.H. Batten et al., Nature, 253, 174, 1975 and M. Plavec and R.S. Polidan, Nature, 253, 173, 1975) have stimulated much work on this system. Photometric studies of the variable circumstellar disk have been published by E.C. Olson (Astrophys. J., 237, 496, and 241, 257, 1980) and many of his conclusions have been confirmed and complemented by study of the UV spectrum (M.J. Plavec, Astrophys. J., 275, 251, 1983), whose spectral classifications (similar to Batten's) are given in the Catalogue. Plavec also finds Delta m V approx 2.5. A modern discussion of the undisturbed light-curve was published by E.C. Olson (Publ. Astron. Soc. Pacific, 96, 162, 1984) who finds i=85.8 deg. Polarization in the circumstellar matter has been studied by V. Piirola (Astron. Astrophys., 90, 48, 1980 and Astron. Astrophys. Supp., 44, 461, 1981). Weak X-rays have been detected from this system (N.E. White and F.E. Marshall, Smithsonian Astrophys. Obs. Special Rep., Vol. 2, No. 392, 93, 1982). These papers form only a part of the recent literature on this active system. Star is brighter component of A.D.S. 830: companion 11.2m at 13.8". System52Orbit1End System53Orbit1Begin This is a Wolf-Rayet binary in the Small Magellanic Cloud, possibly associated with the cluster and H II region N.G.C. 346. The system displays eclipses and the period was determined photometrically (J. Breysacher and C. Perrier, Astron. Astrophys., 90, 207, 1980) and the orbital inclination is estimated to be about 80 deg. Photometric and spectroscopic values of e and omega are in agreement, but Breysacher et al. point out that the large eccentricity is unusual in a Wolf-Rayet system with only a moderately long period. The epoch is the time of periastron passage as derived from the O-type spectrum. They also find the derived masses to be low, and express doubts whether or not the He II lambda 4686 emission truly represents the orbital motion of the Wolf-Rayet component. That line may also be in emission in the O-type spectrum. System53Orbit1End System54Orbit1Begin One node of this highly eccentric orbit is very well observed. The two components are blended, however, over most of the orbit. Velocities are obtained from lambda 4481 Mg II only. Petrie(II) found Delta m=0.16. System54Orbit1End System55Orbit1Begin The new data obtained by Hutchings and Thomas supersede those on which Kraft's (Astrophys. J., 135, 408, 1962) original orbit was based, clarifying some issues and confusing others. There appears to have been an error in the tabulation in Kraft's paper, where a value was given for K1 incompatible with the velocity-curve as drawn. Kraft's data lead to a value of K1 similar to that found by Hutchings and Thomas. The high orbital eccentricity found by Kraft is probably a result of distortion of the spectral line profiles by the hot-spot. Hutchings and Thomas found a smaller eccentricity than Kraft did and preferred to adopt a circular solution. The epoch is T0. There is evidence for a period change between the two epochs of observation. Hutchings and Thomas also believe they have detected the secondary spectrum, which should be measurable in the red region of the spectrum. The system is of the Z Cam type; light variations are not caused by eclipses (P. Szkody, Publ. Astron. Soc. Pacific, 86, 38, 1974). Attempts to detect soft X-rays from the system during a flare led only to the setting of an upper limit (P. Henry et al., Astrophys. J., 197, L117, 1975). System55Orbit1End System56Orbit1Begin This is another Wolf-Rayet binary in the Small Magellanic Cloud, first observed by A.F.J. Moffat (Astrophys. J., 257, 110, 1982). The system is not yet known to display eclipses, but Moffat believes that it may be found to do so; he had found a period of 6.861d, ruled out by the new observations. The designation signifies the number of the star in Sanduleak's list (Astron. J., 73, 246, 1968). The epoch is T0 for the absorption component. System56Orbit1End System57Orbit1Begin The period given in the Catalogue is derived from the radial velocities alone -- a somewhat heterogeneous set. The spectroscopic elements are all still highly uncertain, but S.L. Lippincott (Astrophys. J., 248, 1053, 1981) has published a thorough discussion of the astrometric orbit of this Population II binary. Her value for the period of 21.43y is certainly closer to the truth than that derived spectroscopically. She finds i=109.5 deg, omega=335.9deg and e=0.61. She estimates Delta m approx 4.5. Several faint and distant companions are listed in I.D.S. System57Orbit1End System58Orbit1Begin Bertaud and Floquet list the spectral type as Am, without further qualification. Bennett et al. comment on the prominence of lines of strontium in both spectra. There is no distinguishable difference between the spectra of the two stars. System58Orbit1End System59Orbit1Begin This recently discovered cataclysmic variable is remarkable for its short period and eclipses of a few minutes duration. Orbital solutions are necessarily uncertain. The orbital inclination is probably around 76 deg, the mass of the white dwarf probably between 0.5 MSol and 1 MSol and that of the other component probably around 0.25 MSol. The epoch is mid-eclipse of the `disk'. System59Orbit1End System60Orbit1Begin The new observations by Andersen are of the highest quality and supersede even those of D.M. Popper (Astrophys. J., 162, 928, 1970), with which they agree well except perhaps for V0, as well as those of C. Hagemann (Mon. Not. Roy. Astron. Soc., 119, 141, 1959) and A. Colacevich (Publ. Astron. Soc. Pacific, 47, 84, 1935). Photometric observations (J.V. Clausen et al., Astron. Astrophys., 46, 205, 1976) show e approx 0.01 and consequently a circular orbit was assumed in a spectroscopic solution. The epoch is the time of primary minimum. The small eccentricity appears to be real, however, and changes in the period suggest apsidal motion. The orbit would be of a quality if these were verified. The light-curve gives i=88 deg and L2 /L1=0.28 (at lambda 5500). There are companion stars each of 7.0m at 0.7" and 6.4" (I.D.S.). The question of their physical relationship to zeta Phe itself is still open, but the spectrum of the closer companion shows up in the combined light of the system. System60Orbit1End System61Orbit1Begin The new study by Andersen et al. supersedes the already good results obtained by M. Imbert (Astron. Astrophys. Supp., 36, 453, 1979) and by B.J. Hrivnak and E.F. Milone (Astrophys. J., 282, 748, 1984). This system is now amongst those with the best determined absolute dimensions, certainly of systems containing an evolved component. The discussion by Andersen et al. is very complete, including atmospheric abundances and evolutionary status. The epoch is the time of primary minimum and the eccentricity (actually 0.188) and longitude of periastron have been constrained to agree with the photometric value of e cos omega. The orbital inclination is close to 88.5 deg and the two stars differ by 0.17m in V. Masses are known to better than one percent. System61Orbit1End System62Orbit1Begin System62Orbit1End System63Orbit1Begin System63Orbit1End System64Orbit1Begin This star is a triple system since the spectroscopic pair is one component of the visual binary A.D.S. 999 with a possible orbital period of 75 years. The spectroscopic pair may prove to show eclipses. The spectral type is the mean for all three components (maximum separation in the visual orbit is less than 1"). Duquennoy computes F8 V and F9 V for the two components of the spectroscopic binary and believes that all three stars lie on the main sequence, with the visual companion about F4. O.J. Eggen (Astron. J., 70, 19, 1965) who did not know of the duplicity of one component, supposed the system to contain evolved stars. The two components of the visual binary are almost equal in luminosity while Delta V for the components of the spectroscopic pair probably lies between 0.2 and 0.4. System64Orbit1End System65Orbit1Begin The new orbit supersedes that by W.H. Christie (Astrophys. J., 77, 310, 1933) both because of the greater precision of the new observations and because they reveal the secondary spectrum. Beavers et al. estimate Delta m=1.6. They find that the orbital eccentricity, although small, is very probably real. This spectroscopic binary is the fainter member of the common-proper-motion pair that makes up zeta Psc. The brighter, A-type star, zeta Psc A, is 23" distant and has V=5.24. A 12.2m component C, about 1" from B, is probably also related. Each of A and B have shown evidence of being double during occultations. System65Orbit1End System66Orbit1Begin A mercury-manganese star for which `possible' orbital elements are given by Stickland and Weatherby. G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976) also considered the velocity of this star to be variable. System66Orbit1End System67Orbit1Begin The authors offer two solutions, the circular orbit given in the Catalogue and an elliptical one which they prefer on the grounds that most similar systems have elliptical orbits. The eccentricity proposed is 0.16+/-0.07, and V0, K and the standard deviation of an observation of unit weight are almost the same in the two solutions. There seems, therefore, no reason for adopting the elliptical orbit. If the orbit is elliptical, the period would be slightly shorter (11.588d); the epoch is T0. System67Orbit1End System68Orbit1Begin Unpublished elements provided by Fekel supersede the preliminary ones published by T. Simon, F.C. Fekel and D.M. Gibson (Astrophys. J., 295, 153, 1985). The system appears to be of the RS CVn type. IUE observations reveal the presence of a white-dwarf companion. Radio flares have been observed and the system is a source of soft X-rays (F.M. Walter and S. Bowyer, Astrophys. J., 245, 671, 1981). An 11.2m companion at 177.6" is listed in I.D.S. -- only one measurement of its position appears to have been made (by Burnham). Reference: F.C.Fekel,,,, (Unpublished) System68Orbit1End System69Orbit1Begin This is an X-ray pulsar and the measured quantity is, of course, the delay in the arrival time of the X-ray pulses rather than a radial velocity -- which is inferred from the deduced size of the orbit. The systemic velocity is unknown. The elements given in the Catalogue were the first determined. Other investigations by M.J. Ricketts et al. (Space Science Rev., 30, 399, 1981) and by R.L. Kelly et al. (Astrophys. J., 251, 630, 1981) lead to very similar elements. The orbit is undoubtedly exceedingly well known, but the existence of apsidal motion is still unsettled. There is some evidence for a slow rate (0.1 deg/yr) of apsidal regression. The system is also known as a gamma-ray source (P.M. Chadwick et al., Astron. Astrophys., 151, L1, 1985). J.B. Hutchings and D. Crampton (Astrophys. J., 247, 222, 1981) have identified an optical counterpart, but were unable to determine any orbital elements for it. System69Orbit1End System70Orbit1Begin Epoch is T0. Spectrum very badly distorted by gaseous streams. Modern photoelectric (ubvy I) light-curves have been published by E.C. Olson (Publ. Astron. Soc. Pacific, 97, 731, 1985) but no analysis has been attempted except to determine the colours of the components. After allowing for (heavy) reddening, the colours suggest somewhat earlier spectral types (B0.5 and B3) than Struve gave. System70Orbit1End System71Orbit1Begin The elements given here supersede earlier ones by the same authors and some others (F. Primini et al., Astrophys. J., 210, L71, 1976). This is another X-ray binary pulsar, and the orbital elements of the X-ray component are known with very high accuracy. The epoch is the time of minimum delay (or maximum advance) in arrival time of pulses. The eccentricity is known to be <0.0007; the orbital period was fixed in the solution. The values of K2 and V0 are derived from optical spectroscopic measurements by J.B. Hutchings et al. (Astrophys. J., 217, 190, 1977) and are much less precisely determined. Hutchings et al. estimate the orbital inclination to be about 70 deg : Primini et al. confine it between 53 deg and 73 deg. Hutchings et al. show that He II emission (lambda 4686) varies in phase with the X-ray component but shows a somewhat smaller amplitude. D.E. Gruber and R.E. Rothschild (Astrophys. J., 283, 546, 1984) report variability of the X-ray emission and G. Hammerschlag-Hensberge et al. (Astrophys. J., 283, 249, 1984) give the results of ultraviolet spectroscopy. Photometry by J. van Paradijs and L. Kuiper (Astron. Astrophys., 138, 71, 1986) shows the system to be an ellipsoidal variable at optical wavelengths, and the magnitude range given in the Catalogue corresponds to the approximate limits that they found. System71Orbit1End System72Orbit1Begin This is a short-period binary with an active chromosphere. Emission is seen at H-alpha and in the ultraviolet. The small light variability is not the result of eclipses but is ascribed by Bopp et al. to starspots. Spectral lines of both components are rotationally broadened and hard to measure. If the components have normal masses for G5 V stars, the orbital inclination is about 30 deg. The absorption lines in the two spectra are described as `of nearly equal intensity'. The epoch is superior conjunction of the more massive star. System72Orbit1End System73Orbit1Begin Earlier investigation by P.D. Jose (Astrophys. J., 114, 370, 1951) was based on an incorrect value for the period. H.A. Abt (Astrophys. J. Supp., 6, 37, 1960) classified the spectrum as A3, F2, F5 IV from the K line, hydrogen lines and metallic lines respectively. Fletcher found Delta m=0.09, by Petrie's method. New observations obtained by Abt and Levy (Astrophys. J. Supp., 59, 229, 1985) did not lead them to make any changes to these orbital elements. System73Orbit1End System74Orbit1Begin This star is a visual binary consisting of two nearly equal stars. Fletcher's spectroscopic observations demonstrated that the period was near 16 years rather than 32 years. He gives P=16.14y, T=1972.742. The elements given are all determined from the spectroscopic observations, although they are close to the latest set of elements derived from the visual observations by W.H. van den Bos (Publ. Astron. Soc. Pacific, 74, 291, 1962). The value given for K is K1+K2 and the values of the mass function and a sin i are correspondingly modified in significance. Slightly different elements were published by C.L. Morbey (Publ. Astron. Soc. Pacific, 87, 689, 1975) who has devised a method of combining visual and spectroscopic observations in a single solution for the orbital elements. System74Orbit1End System75Orbit1Begin System75Orbit1End System76Orbit1Begin Earlier investigations by J.H. Moore (Publ. Astron. Soc. Pacific, 41, 254, 1929) and B.P. Gerasimovic (Astrophys. J., 84, 232, 1936) are confirmed by Roemer's results. The F8 Ib star is a Cepheid variable with a period of about four days. The magnitude of the star is thus variable through a small range. The secondary spectrum is estimated. There is some slight evidence of a small variation in systemic velocity of amplitude 1 km/s and period 6 to 8 years, but the available material is insufficient to decide its reality. The velocity variation due to the Cepheid pulsation has a range of 5 to 6 km/s and is irregular. An astrometric orbit has been published by A.A. Wyller (Astrophys. J., 62, 389, 1957). His value of omega agrees well with Roemer's and he finds i=58 deg. The uncertainties, however, are very large. Period is 30.46y and periastron passage is 1928.48. Star is brighter component of A.D.S. 1477, companion 9.0m at 18". System76Orbit1End System77Orbit1Begin System77Orbit1End System78Orbit1Begin Luyten's orbit is based on observations by R.E. Wilson (Lick Obs. Bull., 9, 116, 1917). Wilson assumed a fixed value of T to obtain his elements. Luyten assumed a circular orbit and his epoch is T0. D.S. Evans (Mon. Notes Astron. Soc. South Africa, 16, 4, 1957) on the basis of nine new Cape observations finds the period should be revised to 193.85 d, but that the other elements need no change. Spectral type is that given by Evans. Star is variable. System78Orbit1End System79Orbit1Begin Elements are based on 22 low-dispersion spectrograms. Light-curves in UBV have been obtained by R.K. Srivastava and T.D. Padalia (Bull. Astron. Inst. Csl, 21, 359, 1970). Eclipses are partial. System79Orbit1End System80Orbit1Begin Star is brighter component of multiple star A.D.S. 1202, which does not seem to be a physical system. System80Orbit1End System81Orbit1Begin The spectral type given is from the H.D. Catalogue: Griffin and Emerson believe the true spectral type to be closer to K0. They gave T in the modified Julian date system in their paper: 2,400,000.5 has been added to their value to put the time of periastron on the same system as that for other systems. System81Orbit1End System82Orbit1Begin Earlier observations were published by the same author (Acta Astron., 27, 51, 1977). Elements derived from the two sets of observations agree well except for a large change (22.5 km/s) in the systemic velocity derived from the secondary component. Because of this and the relatively large scatter of the observations, the orbital elements can only be regarded as preliminary. The system is a W UMa system, and the epoch is the time of primary minimum. P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978) has derived photometric elements from observations published by R.M. Williamon (Astron. J., 80, 140, 1975) and finds that i=82 deg and the fainter component gives about 0.16 of the light in the yellow region. Duerbeck, however, indicates that the form of the light-curve is variable. System82Orbit1End System83Orbit1Begin This is a Wolf-Rayet binary in the Small Magellanic Cloud. Orbital elements (K and V0) are derived from the absorption lines of the O-type spectrum and the O IV emission line (lambda 3834) in the W-R spectrum -- which gives the most reasonable values for the minimum masses. The epoch is the time of conjunction (O-type star behind) as derived from measures of the absorption lines. The magnitude difference between the components is estimated at 2.6m (O-type star the brighter). Although coverage of the velocity-curve is good, the scatter of individual velocity measurements is very large. Note also the large difference in the systemic velocities derived from the two components. System83Orbit1End System84Orbit1Begin Although no luminosity classification of the spectrum is available, Griffin believes that the star is likely to be a giant. System84Orbit1End System85Orbit1Begin Moffat et al. are very cautious in putting forward this orbit. Velocity variations of the same period are found from the emission line He II lambda 4686 and the absorption line H-gamma -- but they are displaced in phase by 0.15 d from each other. The amplitude is the mean from both lines and the systemic velocity is an approximate value derived from the measures of the emission line (H-gamma gives close to 200 km/s). The magnitude is a photoelectrically determined Stromgren v magnitude. The zero of phase is the epoch at which the He II velocities equal the systemic velocity and are increasing. System85Orbit1End System86Orbit1Begin This star is a long-period eclipsing variable classified by A.P. Cowley (Publ. Astron. Soc. Pacific, 81, 297, 1969) as one of the group of systems resembling VV Cep. The orbital elements given here are based on observations by Cowley, J.B. Hutchings and D.M. Popper, and are still only provisional. Nevertheless, the observation of eclipses (J.T. Bonnell and T. Herczeg, Inf. Bull. Var. Stars, No. 1146, 1976) leaves no doubt as to the binary nature of the star. System86Orbit1End System87Orbit1Begin Brighter component of A.D.S. 1326, companion 10.6m at 11". System87Orbit1End System88Orbit1Begin Earlier investigations have been published by J.B. Cannon (J. Roy. Astron. Soc. Can., 4, 195, 1910), H. Ludendorff (Astron. Nachr., 186, 17, 1910), J.A. Hynek (Contr. Perkins Obs., No. 14, 1940) and G.R. Miczaika (Z. Astrophys., 28, 43, 1950). There is also a thesis by F.R. Hickok from which Poeckert has taken the determinations of the period and zero phase (inferior conjunction of the primary star). The system remains very difficult to interpret, since the presence of shells (probably around both components) creates complex line profiles showing both emission and absorption. Poeckert's study is very thorough and based on excellent material. He has probably determined the orbital elements of the primary star as accurately as is, at present, possible. He himself cautions against assuming too easily that the He II emission line (lambda 4686), from which he has determined K2, accurately reflects the motion of the secondary star. Masses and dimensions determined for the system do depend on this assumption. Different lines give different values for V0. System88Orbit1End System89Orbit1Begin Sterne's method for small eccentricities was used, but epoch is time of periastron passage. Lucy & Sweeney adopt a circular orbit for this system. System89Orbit1End System90Orbit1Begin The optical counterpart of this X-ray source is a star of the AM Her type. The values of K and V0 given are derived from measurements of the emission lines of hydrogen, ionized helium and ionized calcium (K). The epoch given is the time of inferior conjunction of the source of emission lines, computed from the information given in the paper. The velocity maximum (mean for all lines) occurs at a phase of 0.23d. System90Orbit1End System91Orbit1Begin Epoch is T0 deduced from the photometric data quoted by Struve et al. Photoelectric observations by G.G. Cillie and B.J. Bok (Harvard Obs. Bull., No. 920, 29, 1951) have been analyzed by G. Russo et al. (Astron. Astrophys. Supp., 47, 211, 1982) who find an orbital inclination close to 83 deg, and a fractional luminosity (in V) for the brighter component of 0.6. The two spectra are almost equal in intensity. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System91Orbit1End System92Orbit1Begin According to Heard and Krautter, D.P. Hube classified the spectrum as B9 III. The star is listed as a mercury-manganese star by Bertaud and Floquet. It has also been studied by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976) who obtained very similar orbital elements from all available observations. System92Orbit1End System93Orbit1Begin Because the period is so long, it is not well determined (the Cape observations do not cover one complete cycle, although some Lick observations are available). The orbit has been deemed to be of low quality, although the precision of the individual observations is high. The star is listed in I.D.S. but is an optical pair. System93Orbit1End System94Orbit1Begin For a bright star, this has proved a surprisingly difficult object, mainly -- as Pike, Lloyd and Stickland point out -- because it is rotating unusually rapidly for a late F-type star. The period has been uncertain. W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 113, 1915) first adopted P=1.73652d which he later revised to 1.73631d (Publ. Dom. Astrophys. Obs., 6, 211, 1935). H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976) derived a period of 1.73645d. Earlier, Luyten had proposed 2.3413d but R.W. Tanner (Publ. David Dunlap Obs., 1, 473, 1949) showed this to be spurious and even questioned the binary nature of the star. Although the new observations are few in number, they are of good quality and are well represented by the somewhat longer period of 1.767d. The r.m.s. scatter of the residuals from the velocity-curve obtained by Pike et al. is several times less than for that published by Abt and Levy. At last, we apparently have reasonably reliable elements for this star. The velocities were determined by cross-correlation and the systemic velocity depends on a conventional measurement of one plate -- it is, therefore, much less certain than are the other elements. The companions listed in I.D.S. are probably optical. System94Orbit1End System95Orbit1Begin System95Orbit1End System96Orbit1Begin Magnitude and spectral type are taken from the H.D. Catalogue since nothing more recent appears to be available. Griffin suggests that the star is probably a giant. System96Orbit1End System97Orbit1Begin A circular orbit was adopted after calculations showed that fitting an elliptical orbit to the observations made no significant improvement to their representation. The epoch is T0. The coverage of the velocity-curve is good, but there are some large residuals. No M-K classification has been published: Griffin suggests that the star is a giant. System97Orbit1End System98Orbit1Begin The new results are in good agreement with Petrie's earlier work (Publ. Dom. Astrophys. Obs., 7, 105, 1938) and in fair agreement with that of Ludendorff (Astrophys. J., 25, 320, 1907). Coverage of periastron is incomplete because the period is so close to an integral number of days that periastron is unobservable from North America during this century. For this reason, Gorza and Heard used some of Petrie's observations to obtain their preliminary solution. The difference between Petrie's value of omega (24.2 deg) and that found by Gorza and Heard may be real. If so, it represents an apsidal regress, perhaps to be ascribed to some form of periastron effect in this very eccentric orbit. A detailed abundance analysis of the spectrum has been published by J. Mitton (Astron. Astrophys. Supp., 27, 35, 1977). The value of K2 is taken from the paper by J. Tomkin and H. Tran (Astron. J., 94, 1664, 1987), who also give e=0.88. System98Orbit1End System99Orbit1Begin Both spectra are visible. Batten and Szeidl thought the primary spectrum might be as late as A2. The secondary spectrum is similar but the K line in it is relatively weak, and the secondary might be an Am star. System99Orbit1End System100Orbit1Begin The reference given in the Catalogue is to an abstract and most of the information given here is taken from a preprint of the full paper. The spectral type of the secondary is estimated from the effective temperature computed from the light-curve by Schiller and Milone. The epoch is the time of primary minimum and the orbit is assumed circular. Schiller and Milone do not compute K1 and K2 directly (the values given are estimates from their velocity-curves); they solve light-curves and velocity-curve together by the Wilson-Devinney method and find a mass-ratio of 0.6 and a total mass of 2.5 MSol. They believe that the primary nearly fills its Roche lobe. They find an orbital inclination of about 84 deg and a visual magnitude difference of 1.85m between the components. The star is a member of the cluster N.G.C. 752. System100Orbit1End System101Orbit1Begin System101Orbit1End System102Orbit1Begin The star is a member of the cluster N.G.C. 752. The spectral type is given by E.G. Ebbighausen (Astrophys. J., 89, 431, 1939) who ascribes it to Trumpler. Incredibly, no subsequent investigator appears to have considered it necessary to modernize, or even mention the type. The two components are apparently closely similar and approximately equal in intensity. The set of elements given is that computed for both components simultaneously; slightly different values are found when the elements are computed for each component separately. Searches have been made for eclipses without success. System102Orbit1End System103Orbit1Begin Provisional orbit. P=20,146.1 d. The star is a visual binary (A.D.S. 1598) with a known visual orbit (P. Muller, J. Observateurs, 32, 35, 1949). The visual and spectroscopic orbital elements refer to the same motion. i=21.2 deg. System103Orbit1End System104Orbit1Begin Epoch is T0. Circular orbit, confirmed by Lucy & Sweeney, is in agreement with the light-curve. The latest photoelectric observations are by S. Bozkurt et al. (Astron. Astrophys. Supp., 23, 439, 1976) in two colours approximating to B and V. They find i=88.5 deg and light-ratios of 0.10 (blue) and 0.18 (yellow). The secondary spectrum is seen during eclipse and is consistent with these light-ratios. There is a noticeable rotation effect in the velocity-curve. A 13 .3m companion at 6.7" is listed in I.D.S. System104Orbit1End System105Orbit1Begin McFarlane et al. give results of both photometric and spectroscopic observations. Although differential V magnitudes are given to three decimal places, the magnitude of the comparison star is given to only one. The spectral types are based at least partly on computation. the light-curve shows that the orbit must be circular. Radial velocities were determined by cross-correlation. The epoch is the time of primary minimum. The orbital inclination is estimated at 87 deg, and the light-ratio (in V) is about 7.5:1. System105Orbit1End System106Orbit1Begin Spectral classification is on the scheme advocated by Walborn for O-type stars. System106Orbit1End System107Orbit1Begin Star is fainter component of the visual triple system A.D.S. 1630. The pair B-C is unresolved on the slit of the Perkins Observatory spectrograph. It is believed that B is the spectroscopic binary. The visual components appear to be physically connected, and the system is therefore at least quadruple. System107Orbit1End System108Orbit1Begin The star is now classified as an Am star. H.A. Abt (Astrophys. J. Supp., 6, 37, 1961) gives types A2, A8, A8 from the K line, hydrogen lines and metallic lines, respectively. Abt also suggests that a small adjustment to the period may be needed. In a recent abundance analysis of the spectrum, J. Mitton (Astron. Astrophys. Supp., 27, 35, 1977) describes the two components as `virtually indistinguishable'. System108Orbit1End System109Orbit1Begin Epoch is T0. Spectral classification from the K line, hydrogen lines and metallic lines, is A2-3, A7 and F0, respectively. Star is brighter component of visual binary: companion 13.9m at 56" (I.D.S.). System109Orbit1End System110Orbit1Begin The study by A.P. Cowley et al. (Astrophys. J., 195, 413, 1975) cited in the Seventh Catalogue has been superseded by four investigations, including the one cited in this Catalogue. The other three are: J.B. Hutchings and T.J. Cote (Publ. Astron. Soc. Pacific, 97, 847, 1985); J.B. Hutchings, B. Thomas and R. Link (Publ. Astron. Soc. Pacific, 98, 507, 1986) and A.W. Shafter et al. (Astrophys. J., 290, 707, 1985). The study by Thorstensen et al. has been chosen because it contains the most thorough discussion of the period -- on which the other investigations have, to some extent, depended. Amplitudes of velocity variation differ from time to time and from line to line, and the choice of values of K and V0 is partly arbitrary. Those given here are for the emission line H-gamma. The scatter of observations is large and the situation is much complicated by the existence of an approximately equal but, nonetheless, distinct, photometric period and the apparently random variations in brightness of approximately 6 magnitudes in V. When the system is in its `low' state (optically faint), the velocity-curve shows a phase shift with respect to that of the `high' state. Nevertheless, observations of the high states extending over eleven years can be matched by the ephemeris given here. The epoch is the time of the inferior conjunction of the line-producing source. System110Orbit1End System111Orbit1Begin Earlier investigation by O. Struve and A. Pogo (Astrophys. J., 67, 336, 1928). The two sets of elements differ considerably, but Ebbighausen ascribes this to incomplete coverage of the earlier velocity-curve and to systematic differences between the Yerkes and Victoria measures. The velocity-curve is well covered by 62 observations and the elements are reasonably well determined, despite the fairly large scatter of individual observations. Determination of K2 is weak. Petrie(I) found Delta m=1.19. System111Orbit1End System112Orbit1Begin Star is brighter component of A.D.S. 1697. Companion is the star described in the following note. The magnitudes of the two stars cannot be measured separately (the stars are about 3.5" apart) and the combined value of V is 4.94. The magnitudes given are Harper's estimates. Luyten believes the uncertainties given by Harper are misprints. Lines of the secondary spectrum are, on average, about 20 percent fainter than those of the primary. System112Orbit1End System113Orbit1Begin Epoch is T0. Luyten's elements have been preferred to Harper's because Harper fixed T to obtain a solution. Harper later revised the period to 2.23655d. Petrie(II) found Delta m=0.61. System113Orbit1End System114Orbit1Begin System114Orbit1End System115Orbit1Begin System115Orbit1End System116Orbit1Begin Star is listed in I.D.S. with a companion of 9.8m, but rapid change in separation suggests pair is optical. System116Orbit1End System117Orbit1Begin The new observations by Abt and Levy have led to a revision of the period adopted in the earlier work of J.A. Pearce (Lick Obs. Bull., 11, 131, 1924). Otherwise, the orbital elements have not changed greatly, except that the small orbital eccentricity found by Pearce and regarded as real by Lucy & Sweeney, has been further reduced. G.H. Herbig (Astrophys. J., 141, 595, 1965) has detected the secondary spectrum on high-dispersion spectrograms of the red region. Star is the brighter component of A.D.S. 1739. The 13.7m companion at 64" is regarded by Abt and Levy as a probably optical one. System117Orbit1End System118Orbit1Begin The residuals from the velocity curve are rather large. Harper considered the possibility of a second variation with a period of one or two years, but rejected this idea. System118Orbit1End System119Orbit1Begin Two spectral classifications quoted by Griffin give slightly different luminosity classes. He himself points out that neither is completely consistent with the depth of traces given by his radial-velocity spectrometer. The epoch is T0. System119Orbit1End System120Orbit1Begin Spectral classification is on Walborn's scheme. Reference: G.L.Rogers, M.Sc. Thesis,, Toronto, 1974 (Unpublished) System120Orbit1End System121Orbit1Begin System121Orbit1End System122Orbit1Begin The very complete spectroscopic and photometric study by Hilditch et al. supersedes the orbit obtained earlier by A.J. Deutsch (Astrophys. J., 102, 496, 1945) partly because Hilditch et al. succeeded in detecting the secondary spectrum, but, more importantly, because they showed the system to be triple. The maximum magnitude is that given by Hilditch et al., the minimum is estimated from their data. The spectral type assigned to the secondary is based partly on the solution of the light-curve. The spectrum of the third body is not seen. The epoch in the short period orbit is the time of primary minimum: in the long-period orbit it is T0. No value is given for K2 by Hilditch et al.; the one in the Catalogue is computed from the values they give for the masses. The systemic velocity of the short period orbit is, of course, variable. From their light curve, Hilditch et al. find i close to 79 deg and a difference in visual magnitude (for the components of the eclipsing pair) of 1.08m. They estimate that the third body is of similar luminosity to the secondary component. System122Orbit1End System123Orbit1Begin The very complete spectroscopic and photometric study by Hilditch et al. supersedes the orbit obtained earlier by A.J. Deutsch (Astrophys. J., 102, 496, 1945) partly because Hilditch et al. succeeded in detecting the secondary spectrum, but, more importantly, because they showed the system to be triple. The maximum magnitude is that given by Hilditch et al., the minimum is estimated from their data. The spectral type assigned to the secondary is based partly on the solution of the light-curve. The spectrum of the third body is not seen. The epoch in the short period orbit is the time of primary minimum: in the long-period orbit it is T0. No value is given for K2 by Hilditch et al.; the one in the Catalogue is computed from the values they give for the masses. The systemic velocity of the short period orbit is, of course, variable. From their light curve, Hilditch et al. find i close to 79 deg and a difference in visual magnitude (for the components of the eclipsing pair) of 1.08m. They estimate that the third body is of similar luminosity to the secondary component. System123Orbit1End System124Orbit1Begin The first spectroscopic observations were by M.F. Walker (Bamberg Veroff., 9, No. 100, 243, 1971) and two orbital studies have been published in recent years. The one by R.H. Kaitchuck et al. has been chosen over that by J. Smak (Acta Astron., 29, 469, 1979) because of the high time-resolution achieved and the number of observations. Like all cataclysmic variables, this remains a very difficult system to interpret. Magnitudes are taken from Walker's photometric study (Astrophys. J., 137, 485, 1963). Although on the V scale, they can be only approximate because the system varies in light independent of its eclipses. The figures given attempt to show the greatest possible range. The epoch is the time of mid-eclipse and is taken, with the period, from O. Mandel (Peremm. Zvezdy, 15, 474, 1965). The period is variable. The values of K and V0 given are for He II lambda 4686. Somewhat different values are obtained from other lines (both emission and absorption). Kaitchuck et al. estimate an orbital inclination of around 70 deg and masses of about 0.75 MSol and 0.6 MSol (white dwarf). System124Orbit1End System125Orbit1Begin Although Griffin could find no modern spectral classification, he believed the star to be a giant. The circular orbit was adopted since a solution for an elliptical orbit did not significantly decrease the sum of squares of the residuals. The epoch is T0. System125Orbit1End System126Orbit1Begin System126Orbit1End System127Orbit1Begin The elements given in the Catalogue are from an unpublished investigation by R.J. Northcott based on Mt. Wilson and David Dunlap spectrograms. H.A. Abt and S.G. Levy (Publ. Astron. Soc. Pacific, 81, 280, 1968) obtained several coude spectrograms, the velocities from which were satisfied by a period of 9.3737d. Comparison of their observations with the individual ones used by Northcott, however, shows that the period she derived is correct. They all agree on the values of K and V0, except there is some evidence for a slight difference between the values of V0 for each component. Reference: R.J.Northcott, Private Comm.,,, 1965 System127Orbit1End System128Orbit1Begin The spectral types given depend partly on computation of the combination of stars needed to produce the observed colours and radial velocity `dips'. Lu estimates the V magnitude difference to be 1.3m. System128Orbit1End System129Orbit1Begin The orbital elements are derived from the emission lines which vary in velocity in phase with the absorption lines (arising from the M-type dwarf) and can be more accurately measured than the latter. The epoch is the time of inferior conjunction of the component producing the visible spectrum (i.e. the M-type star). If a mass of 0.6 MSol is assumed for this star, Thorstensen et al. estimate a mass of 0.93 for the white dwarf. System129Orbit1End System130Orbit1Begin Spectral classification is approximate, but the primary spectral type is not as late as M0 V. All hydrogen lines to H-zeta and the H and K lines of Ca II are seen in emission. On some plates the emission appears to be double and a tentative mass ratio of 0.52 has been derived. The light of the system is variable and one of the stars is a flare star. Other variations in the light of the system are ascribed to surface spots by B.W. Bopp and D.S. Evans (Mon. Not. Roy. Astron. Soc., 164, 343, 1973). The system is very similar to that of BY Dra and, in some respects, to that of YY Gem. Lucy & Sweeney regard the orbit as circular. System130Orbit1End System131Orbit1Begin Epoch is T0, which is much better determined than the time of periastron passage. System131Orbit1End System132Orbit1Begin The brighter component of A.D.S. 1982 which shares a common proper motion with its 7.37m companion at 38" separation. Each component has its own H.D. number, and some confusion has existed in the past as to the number appropriate to the brighter component. This is the same star that was erroneously listed in the Sixth Catalogue as H.D. 16232. Morbey and Brosterhus found that the observations by Adams and Joy were better satisfied by their new period. System132Orbit1End System133Orbit1Begin The period may be variable. The spectral type given in the Sixth Catalogue, A2 II, was assigned by Ch. Fehrenbach et al. (Publ. Obs. Haute Provence, 8, 25, 1966). In view of the short period, it seems unlikely that a genuine bright giant can exist in the system, and the classification by G. Hill et al. (Mem. Roy. Astron. Soc., 79, 131, 1975) is preferred here -- although photometric solutions suggest a somewhat hotter star. A new photometric study based on UBV observations has been published by B. Cester et al. (Astron. Astrophys. Supp., 30, 223, 1977). They estimate that i is approximately 82 deg and that the brighter component gives approximately 0.98 of the total light, in each colour. They suggest that the components form an early type contact system. System133Orbit1End System134Orbit1Begin Epoch is an arbitrary zero of phase: T0 is about 2.41d after zero phase. Lucy & Sweeney confirm that the orbit is circular. System134Orbit1End System135Orbit1Begin A visual binary for which P, e and omega are assumed from the visual orbit by P. Baize (J. Observateurs, 45, 247, 1962). Abt and Levy believe lines of both components (of approximately equal brightness) are blended and that the true value of K1 is higher than given here. This and the incomplete coverage of the velocity-curve account for the low grade assigned. Baize gives i=31.5 deg. System135Orbit1End System136Orbit1Begin Reference: A.Colacevich, Oss. e Mem. Arcetri,, No. 59, 1941 System136Orbit1End System137Orbit1Begin Original elements were computed by W.E. Harper with T fixed (Publ. Dom. Astrophys. Obs., 4, 313, 1930). Therefore the recomputation by Luyten has been preferred. Epoch is T0. System137Orbit1End System138Orbit1Begin Epoch is T0. This is one of the few systems for which Lucy & Sweeney find a real eccentricity not deduced by the original investigator. C.D. Kandpal (Astrophys. Space Sci., 32, 291, 1975), on the basis of his UBV observations, revised Struve's value for the period and gave the depths of primary and secondary minima (in V) as 0.649m and 0.075m respectively. F. Mardirossian et al. (Astron. Astrophys. Supp., 39, 235, 1980) have discussed earlier photometric observations of this star and derive a value of i close to 80 deg and find that the fainter component gives about 2 percent of the light in all colours. They suggest that this is probably a system that contains a genuine `undersize' sub-giant. System138Orbit1End System139Orbit1Begin The elements are described as `marginal' by Abt and Levy themselves. System139Orbit1End System140Orbit1Begin This star is the first studied in a very thorough investigation of the spectroscopic binaries in the Hyades. Its membership in the cluster is, at present, uncertain but by no means ruled out. System140Orbit1End System141Orbit1Begin According to J.H. Moore, who first detected double lines in the spectrum (Lick Obs. Bull., 7, 96, 1912), the lines in the secondary spectrum are much fainter than those in the primary. System141Orbit1End System142Orbit1Begin Although this system has been the subject of several investigations during the recent years, still no velocity-curve has been published since Hiltner's work, nor is there a good modern light-curve. The hydrogen and helium lines give different orbital elements. Those in the Catalogue are derived from the hydrogen lines. The helium lines give: omega=14 deg, e=0.21, K=36 km/s and V0=26 km/s. One might suppose the helium lines to be freer from effects of circumstellar matter for which many investigators find evidence, but they display the greater rotational disturbance during eclipse. The epoch is the time of primary minimum. The spectral classification of the two stars is from the spectrophotometric study by V.G. Karetnikov et al. (Astron. Zh., 56, 1012 and 1220, 1979); photometric results obtained by W. van Hamme and R.E. Wilson would suggest a somewhat later type for the secondary. Van Hamme and Wilson derive a value close to 81 deg for i and find that the primary component gives about 0.75 of the total light. Their results do not completely agree with earlier studies (F.B. Wood, Princeton Obs. Contr., No. 21, 1946); M.I. Lavrov & N.V. Lavrova, Trudy Kazan Obs., 41, 3, 1976) and they themselves comment at some length on the difficulties of obtaining a fully consistent solution of the light-curve. They also make use of unpublished observations of the secondary made by D.M. Popper, which indicate a value for K2 of the order of 190 km/s. O.S. Shulov and G.A. Goudcova (Astrofiz., 5, 477, 1969) find variable polarization in the light of this system. System142Orbit1End System143Orbit1Begin System143Orbit1End System144Orbit1Begin The new orbit by Duerbeck and Hanel certainly supersedes the earlier work by F.C. Jordan (Publ. Allegheny Obs., 3, 137, 1914) and H.G. Horak (Astrophys. J., 115, 61, 1952). By using only the measurements of the metallic lines, Duerbeck and Hanel have shown that the true orbit is circular and that earlier determinations of orbital elements were subject to the effects usually ascribed to gas streams. Even the metallic lines are affected by a rotational disturbance during eclipse. The period is subject to variation. The epoch is the time of primary minimum. The best light-curve available is still that published by C.R. Chambliss (Publ. Astron. Soc. Pacific, 88, 22, 1976) in approximately the UBV system. He derives i=82.5 deg and finds that the primary component contributes about 90 percent of the light in the yellow region. He derives spectral types of A2 V and G5 IV, but Duerbeck and Hanel give A3 V for the primary star. Some of Chambliss' results are confirmed by interference-filter photometry by G.P. McCook et al. (Bull. Am. Astron. Soc., 6, 467, 1974). Earlier debates about apsidal motion (J.A. Pearce, Publ. Astron. Soc. Pacific, 49, 223, 1937 and W.J. Luyten, ibid., p. 329) are no longer of interest since the orbit is circular. System144Orbit1End System145Orbit1Begin Although the visible spectrum is A0, there must be a late-type (presumably giant) companion since otherwise the velocities of the system could not have been measured photoelectrically. Griffin predicts that the system will display eclipses. The star is the brighter component of A.D.S. 2115; the companion is 8.8m at 8.1". According to I.D.S., separation and position angle have shown no perceptible change in more than 100 years. System145Orbit1End System146Orbit1Begin Brighter component of A.D.S. 2151; companion 8.4m at 3". There is some difference in the values of e and omega obtained in Young's original solution and Luyten's recomputation. Lucy & Sweeney find a circular orbit for this system and their conclusion is probably correct. System146Orbit1End System147Orbit1Begin Harper considered no revision of these elements was needed in his `Re-examination of 64 Orbits' (Publ. Dom. Astrophys. Obs., 6, 215, 1935). Spectral types are A0 from the K line and A7 from the metallic lines (Bertaud and Floquet). According to I.D.S. there is a companion, 9.2m at 192.7", that has shown no relative motion for 30 years. System147Orbit1End System148Orbit1Begin Elements agree well with the preliminary values determined by W.H. Christie (Astrophys. J., 83, 433, 1936). There is also an earlier paper by Colacevich (Publ. Astron. Soc. Pacific, 48, 32, 1936). D.S. Hall (Bull. Am. Astron. Soc., 18, 133, 1986) reports a periodic variation in light with the same period as the orbital motion. Brightest component of A.D.S. 2202: companions 10.7m and 11.8m at about 51" and 4", respectively. Reference: A.Colacevich, Oss. e Mem. Arcetri,, No. 59, 1941 System148Orbit1End System149Orbit1Begin The spectrum appears to vary with about half the period of the velocity variation. The orbital elements are obtained from the K line only. The hydrogen lines give a nearly constant velocity while the metallic lines show a large scatter. The secondary spectrum has been detected on tracings, and tentative values of the mass-ratio and light-ratio are 0.4 and 0.3, respectively. Lucy & Sweeney regard the orbit as circular. System149Orbit1End System150Orbit1Begin Epoch is T0 and the circularity of the orbit is confirmed by Lucy & Sweeney. The secondary spectrum is seen during primary eclipse. A new analysis of the light-curves has been made by M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 273, 1980). They find i is approximately 36 deg and that the fainter component gives 0.13 of the total light in V. A 12.1m companion of 11.6" is listed in I.D.S. System150Orbit1End System151Orbit1Begin The epoch is primary minimum. Bertaud and Floquet give spectral types of A2 and F0 from the K line and the metallic lines respectively. Popper describes both spectra as very similar, but cannot rule out a slight difference between them in metallicism. Analysis of light-curves by A. Okazaki (Astrophys. Space Sci., 56, 293, 1978) is preferred because it reconciles discordant results f ound by independent observers and gives i approximately equal to 88 deg and a fractional luminosity in V, for the brighter component, of 0.57. System151Orbit1End System152Orbit1Begin Star is brighter component of A.D.S. 2348. Companion is 10.7m at 24.2". According to Abt, the star has spectral types A7, A7 and F2 from the K line, the hydrogen lines, and the metallic lines, respectively. Epoch is T0. System152Orbit1End System153Orbit1Begin The combined spectral type has been classified as G0 IV-V. The individual types given here are estimated by Griffin and are not direct MK classifications of the spectrum. System153Orbit1End System154Orbit1Begin The upper row of figures refers to the G-type component. In earlier editions of this Catalogue no classification of the orbit quality was made since the only published discussion of the orbital elements was McLaughlin's brief abstract. H.A. McAlister (Astron. J., 87, 563, 1982) has now published a preliminary orbit based on speckle interferometry which provides a measure of confirmation of McLaughlin's work. Assuming the spectroscopic values of P, T and e, McAlister found a value for omega close to McLaughlin's own, confirmed the prediction that i is close to 90 deg (McAlister found i=88 deg) and also found a maximum separation of about the size that McLaughlin predicted -- actually a little smaller. Although all results remain preliminary, it seems likely that McLaughlin's elements will eventually prove to have been not far wrong. McAlister derives a distance of 73.8 parsecs and masses of 4.73 MSol (G-type star) and 2.75 MSol. On this basis he proposes that the spectral types should be revised to G8 II-III + B9V. The star is the brighter component of A.D.S. 2324; companion is 10.8m at 57". System154Orbit1End System155Orbit1Begin The new results by Andersen, Pavlovski and Piirola clearly supersede the earlier work by O. Struve (Astrophys. J., 99, 295, 1944) and V. Ya. Alduseva (Pis. Astron. Zh., 12, 212, 1986) and the very brief note by W. Strupat (Mitt. Astron. Gesells., 62, 275, 1984). The analysis by Andersen et al. brings out even more clearly the similarity of this system to SX Cas (Note HD 232121) and the note for this system should be read against the background of the note for the other. Once again, the secondary's velocity-curve is much better determined (from photoelectric measures) than the d quality that has been assigned would suggest. Once again, the A-type `primary' spectrum is that of a shell or disk that completely conceals from view a presumably hotter star. The spectral types estimated by Andersen et al. agree with those determined by M.J. Plavec and J.L. Weiland (Bull. Am. Astron. Soc., 15, 916, 1983) from IUE spectra. The period is known to be increasing: that given and the epoch (time of primary minimum) are those appropriate to the interval covered by the observations of Andersen et al. The orbit is assumed circular -- the velocity-curve of the secondary star so indicates. The amplitude of the primary star is only a best estimate, but it does help to lead to a consistent picture of a semi-detached system. The light-curve is known to be variable and has been discussed in detail by P. Kalv (Tartu Astron. Obs. Teated, No. 58, 3, 1979) and by S. Kriz et al. (Bull. Astron. Inst. Csl, 31, 284, 1980). New photometric observations are also given by Andersen et al. They find an orbital inclination of 80 deg, but cannot give a magnitude difference since the primary component is completely hidden. System155Orbit1End System156Orbit1Begin Epoch is the time of primary minimum. From his own analysis of photometric observations by K.-Y. Chen (Acta Astron., 25, 89, 1975) Popper derives an orbital inclination close to 86 deg and finds a magnitude difference between the components of 0.8m in V. The spectral types of the two components are similar but not the same. Popper gives B-V=+0.34 and +0.40 for primary and secondary respectively. System156Orbit1End System157Orbit1Begin The major advance, since the publication of the Seventh Catalogue, in our understanding of this triple system has been the successful detection of the secondary component by J. Tomkin and D.L. Lambert (Astrophys. J., 222, L119, 1978). Their result for K2 is given in the present Catalogue, the other elements being taken from the paper cited there. The elements of the short-period pair in this system must now be well known, except that V0, of course, is variable. Hill et al. believed the 32-year periodic variation in times of minima to be the result of apsidal motion of the close pair. Other explanations continue to be offered, however. The long-period orbit is less certain. The value found for KAB by Hill et al. is appreciably larger than that found by Ebbighausen and Gange (Publ. Dom. Astrophys. Obs., 12, 151, 1962). P.J. Bachmann and J.L. Hershey (Astron. J., 80, 836, 1975) derived an orbit for the long-period pair from simultaneous analysis of spectroscopic, astrometric and photometric (light-time) observations. They derived a period of 1.8613y (T=1903.375) and an orbital inclination of 56 deg. The mass they derived for the pair AB is, however, higher than that now found, and the orbit derived from speckle interferometry by A. Labeyrie et al. (Astrophys. J., 194, L174, 1974) is perhaps to be preferred, even though there is evidence that the observations were affected by the presence of circumstellar matter. According to Labeyrie et al. i approx 80 deg. The orbital inclination of the short-period pair is close to 82 deg, according to both G. Hill and J.B. Hutchings (Astrophys. J., 162, 265, 1970) and R.E. Wilson et al. (Astrophys. J., 177, 191, 1972). The latter find that the primary gives 0.97 of the total light (in V) of the close pair. There are rather divergent estimates of the magnitude difference AB-C; Labeyrie et al. give 2.5m. The system is known to have radio flares (C.M. Wade and R.M. Hjellming, Nature, 235, 270, 1972) and is also a source of X-rays (H.W. Schnopper et al., Astrophys. J., 210, L75, 1976). Other recent investigations of the system include several of the UV Mg II lines, which also show evidence of gas-streaming (see e.g. H. Cugier and P. Molaro, Astron. Astrophys., 128, 429, 1983 and K.-Y. Chen et al., Astron. J., 86, 258, 1981). Y. Kondo et al. also find evidence for mass loss from the primary component (Inf. Bull. Var. Stars, No. 1312, 1977). H. Zirin and M.A. Liggett (Astrophys. J., 259, 719, 1982) have studied variations in the intensity of the line of He II lambda 10,830. A thorough study of the emission has recently been completed (M.T. Richards, S.W. Mochnacki and C.T. Bolton, Astron. J., 96, 326, 1988). Two independent studies of the rotation of the primary component confirm that it is rotating synchronously (S. Rucinski, Acta Astron., 29, 339, 1979; J. Tomkin and H.-S. Tan, Publ. Astron. Soc. Pacific, 97, 51, 1985). System157Orbit1End System158Orbit1Begin The major advance, since the publication of the Seventh Catalogue, in our understanding of this triple system has been the successful detection of the secondary component by J. Tomkin and D.L. Lambert (Astrophys. J., 222, L119, 1978). Their result for K2 is given in the present Catalogue, the other elements being taken from the paper cited there. The elements of the short-period pair in this system must now be well known, except that V0, of course, is variable. Hill et al. believed the 32-year periodic variation in times of minima to be the result of apsidal motion of the close pair. Other explanations continue to be offered, however. The long-period orbit is less certain. The value found for KAB by Hill et al. is appreciably larger than that found by Ebbighausen and Gange (Publ. Dom. Astrophys. Obs., 12, 151, 1962). P.J. Bachmann and J.L. Hershey (Astron. J., 80, 836, 1975) derived an orbit for the long-period pair from simultaneous analysis of spectroscopic, astrometric and photometric (light-time) observations. They derived a period of 1.8613y (T=1903.375) and an orbital inclination of 56 deg. The mass they derived for the pair AB is, however, higher than that now found, and the orbit derived from speckle interferometry by A. Labeyrie et al. (Astrophys. J., 194, L174, 1974) is perhaps to be preferred, even though there is evidence that the observations were affected by the presence of circumstellar matter. According to Labeyrie et al. i approx 80 deg. The orbital inclination of the short-period pair is close to 82 deg, according to both G. Hill and J.B. Hutchings (Astrophys. J., 162, 265, 1970) and R.E. Wilson et al. (Astrophys. J., 177, 191, 1972). The latter find that the primary gives 0.97 of the total light (in V) of the close pair. There are rather divergent estimates of the magnitude difference AB-C; Labeyrie et al. give 2.5m. The system is known to have radio flares (C.M. Wade and R.M. Hjellming, Nature, 235, 270, 1972) and is also a source of X-rays (H.W. Schnopper et al., Astrophys. J., 210, L75, 1976). Other recent investigations of the system include several of the UV Mg II lines, which also show evidence of gas-streaming (see e.g. H. Cugier and P. Molaro, Astron. Astrophys., 128, 429, 1983 and K.-Y. Chen et al., Astron. J., 86, 258, 1981). Y. Kondo et al. also find evidence for mass loss from the primary component (Inf. Bull. Var. Stars, No. 1312, 1977). H. Zirin and M.A. Liggett (Astrophys. J., 259, 719, 1982) have studied variations in the intensity of the line of He II lambda 10,830. A thorough study of the emission has recently been completed (M.T. Richards, S.W. Mochnacki and C.T. Bolton, Astron. J., 96, 326, 1988). Two independent studies of the rotation of the primary component confirm that it is rotating synchronously (S. Rucinski, Acta Astron., 29, 339, 1979; J. Tomkin and H.-S. Tan, Publ. Astron. Soc. Pacific, 97, 51, 1985). System158Orbit1End System159Orbit1Begin Petrie(II) found Delta m=1.59. Luyten has computed another set of elements from these same observations. The range of variation is small and according to the Finding List the star may be an ellipsoidal variable. It has recently attracted attention as a variable radio source (D.M. Gibson and R.M. Hjellming, Publ. Astron. Soc. Pacific, 86, 652, 1974). System159Orbit1End System160Orbit1Begin Two independent spectroscopic investigations of this system were published simultaneously. The other is by E.J. Weiler (Publ. Astron. Soc. Pacific, 86, 56, 1974). FitzGerald's is the more complete discussion and is based on better coverage of the velocity curve and is preferred here even though his spectrograms are of several different dispersions. The two sets of elements are in close agreement (Weiler gives K1=76.0 km/s, K2=72.3 km/s, V0=+24.6 km/s). The epoch given by FitzGerald is T0 for the primary star. The two authors disagree as to spectral classification; Weiler assigns G0 V and K0 IV to the two stars. Both emphasize the difficulty of classification and remark on the presence of H and K emission in the secondary spectrum. The star is probably of the RS CVn type. Formerly designated as BV 307, its variability was discovered by W. Strohmeier et al. (Veroff. Remeis-Sternw. Bamberg, 5, 3, 1962). Primary eclipse is over a magnitude deep, and FitzGerald reports that J.R. Percy has established the existence of a secondary eclipse of at least 0.3m depth. The period's length being close to an integral number of days makes observation of the entire light curve difficult. FitzGerald finds, by Petrie's method, that Delta m=0.6. System160Orbit1End System161Orbit1Begin System161Orbit1End System162Orbit1Begin Epoch is time of primary minimum and the orbit was assumed to be circular. The spectral type is the mean for the two components. Two modern light-curves have been published since the Seventh Catalogue: H. Jorgensen (Astron. Astrophys., 72, 356, 1979, ubvy) and D.M. Popper and P. Etzel (Astron. J., 86, 102, 1981). Results obtained from them are in good agreement. Popper and Etzel adopted an orbital inclination of 89.2 deg and a fractional luminosity of 0.64 (in V) for the primary component. Jorgensen estimated Delta V=0.7m. System162Orbit1End System163Orbit1Begin The new orbit by Abt and Levy confirms and supersedes the earlier investigation by W.E. Harper (Publ. Astron. Soc. Pacific, 6, 79, 1932) and the recomputation of those elements by Luyten. The spectrum is that of an Am star, classified by Abt and Levy as A2, A9, F2 from the K line, hydrogen lines, and metallic lines respectively. The epoch given is the time of maximum positive radial velocity. The star is the brighter component of A.D.S. 2433 with a 12.0 m companion at 31". System163Orbit1End System164Orbit1Begin The system is recognized as a magnetic accreting white-dwarf binary, similar to AM Her. It has attracted much attention and other spectroscopic discussions have been published (D. Schneider and P. Young, Astrophys. J., 238, 946, 1980; D.A. Allen, M.J. Ward and A.E. Wright, Mon. Not. Roy. Astron. Soc., 195, 155, 1981; J. Bailey and M. Ward, Mon. Not. Roy. Astron. Soc., 196, 425, 1981; J.B. Hutchings et al., Astrophys. J., 252, 690, 1982 and K. Mukai and P. Charles, Mon. Not. Roy. Astron. Soc., 212, 609, 1985). The results of different investigations do not agree well, which may reflect different ways of defining the emission lines measured or real changes in the system. Either way, the relation between the measured quantities and the physical properties of the system is very uncertain. The star shows variable polarization and an eclipse in X-rays and infrared, as well as some variation in visible light. The epoch given is the time of maximum positive velocity of the wings of the H lines, although Crampton et al. calculate phases from the appearance of the linear polarization pulse. System164Orbit1End System165Orbit1Begin The new observations by Abt and Levy lead to a considerable improvement in the orbital elements over those previously published by Abt himself (Astrophys. J. Supp., 6, 37, 1961). Abt and Levy give the spectral types as A2.5, A6, F0 from the K line, hydrogen lines and metallic lines respectively. System165Orbit1End System166Orbit1Begin The epoch is the approximate time of primary minimum. A photoelectric V light-curve has been published by S. Mancuso, L. Milano and G. Russo (Astrophys. Space Sci., 47, 277, 1977) and analyzed by them and by M.T. Edalat: (Astrophys. Space Sci., 58, 3, 1978 and 59, 443, 1978). Complete (UBV) light-curves were published and analyzed by B.B. Sanwal and U.S. Chaubey (Astrophys. Space Sci., 75, 329, 1981). All investigators agree that i is close to 85 deg or 86 deg, but differ on the ratios of the radii and the fractional luminosities. about 0.8 of the total light in V comes from the brighter component. Sanwal and Chaubey find some evidence for a disk around that star. System166Orbit1End System167Orbit1Begin A similar orbital solution has been published by J. Tomkin, C. Sneden and P.L. Cottrell (Publ. Astron. Soc. Pacific, 96, 609, 1984). They find a small and possibly significant eccentricity (0.037) and derive a slightly longer period (287.55d). They also classify the spectrum as G5 III. The elements obtained by Lucke and Mayor are preferred primarily because they are based on more observations. The star is the brighter component of A.D.S. 2509; its companion is 12.2m at 1". System167Orbit1End System168Orbit1Begin System168Orbit1End System169Orbit1Begin Although no new orbit has been published since the Seventh Catalogue appeared, this system, being an active (but non-eclipsing) system of the RS CVn type, has attracted a great deal of attention. Spectrophotometric studies have been made by C.G. Rhombs and J.D. Fix (Astrophys. J., 216, 503, 1977) and E.J. Weiler (Mon. Not. Roy. Astron. Soc., 182, 77, 1978) who studied the emission-line (H, K and H-alpha) variations. Observations made with IUE, giving evidence for flares, have been published by T. Simon, J.L. Linsky and F.H. Schiffer (Astrophys. J., 239, 911, 1980) and the first two of those authors have also discussed a chromospheric model (Astrophys. J., 241, 759, 1980). Simultaneous optical, UV and radio observations are reported and discussed by E.J. Weiler et al. (Astrophys. J., 225, 919, 1978). System169Orbit1End System170Orbit1Begin Velocity variation of this star has long been suspected and K. Kodaira (Publ. Astron. Soc. Japan, 23, 159, 1971) found a period closely similar to that given by Abt and Levy. The velocity variation seems to be well established, but the maximum velocity and most of the descending branch have not been observed. The star belongs to the alpha Per cluster. System170Orbit1End System171Orbit1Begin Although elements obtained by B. Paczynski (Acta Astron., 15, 197, 1965) were preferred in the Seventh Catalogue, the new observations have shown that R.P. Kraft's original value of 1.904d for the orbital period (Astrophys. J., 139, 457, 1964) was more nearly correct. The value of K1 refers to the late-type component with an absorption spectrum; that of K2 (34 km/s) is derived from the emission wings of H-beta. The epoch is T0. The star is also Nova Per 1901. System171Orbit1End System172Orbit1Begin Harper (Publ. Astron. Soc. Pacific, 6, 214, 1935) did not consider it necessary to revise these elements. The star is identified as an occultation double in the Bright Star Catalogue. System172Orbit1End System173Orbit1Begin These elements supersede those determined earlier by Harper (Publ. Dom. Astrophys. Obs., 4, 48, 1927) with P=11.422d. There are diverse spectral classifications for this star and the Am character is regarded as doubtful by Bertaud and Floquet, although it is retained among the Am stars by Curchod and Hauck. The epoch is the time of inferior conjunction of the visible star. The star is an ellipsoidal variable, the light variation being periodic with the orbital period. System173Orbit1End System174Orbit1Begin The star is an ellipsoidal variable; the period was determined photometrically (H.W. Duerbeck, Astron. Astrophys., 61, 161, 1977) and the epoch is the time of the deeper minimum. The orbital inclination is estimated at 35 deg; with this value it is found that the binary probably consists of main-sequence stars of types A and K. System174Orbit1End System175Orbit1Begin Popper's elements supersede the only previous spectroscopic study of this system by S. Gaposchkin (Harvard Obs. Bull., No. 918, p. 12, 1946). The system was the first Algol-type system for which both masses were determined directly and has one of the most extreme mass-ratios. A circular orbit was assumed and the epoch given is the time of primary minimum. Classification of the secondary spectrum is difficult because only a few lines in the red region of the spectrum are visible. Photometric analysis yields an effective temperature for the secondary star corresponding to late G or early K spectral type. The most recent analysis of the light-curve is by B. Cester et al. (Astron. Astrophys., 62, 291, 1978) who analyzed BV observations obtained by R.H. Koch (Astron. J., 65, 139, 1960) and found i to be close to 80 deg and that the primary component gives about 0.77 of the total light in V. System175Orbit1End System176Orbit1Begin Coverage of the velocity curve is good and K and V0 are probably well determined. A circular orbit would fit the observations almost as well, and was adopted by Lucy & Sweeney. The star is now recognized as an ellipsoidal variable with the same period as the orbital period. It is the brighter component of A.D.S. 2622: companion 10.6m at 5.4". System176Orbit1End System177Orbit1Begin The Durchmusterung number is from the C.P.D. The system is of interest because it is the first central star in a planetary nebula (N.G.C. 1360) to have been shown to be a spectroscopic binary. Elements, which are derived from measures of the absorption lines H-beta and H-gamma only, are very provisional, even the period being still in doubt. The eccentricity was assumed to be zero. The epoch is an arbitrary zero of phase, close to the time of maximum positive velocity. System177Orbit1End System178Orbit1Begin The value of T given by Struve in his paper is apparently a misprint. The two components have nearly the same intensity. System178Orbit1End System179Orbit1Begin The spectrum is variable, and the variation may be periodic. The spectrum has previously been classified as A4, A8, F0. The light-curve does not agree in phase with the velocity-curve, and the velocity-curve shows a secondary minimum. It is clear that the velocity-curve is grossly distorted. K. Lassovsky (Astron. Nachr., 252, 221, 1934) finds i=87 deg and the light-ratio to be 0.67. S. Gaposchkin (Variable Stars, Harvard Monograph 5, p. 75, 1936) gives slightly different elements. One spectrogram obtained during primary eclipse seems to show a spectral type of about F5. System179Orbit1End System180Orbit1Begin The spectrum shows emission at H and K which, according to the Wilson-Bappu relation, corresponds to an absolute magnitude of +4.85 -- in good agreement with the spectral type. Carquillat et al. estimate that the invisible secondary may be a K dwarf and that the orbital inclination is at least 65 deg. Fekel (private communication) has detected the secondary in the red. System180Orbit1End System181Orbit1Begin As one of the brightest and most active members of the RS CVn group, this system has attracted much attention and a complete listing of papers about it is quite impracticable. Fekel's discussion supersedes that by B.W. Bopp and F.C. Fekel (Astron. J., 81, 771, 1976) which was cited in the Seventh Catalogue. The new elements do not differ much from the old, but are more precisely determined. A spectrophotometric study of the variable H-alpha emission was published by D. Fraquelli (Astrophys. J., 276, 243, 1984). Her elements from the absorption lines agree well with Fekel's. Those from the emission lines show a slight (violet) displacement of V0 and a much lower value of K2. The orbit was assumed circular after an elliptical solution showed the eccentricity not to be significant. The epoch is T0 for the more massive component, which has very strong H and K emission. Fekel's paper contains discussions of evolutionary models and the starspot hypothesis, and -- together with the other papers cited above -- is an excellent introduction to the extensive literature on this star. Some of the papers cited for HD 21242 in this Catalogue also contain discussions of this system. Radio flares were first observed by F.N. Owen (I.A.U. Circ., No. 2929, 1976). Special mention should be made of the Doppler imaging study by S.S. Vogt and G.D. Penrod (Publ. Astron. Soc. Pacific, 95, 565, 1983). The star is the brighter component of A.D.S. 2644: companion is 8.4m at 6.2". System181Orbit1End System182Orbit1Begin Unlikely to be a member of the Pleiades. System182Orbit1End System183Orbit1Begin Griffin claims this as the first spectroscopic orbit determined for an S-type star. Although the star is designated BD Cam, he questions the variability of its light. System183Orbit1End System184Orbit1Begin Not a member of the Pleiades. System184Orbit1End System185Orbit1Begin The epoch is T0. The spectral classification is a preliminary one, communicated by N. Houk to Salzer and Beavers. The invisible secondary is believed to be an F-type dwarf. System185Orbit1End System186Orbit1Begin Brighter component of A.D.S. 2726: companion 8.4m at 1.0". Previous investigations by F.C. Jordan (Publ. Allegheny Obs., 2, 63, 1910), H. Ludendorff (Astron. Nachr., 188, 211, 1911), A.B. Muller, Th. Walraven, and L. Woltjer (Bull. Astron. Inst. Netherl., 13, 51, 1956). New observations by A. Blaauw and T.S. van Albada (Astrophys. J., 137, 791, 1963) fit Jordan's velocity-curve. Lynds used Sterne's method for small eccentricities. The star shows a light variation of about 0.03m with half the orbital period. This variation probably arises from ellipticity. There is some evidence for irregularity in this variation. Spectral classification is by W.W. Morgan, A.D. Code, and A.E. Whitford, (Astrophys. J. Supp., 2, No. 14, 1956). W.A. Hiltner (Astrophys. J. Supp., 2, No. 24, 1956) gave B1 II. Petrie(I) found Delta m=1.26. System186Orbit1End System187Orbit1Begin Petrie found Delta m=0.31. From his empirical mass-luminosity relation he estimated that i=19 deg. System187Orbit1End System188Orbit1Begin Epoch is T0. Star is a member of the Pleiades. System188Orbit1End System189Orbit1Begin Epoch is an arbitrary zero: T0 is about 0.72d later. Brighter component of A.D.S. 2750: companion 11.6m at 64.7". System189Orbit1End System190Orbit1Begin Epoch is an arbitrary zero: T0 is about 0.80d later. Brighter component of A.D.S. 2772: companion 9.4m at 3.2". System190Orbit1End System191Orbit1Begin The star is a member of the Pleiades and has been found from a model-atmosphere analysis to be an early-type analogue of the Am stars (P.S. Conti and S.E. Strom, Astrophys. J., 152, 483, 1968). System191Orbit1End System192Orbit1Begin This is the first binary showing a double-lined spectrum to be detected in the Pleiades. Orbits were published almost simultaneously by J.A. Pearce (Publ. Astron. Soc. Pacific, 10, 435, 1957) and Abt. Both orbits are good, and there is little reason for choosing between them. Abt has fewer observations than Pearce, but they were obtained with a spectrograph of higher dispersion. Abt's value of the period is probably to be preferred to Pearce's slightly longer one, but Pearce was probably more nearly correct in assuming a circular orbit. Pearce's value of K1 and K2 are both larger than Abt's values. This is especially pronounced for K2. Although probably not significant, these differences are worrying. Pearce found Delta m=1.11 from measures of the equivalent width of H-gamma in the two component spectra; he classified the spectra as A0 and A1. Abt estimated Delta m to be 1.4m, and tentatively classified the secondary as an Am star. Abt believes there may be shallow eclipses. System192Orbit1End System193Orbit1Begin Listed in I.D.S. as L.D.S. 104. Companion is 8.0mag at 1480". System193Orbit1End System194Orbit1Begin No measures of the secondary component have been made but the star displays a composite spectrum. Pedoussaut et al. quote an unpublished estimate of Delta m(pg)=0.8, made by Markowitz. They suggest that the system may sometimes be resolvable by speckle interferometry. The spectrum shows H and K emission. System194Orbit1End System195Orbit1Begin The period and orbital elements were derived by Morbey and Brosterhus from data published at several observatories -- principally Allegheny. A small-amplitude variation (less than 0.1m) is reported by O.M. Kolykhalova, A.V. Mironov and V.G. Moshkalev (Peremm. Zvezdy, 21, 105, 1978). They believed the system to be an eclipsing binary with a period of 22.58d. The spectroscopic observations do not fit that period, whereas the photometric observations, plotted on the spectroscopic period, give a light-curve resembling that of an ellipsoidal variable. New observations by B.E. Martin and D.P. Hube (Inf. Bull. Var. Stars, No. 3240, 1988) support that result. System195Orbit1End System196Orbit1Begin A member of the Pleiades (Atlas) erroneously listed as 28 Tau in the Sixth Catalogue. The star is also the brighter component of A.D.S. 2786. The 6.8m companion at 0.4" is uncertain however, and cannot be identified with the spectroscopic companion. The epoch given is T0. Lucy & Sweeney adopt a circular orbit. System196Orbit1End System197Orbit1Begin A member of the Pleiades whose duplicity was discovered by H.A. Abt et al., (Astrophys. J., 142, 1604, 1965). Pearce and Hill used the observations by Abt et al. as well as Victoria observations to obtain the elements given here. They assumed a circular orbit (in accord with the conclusion of Lucy & Sweeney) and the epoch is the time when the velocity is equal to the systemic velocity and decreasing. Apart from a difference in V0, the agreement between the two sets of elements is satisfactory. The star is the brightest component of A.D.S. 2786 and has companions of 9.7m and 8.9m at 3.2" and 10.2". System197Orbit1End System198Orbit1Begin This interesting system which belongs to the Hyades and contains a white dwarf continues to attract attention. Two orbital studies have been published since the appearance of the Seventh Catalogue (R. Gilmozzi and P. Murdin, Mon. Not. Roy. Astron. Soc., 202, 587, 1983 and E. Hamzaoglu and F. Sabbadin, Inf. Bull. Var. Stars, No. 2092, 1982). Young's study still has the smallest formal errors and is retained here. The agreement between studies is good, however, and justifies the higher quality grade given for the system. The work of Gilmozzi and Murdin is also important for its spectrophotometric study of the H, K and H-alpha lines. Other spectrophotometric investigations have so far been published only in abstract form. In one (B. Bois, S.W. Mochnacki and H.H. Lanning, J. Roy. Astron. Soc. Can., 79, 235, 1985) it is suggested that there is a third body in the system. The epoch is the time of primary minimum (eclipse of the white dwarf). Two photometric discussions have also been published since the Seventh Catalogue: C. Ibanoglu (Astrophys. Space Sci., 57, 219, 1978) and S. Rucinski (Acta Astron., 31, 37, 1981). The older study by B. Cester and M. Pucillo (Astron. Astrophys., 46, 197, 1976), giving an orbital inclination of about 80 deg and a fractional luminosity (in u) for the K-type component of 0.77 still appears valid. System198Orbit1End System199Orbit1Begin Epoch is T0. Spectral type of secondary is estimated after using the mass-luminosity relation to determine the mass of the primary. Circular orbit assumed. System199Orbit1End System200Orbit1Begin Based on the observations of A. Blaauw and T.S. van Albada (Astrophys. J., 137, 791, 1963) this set of elements, for which a circular orbit is assumed, appears to be a distinct improvement over theirs. Epoch is T0. System200Orbit1End System201Orbit1Begin System201Orbit1End System202Orbit1Begin The paper by Baade et al. contains both photometric and spectroscopic results. Rotational broadening of the F2 spectrum makes it hard to measure, however, and the spectroscopic elements should be regarded as preliminary. In particular, the orbital eccentricity is uncertain and the orbit should probably be regarded as circular. The epoch is the time of primary minimum. We have assumed that the value given for omega, by Baade et al., is in radians. Combination of photometric and spectroscopic data leads to a value for the mass of the F2 star considerably lower than the expected main-sequence value. The invisible secondary does not seem to be a main-sequence star either. The photometric solution gives an orbital inclination of 83 deg and a fractional luminosity (in V) for the primary star of 0.86. System202Orbit1End System203Orbit1Begin In the Seventh Catalogue doubt was expressed whether or not X Per was correctly identified with the X-ray source 4U 0352 +30 and whether or not the observed radial-velocity variation was real. The first doubt has been laid to rest and the second intensified. G.D. Penrod and S.S. Vogt (Astrophys. J., 299, 653, 1985) claim that the velocity variations found by Hutchings et al. are in fact only the results of variable asymmetric emission components in the higher Balmer lines. The elements given should therefore be looked upon with considerable reserve although, presumably, the star is a binary of some kind. The epoch would be T0, if the observations are correctly interpreted as velocity variations. The star is the brighter component of A.D.S. 2859: companion is 12.0m at 22.5". System203Orbit1End System204Orbit1Begin The elements given in the Catalogue supersede those obtained by W.E. Harper (Publ. Dom. Astrophys. Obs., 4, 161, 1928). Another recent set of elements was determined by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976). All three sets agree well, although this is partly because Abt and Levy included Harper's observations in their solution. The two spectra are similar; the classification is taken from the paper by Abt and Levy. Two faint and distant companions are listed in I.D.S. System204Orbit1End System205Orbit1Begin Photometric observations by M.B.K. Sarma and N.B. Sanwal (Astrophys. Space Sci., 74, 41, 1981) appear to have stimulated this spectroscopic investigation. It is based on eleven plates of only moderate dispersion. No sign of the secondary spectrum is seen. The epoch is the time of primary minimum. Nakamura, Yamasaki and Kitamura also re-analyze the light curve. Their solution differs from that of Sarma and Sanwal but the orbital inclination appears to be around 75 deg and the fractional luminosity of the brighter star (in V) about 0.9. System205Orbit1End System206Orbit1Begin Epoch is T0. Acker draws attention to the fact that the spectral type is that of a normal A star. System206Orbit1End System207Orbit1Begin Not a member of the Pleiades. D.P. Hube (private communication) finds that new observations are not satisfied by the period given by Pearce and Hill. System207Orbit1End System208Orbit1Begin The component assigned the suffix `2' by Imbert is the one occulted at primary eclipse. From an approximate solution of the only available light-curve -- a photographic one by W. Strohmeier and R. Knigge (Veroff. Remeis-Sternw., 5, No. 6, 1960) -- Imbert estimates that the orbital inclination is nearly 89 deg and that the components differ by about 0.2m in visual magnitude. Imbert also estimates spectral types of G8 and G0, compared with the H.D. type, F8, given in the Catalogue. A modern light-curve of this system is very much needed. System208Orbit1End System209Orbit1Begin The new orbit by Lacy and Frueh supersedes that derived by A. Young (Publ. Astron. Soc. Pacific, 87, 717, 1973) and quoted in the Seventh Catalogue. The spectral types are inferred from the colour indices and are not direct classifications. Lacy and Frueh also studied the light-curve and found an orbital inclination close to 90 deg and a light ratio in V of about 8.5:1. The orbital eccentricity appears to be real and there is evidence for apsidal motion with a period of about 140 years. Photometric observations of the system were also obtained by D.S. Hall, R.H. Gertken and E.W. Burke (Publ. Astron. Soc. Pacific, 82, 1077, 1970) and discussed by M. Mezzetti et al. (Astron. Astrophys., 42, 15, 1980). Two companions are listed in I.D.S., the brighter, suggested by Lacy and Frueh to be physically associated with the close pair, is 9.4m at 39.3". System209Orbit1End System210Orbit1Begin The spectral classification is by R.O. Redman (Publ. Dom. Astrophys. Obs., 4, 325, 1930); although he provided no luminosity classification, he observed the star in the course of a programme of observing K giants. The magnitude given is from the H.D. Catalogue for reasons discussed by Griffin. System210Orbit1End System211Orbit1Begin The new spectroscopic (Reticon) observations of this system by Fekel and Tomkin supersede all earlier investigations (C. Casini, P. Galeotti and G. Guerrero, Contr. Oss. Astron. Milano-Merate, No. 288, 1968); E.G. Ebbighausen and O. Struve (Astrophys. J., 124, 507, 1956); D.B. McLaughlin, Publ. Michigan Obs., 6, 39, 1932; F.C. Schlesinger, Publ. Allegheny Obs., 3, 173, 1914 and E.F. von Aretin, Gottingen Astron. Mit., 15, 1, 1913). Fekel and Tomkin have detected the secondary component with complete certainty and have conclusively demonstrated the existence of a third body moving in an unusually short-period orbit. Elements of both orbits can now be regarded as reasonably well determined. The variation due to motion of the close pair in the long-period orbit shows up in the observed velocities of both visible components. The elements given in the Catalogue are those found if the short-period orbit is assumed to be circular (the epoch is the time of primary minimum). A small eccentricity cannot be entirely ruled out, and adopting one brings the elements derived for the long-period orbit, from each component, into better agreement. Interaction between the orbits -- which must be nearly coplanar, since no variation in eclipse depths is observed -- such as apsidal motion and nodal regression, may lead to periodic variations in the orbital elements of the close pair, which may be detected in the future. The spectral type of the primary star is agreed upon by several investigators. That given for the secondary star was derived by G. Grant (Astrophys. J., 129, 78, 1959) and found by Fekel and Tomkin to be in agreement with their own estimates (although they put the star in luminosity class V). The magnitude difference between primary and secondary is estimated to be Delta V=2.3m. The third star is invisible, but its mass is estimated to be 0.7 MSol and it is probably a K dwarf. Photometric analyses by J.B. Hutchings and G. Hill (Astrophys. J., 166, 373, 1971) and B. Cester et al. (Astron. Astrophys., 62, 291, 1978) do not entirely agree, but indicate that i is close to 80 deg. Fekel and Tomkin favour the result i=76 deg, obtained by Cester et al., since this requires the system to be semi-detached. System211Orbit1End System212Orbit1Begin The new spectroscopic (Reticon) observations of this system by Fekel and Tomkin supersede all earlier investigations (C. Casini, P. Galeotti and G. Guerrero, Contr. Oss. Astron. Milano-Merate, No. 288, 1968); E.G. Ebbighausen and O. Struve (Astrophys. J., 124, 507, 1956); D.B. McLaughlin, Publ. Michigan Obs., 6, 39, 1932; F.C. Schlesinger, Publ. Allegheny Obs., 3, 173, 1914 and E.F. von Aretin, Gottingen Astron. Mit., 15, 1, 1913). Fekel and Tomkin have detected the secondary component with complete certainty and have conclusively demonstrated the existence of a third body moving in an unusually short-period orbit. Elements of both orbits can now be regarded as reasonably well determined. The variation due to motion of the close pair in the long-period orbit shows up in the observed velocities of both visible components. The elements given in the Catalogue are those found if the short-period orbit is assumed to be circular (the epoch is the time of primary minimum). A small eccentricity cannot be entirely ruled out, and adopting one brings the elements derived for the long-period orbit, from each component, into better agreement. Interaction between the orbits -- which must be nearly coplanar, since no variation in eclipse depths is observed -- such as apsidal motion and nodal regression, may lead to periodic variations in the orbital elements of the close pair, which may be detected in the future. The spectral type of the primary star is agreed upon by several investigators. That given for the secondary star was derived by G. Grant (Astrophys. J., 129, 78, 1959) and found by Fekel and Tomkin to be in agreement with their own estimates (although they put the star in luminosity class V). The magnitude difference between primary and secondary is estimated to be Delta V=2.3m. The third star is invisible, but its mass is estimated to be 0.7 MSol and it is probably a K dwarf. Photometric analyses by J.B. Hutchings and G. Hill (Astrophys. J., 166, 373, 1971) and B. Cester et al. (Astron. Astrophys., 62, 291, 1978) do not entirely agree, but indicate that i is close to 80 deg. Fekel and Tomkin favour the result i=76 deg, obtained by Cester et al., since this requires the system to be semi-detached. System212Orbit1End System213Orbit1Begin The one paper contains the first photometric and spectroscopic studies of this system. The epoch is the time of primary minimum. The spectral classification is by the authors and is somewhat earlier than has previously been thought. Analysis of the light-curve yields i=90 deg and a fractional luminosity in V of 0.97 for the visible component. The photometric observations alone are fitted best if the mass-ratio is 0.32, but this value combined with the spectroscopic mass function would place the primary component below the main sequence. A mass-ratio of 0.2 would reconcile the spectroscopic and photometric observations more easily, but would not represent the light-curve so well. System213Orbit1End System214Orbit1Begin There is some evidence for variable line intensities. Previous investigations by C. Hujer (Astrophys. J., 67, 399, 1928) and O. Struve (Astrophys. J., 65, 300, 1927). System214Orbit1End System215Orbit1Begin Although our understanding of this system has much increased during the last decade, no new orbital elements have been published since those of Hiltner and Hardie. That the eccentricity is spurious was long suspected, and was confirmed by the publication, while the Seventh Catalogue was in press, of an infrared light-curve by B.B. Bookmyer (Publ. Astron. Soc. Pacific, 89, 533, 1977). The secondary minimum is clearly defined and only slightly displaced from midway between successive primary eclipses. The spectroscopic values of e and omega cannot represent the true orbit and therefore the value of K (and quantities derived from it) is also suspect. The spectral types are taken from M. Plavec's IUE study of the system (Astrophys. J., 272, 206, 1983), and depend on fitting model atmospheres rather than on traditional classification. They agree well with those derived by G. Grant (Astrophys. J., 129, 62, 1959) from UBV photometry. Other photometric studies (based on Grant's observations) have been published by M.I. Lavrov and N.V. Lavrova (Izv. Astron. Obs. Engelhardt, 41-2, 196, 1976), A.G. Tsouroplis (Astrophys. Space Sci., 47, 361, 1977) and F. Mardirossian et al. (Astron. Astrophys. Supp., 40, 57, 1980). Grant's conclusions that the orbital inclination is close to 90 deg and that the brighter component gives about 0.96 of the light in V do not appear to need appreciable modification. The period is variable. The sign of V0 given by Hiltner and Hardie is obviously incorrect and has been changed. The system is famous for the discovery of a `ring' around the B-type star by A.B. Wyse (Lick Obs. Bull., 19, 42, 1934) and A.H. Joy (Publ. Astron. Soc. Pacific, 54, 21, 1942). An important discussion of this feature, based on spectroscopy at high time-resolution, has been published by R.H. Kaitchuck and R.K. Honeycutt (Astrophys. J., 258, 224, 1982). There is a faint visual companion about 1" away (P.L. Battistini, M. Fracassini and L.E. Pasinetti, Astrophys. Space Sci., 14, 438, 1971). System215Orbit1End System216Orbit1Begin Chochol's spectroscopic observations cover the primary velocity-curve much better than do those of E. Budding (Astrophys. Space Sci., 36, 329, 1975) or A.J. Wesselink (Leiden Ann., 17, Pt. 3, 30, 1941). The observations of the secondary component are, however, few and uncertain, and the value of K2 should be treated with considerable reserve. The epoch is the time of primary minimum, although it is not quite clear just which ephemeris Chochol used in the calculation of phases. He assumed e=0. Chochol also published photometric observations and analyzed them along with the UBV observations of M. Kitamura and A. Yamasaki (Tokyo Astron. Bull, No. 220, 2563, 1972). He found an orbital inclination close to 80 deg and a fractional luminosity in V, for the primary component, of 0.74. Other photometric studies have been published by E. Budding (Astrophys. Space Sci., 46, 407, 1977) and F. Mardirossian (Astron. Astrophys., 86, 264, 1980). The latter authors suggest as did Chochol, apparently independently, that the system is semi-detached. The star is the second brightest member of the visual multiple A.D.S. 2984 (N.G.C. 1502). System216Orbit1End System217Orbit1Begin No epoch is given and the velocity-curve is said to be subject to `erratic changes'. A recent abstract (S.L. Morris and C.T. Bolton, Bull. Am. Astron. Soc., 18, 985, 1986) states that the true period is 0.91d, but no data are given. All elements should be considered very uncertain. System217Orbit1End System218Orbit1Begin A silicon star that according to K.D. Rakos (Lick Obs. Bull., 5, 227, 1962) shows small light variations (about 0.03m) in a period of 11.94 days. System218Orbit1End System219Orbit1Begin The observations and solution by Popper supersede those by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 3, 184, 1925). The epoch is the time of primary minimum. The line of apsides rotates in a period of 76.55 years (N. Gudur, Astrophys. Space Sci., 57, 17, 1978); in 1974 omega was 285 deg. A recent photometric study by E. Woodward and R.H. Koch (Astrophys. Space Sci., 129, 187, 1987) leads to an orbital inclination close to 82 deg and a fractional luminosity for the primary star (in yellow light) of 0.57. Spectrophotometry by G.L. Clements and J.S. Neff (Astrophys. J. Supp., 41, 1, 1979) gives a difference in bolometric magnitude of 0.65m. Those authors also suggest a somewhat earlier spectral type (between B3 and B4). The star is the brightest component of A.D.S. 2990: companions are 8.8m at 1" and 12.6m at 36". System219Orbit1End System220Orbit1Begin The secondary component is not visible except on two traces obtained at Palomar. Griffin and Gunn estimate that it is a late K dwarf, with Delta V somewhere between 1.5m and 2.0m. Radial velocity, proper motion and apparent magnitude of the star are consistent with its membership in the Hyades. System220Orbit1End System221Orbit1Begin A two-spectra binary containing two equal Am stars, for which only a few observations were available until recently. The spectra are classified as A1, A3V, A3 from the K line, the hydrogen lines, and the metallic lines respectively. The epoch is the time of maximum positive radial velocity for the marginally more massive component. Abt and Levy estimate the orbital inclination to be 62 deg and the rotational velocities (v sin i) to be in the neighbourhood of 30 km/s. System221Orbit1End System222Orbit1Begin The new observations do not appear to be much better than those by O. Struve (Astrophys. J., 106, 92, 1947) primarily because they are fewer in number. The analysis is more refined, however, and attempts to take account of the fact that the observed velocities are not those of the centre of mass of the two components. The values given for K1 and K2 have been corrected for this effect. The epoch is the time of primary minimum. Nesci et al. analyzed anew the BV light-curves obtained by M. Huruhata, T. Dambaru and M. Kitamura (Publ. Astron. Soc. Japan, 6, 217, 1954) using the newly derived mass ratio. They found an inclination of 82 deg and a fractional luminosity in V for the primary component of 0.36. Other photometric studies have been published by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978) and C. Maceroni et al. (Astron. Astrophys. Supp., 49, 123, 1982), superseded by the new investigation. Reports of variable polarization (V.A. Oshchepkov, Comm. 27, I.A.U. Inf. Bull. Var. Stars, No. 782, 1973) have not been confirmed. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System222Orbit1End System223Orbit1Begin Earlier investigation by J.B. Cannon yields results in good agreement with these elements. The probable errors of Johnson's and Neubauer's elements are low, and the orbit is probably well known. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. Star is brightest component of A.D.S. 3071: closest companion is 11.8m at 14.8". System223Orbit1End System224Orbit1Begin Spectral classification is by Slettebak quoted by Osawa. Also according to Osawa, Bidelman classified the star as G5 II and A or B. Osawa points out that there is a possibility of observing eclipses. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. System224Orbit1End System225Orbit1Begin Membership of this system in the Hyades was questioned in the past because of an apparently discordant radial velocity. The discovery by Griffin and Gunn that the star is a double-lined binary has removed the anomaly. Griffinn and Gunn estimate Delta V=0.5m from the relative depths of radial-velocity traces on their spectrometer. They find that spectral types of G4 V and G7 V would be consistent with their observations. System225Orbit1End System226Orbit1Begin This system has attracted attention since its discovery as a flaring radio source (R.M. Hjellming and C. Wade, Nature, 242, 250, 1973). Orbital elements were published nearly simultaneously by R. Rajamohan and M. Parthasarathy (Pramana, 4, 153, 1975, Kodaikanal Preprint, No. 74), S.C. Wolff and R.J. Wolff (Publ. Astron. Soc. Pacific, 86, 176, 1974) and the authors cited in the Catalogue. Older observations (J.F. Heard, Astrophys. J., 87, 72, 1938, W.E. Harper, Publ. Dom. Astrophys. Obs., 4, 309, 1930 and J.B. Cannon, Publ. Dom. Obs., 1, 285, 1911) were included by Hill et al. in their discussion of the long-period orbit. Since the publication of the Seventh Catalogue a further study of the short-period orbit has been published by H.W. Duerbeck and A. Schettler (Acta Astron., 29, 225, 1979). Their results confirm those of Hill et al. and they also find the systemic velocity to be roughly in agreement with expectations from the long-period orbit. Their photometric observations show the short-period system to be an ellipsoidal variable. There is a possibility that the third body eclipses the primary star. Only one spectrum is visible and Duerbeck and Schettler did not find any effects of blending in the hydrogen lines, as were suspected by Hill et al.. Duerbeck and Schettler suggest that the secondary is an F5 subgiant. Rotational broadening of the only visible spectrum makes accurate measurement of velocities difficult. System226Orbit1End System227Orbit1Begin This system has attracted attention since its discovery as a flaring radio source (R.M. Hjellming and C. Wade, Nature, 242, 250, 1973). Orbital elements were published nearly simultaneously by R. Rajamohan and M. Parthasarathy (Pramana, 4, 153, 1975, Kodaikanal Preprint, No. 74), S.C. Wolff and R.J. Wolff (Publ. Astron. Soc. Pacific, 86, 176, 1974) and the authors cited in the Catalogue. Older observations (J.F. Heard, Astrophys. J., 87, 72, 1938, W.E. Harper, Publ. Dom. Astrophys. Obs., 4, 309, 1930 and J.B. Cannon, Publ. Dom. Obs., 1, 285, 1911) were included by Hill et al. in their discussion of the long-period orbit. Since the publication of the Seventh Catalogue a further study of the short-period orbit has been published by H.W. Duerbeck and A. Schettler (Acta Astron., 29, 225, 1979). Their results confirm those of Hill et al. and they also find the systemic velocity to be roughly in agreement with expectations from the long-period orbit. Their photometric observations show the short-period system to be an ellipsoidal variable. There is a possibility that the third body eclipses the primary star. Only one spectrum is visible and Duerbeck and Schettler did not find any effects of blending in the hydrogen lines, as were suspected by Hill et al.. Duerbeck and Schettler suggest that the secondary is an F5 subgiant. Rotational broadening of the only visible spectrum makes accurate measurement of velocities difficult. System227Orbit1End System228Orbit1Begin The old single-spectrum orbit by R.F. Sanford (Astrophys. J., 59, 356, 1924) has been recently superseded by two independent investigations that have revealed the presence of the spectra of both components. One of these investigations is that by Griffin et al. cited in the Catalogue, the other is by R.D. McClure (Astrophys. J., 254, 606, 1982). In terms of accuracy, there is not much to choose between these two good orbits, but Griffin et al. cover the velocity-curve of the primary component more nearly completely than does McClure. Their results agree well, except for V0, which may be partly affected by differences in zero points. The possibility of an underlying real variation in V0 is not, however, ruled out by Griffin et al. The epoch is T0. An important discovery by McClure was that the system displays eclipses and is therefore a very useful check on estimates of the distance to the Hyades, of which H.D. 27130 is a member. McClure estimates an orbital inclination of about 85 deg. Griffin et al. find that the observed magnitudes and colours can be fitted with individual stars of spectral types G6 V and K6 V, differing in V magnitude by 2.3m which is consistent with the appearance of their radial-velocity traces. System228Orbit1End System229Orbit1Begin System229Orbit1End System230Orbit1Begin This is one of three possible members of the Hyades, investigated by Griffin, Mayor and Gunn, that turned out to be two-spectra binaries. The orbit was assumed circular and the epoch is T0. Griffin et al. estimate the magnitude difference between the components as Delta B=1.3m (from the radial-velocity traces). This system does belong to the Hyades. System230Orbit1End System231Orbit1Begin This is another two-spectra binary belonging to the Hyades. Although eclipses were looked for, none have been detected -- B.G. Jorgensen and E.H. Olsen, (Inf. Bull. Var. Stars, No. 652, 1972), but the system must have a high orbital inclination. The double lines were first discovered by R. v.d.R. Woolley, D.H.P. Jones and L.M. Mather (Roy. Obs. Bull., No. 23, 1960). Batten and Wallerstein estimated Delta m (photographic)=0.42. McClure (Astrophys. J., 254, 606, 1982) obtained a few new observations to refine the elements. His changes were all within the observational errors, but he suggested the period should be changed to 75.664d. System231Orbit1End System232Orbit1Begin Another Hyades spectroscopic binary. Unfortunately the lines of the A-type component are too broad for accurate measurement and mass determination. The value of K given refers to the G-type star. Deutsch et al. point out the possibility of observing lunar occultations of this system. H.A. McAlister (Astrophys. J., 212, 459, 1977) has resolved the components by speckle interferometry and is continuing his observations. A distant companion (10.7m at 166.4") is listed in I.D.S. System232Orbit1End System233Orbit1Begin Although no attempt has been made to determine the orbital elements since Struve's, his values are now known to be quite inadequate as a description of the system. Epoch is time of primary minimum. A thorough (IUE and optical) spectrophotometric study of the system was recently published by J.J. Dobias and M.J. Plavec (Publ. Astron. Soc. Pacific, 99, 159, 1987). The spectral types given were taken from this paper and were derived by fitting model atmospheres to the observed flux. Dobias and Plavec give Delta m (visual)=1.1. It appears likely that the mass-ratio is very small. The light-curve is known to vary in shape; D.S. Hall and T. Stuhlinger (Acta Astron., 28, 207, 1978) analyze modern UBV light-curves. It appears that many of the difficulties in interpretation of both light-curve and velocity-curve arise from an accretion disk surrounding the primary star. Hall and Stuhlinger therefore present their results very tentatively, but they find an orbital inclination close to 86 deg. New spectroscopic observations are highly desirable. System233Orbit1End System234Orbit1Begin A `manganese star' that has common proper motion with 56 Tau. Epoch is T0. System234Orbit1End System235Orbit1Begin Only H-gamma and lambda 4481 were measured on most plates, but the elements appear to be well determined. According to I.D.S. there is a suspected companion at 0.1", and an 11.8m companion at 49". Luyten derives slightly different elements from these observations. System235Orbit1End System236Orbit1Begin Another binary in the Hyades. Wright and Northcott find Delta m=0.07 by Petrie's method. If the components obey the mass-luminosity law, the orbital inclination is 51 deg. System236Orbit1End System237Orbit1Begin Abt gives the spectral types from the K line, the hydrogen lines, and the metallic lines as A5, F2, and F2 respectively. Lucy & Sweeney adopt a circular orbit. Two faint companions are listed in I.D.S.: 12.7m at 7.0" and 12.2m at 79.3". System237Orbit1End System238Orbit1Begin Star is brighter component of A.D.S. 3169. Companion is two magnitudes fainter. Several orbits have been computed. Because period of the spectroscopic binary is apparently an exact number of days, the distribution of observations is very poor. Lucy & Sweeney confirm the reality of the orbital eccentricity. System238Orbit1End System239Orbit1Begin The orbital elements are derived from a combination of the available photographic and photoelectric observations. The standard deviation of individual observations, although absolutely small, is a substantial fraction of the amplitude. The orbit is considered only preliminary by Griffin and Gunn themselves. The star is an important member of the Hyades. A 12.m6 companion at 107" is listed in I.D.S. System239Orbit1End System240Orbit1Begin Another binary in the Hyades. Griffin et al. report no sign of a secondary `dip' in their traces. System240Orbit1End System241Orbit1Begin The new orbit by Abt and Levy is probably an improvement on all earlier discussions (K. Jantzen, Astron. Nachr., 196, 117, 1913; W.E. Harper Publ. Dom. Astrophys. Obs., 6, 217, 1935 and H.A. Abt Astrophys. J. Supp., 6, 37, 1961). The eccentricity was taken as zero after a preliminary solution showed it to be very small and the epoch is T0. Apart from the eccentricity, the new orbit is in good agreement with the older ones. Abt and Levy give the spectral types as A1.5, A8 and F2 from the K line, hydrogen lines and metallic lines, respectively. System241Orbit1End System242Orbit1Begin Another two-spectra binary that is probably in the Hyades. Observations have had to be corrected for pair-blending of the two spectra. The period given is the apparent period. Griffin et al. estimate that the components have spectral types of G6 V and K5 V and differ in visual magnitude by 2.0m. They note a faint visual companion of about 14th magnitude some 8" to 10" away. System242Orbit1End System243Orbit1Begin Another binary in Hyades. System243Orbit1End System244Orbit1Begin Abt finds a range of nearly 30 km/s from observations obtained at four observatories. As he points out, the elements lead to a rather large mass-function. E.G. Frost, S.B. Barrett and O. Struve (Publ. Yerkes Obs., 7, Part 1, 1929) report double lines on four plates, but no other observers have reported them. The star should be further observed. According to I.D.S. there is an 11.1m companion at 137". Any physical connection seems doubtful. System244Orbit1End System245Orbit1Begin Luyten's elements are preferred to those originally derived by W.E. Harper (Publ. Dom. Astrophys. Obs., 4, 316, 1930) because Harper had to fix T to obtain a solution. Brighter component of A.D.S. 3267: companion 13.0m at 39.6". Epoch is T0. Lucy & Sweeney agree with Luyten in adopting a circular orbit. System245Orbit1End System246Orbit1Begin Another spectroscopic binary in the Hyades. System246Orbit1End System247Orbit1Begin Another spectroscopic binary in the Hyades. The spectral type is either G8 V or K0 V. Some authorities also give slightly different values for the apparent magnitude. Griffin et al. give both the apparent and the true orbital periods. That quoted is the apparent. System247Orbit1End System248Orbit1Begin 2Earlier investigations by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 2, 63, 1915) and R.M. Petrie (Publ. Astron. Soc. Pacific, 52, 286, 1940). Values of P, e, and omega agree well for all three orbits. Ebbighausen believes his larger value of K is a result of the greater number of spectrograms he obtained near the ascending node, and does not reflect real changes in the elements. The difference in V0 between his and Plaskett's orbits (3 km/s) is probably an instrumental effect, but the possibility of a third body in the system cannot be ruled out. The `wave effect' found by Plaskett does not exist. None of the investigators has been able to detect the secondary spectrum. Star is a member of the Hyades. It is listed in I.D.S. with theta 1 Tau, separation 337". System248Orbit1End System249Orbit1Begin Another spectroscopic binary in the Hyades. The spectrum is broadened by rotation and is also somewhat early in type for the Palomar radial-velocity spectrometer. For these reasons individual velocity measurements are not as precise as is usual with this instrument. System249Orbit1End System250Orbit1Begin Hube finds a luminosity ratio at lambda 4482 between 1.37 and 1.49. If the stars lie on the main sequence, he estimates an orbital inclination of 54 deg. System250Orbit1End System251Orbit1Begin Another spectroscopic binary in the Hyades. Complete phase coverage is difficult to obtain because the orbital period is so close to one year. System251Orbit1End System252Orbit1Begin Another spectroscopic binary in the Hyades. System252Orbit1End System253Orbit1Begin This system was first discovered as an X-ray source and then identified with a star believed to be still contracting to the main sequence (E.D. Feigelson and G.A. Kriss, Astrophys. J., 248, L35, 1981). The epoch is the time of conjunction with star A in front (the spectra are almost equal). The eccentricity should probably be taken as zero, since it is only half its mean error, no value is given for omega. This appears to be the first system detected with components still contracting to the main sequence. System253Orbit1End System254Orbit1Begin Lower half of velocity-curve is not well covered. Abt notes that O.J. Lee (Astrophys. J., 32, 300, 1910) reported double lines. Lucy & Sweeney adopt a circular orbit. System254Orbit1End System255Orbit1Begin The period is 10,470 days. Sanford's orbital elements, which supersede the results of his own earlier investigations (Astrophys. J., 43, 268, 1931, Publ. Astron. Soc. Pacific, 60, 251, 1948), are still the only ones available. The spectral types given are derived from a spectrophotometric study (including IUE observations) by D.L. Harmer et al. (Mon. Not. Roy. Astron. Soc., 204, 927, 1983) and are not based on traditional methods of classification. Harmer et al. estimate a Delta V of about 3 m. It is possible that the early-type component is a Be star. They estimate a distance of 320 parsecs and find it difficult to reconcile the spectroscopic and photometric results with the astrometric orbit published by A.A. Wyller (Astron. J., 62, 384, 1962). Wyller found i=82 deg, omega=145 deg. McAlister was unable to resolve the system by speckle interferometry (Publ. Astron. Soc. Pacific, 88, 317, 1976, 90, 288, 1980). Sanford thought the residuals from his velocity-curve to be large, but he could find no periodicity in them. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. System255Orbit1End System256Orbit1Begin The orbit was assumed circular and the epoch is T0. The magnitude difference between the components is estimated from the `dips' in the radial-velocity traces to be Delta B=2.5m. The system appears to be more distant than the Hyades cluster, but moving with it. Griffin et al. assign it to the Hyades moving group. System256Orbit1End System257Orbit1Begin The best set of elements still seems to be Wilson's although the following investigations have been published: Z. Daniel (Publ. Allegheny Obs., 3, 93, 1914); W.E. Harper (Publ. Dom. Obs., 1, 115, 1913 and Publ. Dom. Astrophys. Obs., 6, 218, 1935); and H.A. Abt (Astrophys. J. Supp., 6, 37, 1961). Luyten also computed the elements, using observations from the three earlier investigations. Harper proposed, in 1935, to modify the period to 3.57104d and Abt confirmed this, further modifying it to 3.571082d. Harper, in 1913, detected the secondary spectrum, and found a mass-ratio of 0.47. Abt also confirms this. Combined with Wilson's mass-function this would yield m_1 sin^3 i=3.4 MSol, m_2 sin^3 i=1.6 MSol. There is, however, a rather large difference in K1 as determined by Wilson and Harper. According to Abt, the spectral type is A3, A8, A7 by the K line, the hydrogen lines and the metallic lines, respectively. I.D.S. lists an 8.5m companion at 69.7". Petrie(II) found Delta m=2.31. Fekel (private communication) has detected the secondary spectrum in the red. System257Orbit1End System258Orbit1Begin Although this system was included in the study of Hyades binaries by Griffin et al., those authors do not commit themselves on the question of cluster membership. There is some difficulty in reconciling Palomar photographic observations with the photoelectric ones, which may indicate a small uncertainty in the period. But for that problem the orbit might well have merited a b quality. The orbit was taken to be circular after preliminary calculations showed that introducing an orbital eccentricity afforded no appreciable improvement. The epoch is T0. Griffin et al. draw attention to discordant measurements of magnitude. System258Orbit1End System259Orbit1Begin No new spectroscopic observations have been published since those of Struve et al. and the only photoelectric observations still appear to be those of M. Huruhata and M. Kitamura (Publ. Astron. Soc. Japan, 5, 102, 1953), F. Hinderer (J. Observateurs, 43, 161, 1960) and L. Binnendijk (Astron. J., 68, 22, 1963). The results of these observations were not entirely accordant and modern solutions (mainly from Binnendijk's observations -- S.W. Mochnacki and N.A. Doughty, Mon. Not. Roy. Astron. Soc., 156, 243, 1972, R.E. Wilson and E.J. Devinney, Astrophys. J., 182, 539, 1973, L. Binnendijk, Vistas in Astron., 21, 359, 1977, P.G. Niarchos, Astrophys. Space Sci., 58, 301, 1978, S.R. Jabbar and Z. Kopal, Astrophys. Space Sci., 92, 99, 1983) do not fully agree either. Estimates of the orbital inclination range from about 60 deg to 84 deg and of the fractional luminosity of the brighter star from about 0.55 to 0.86. New observations, both photometric and spectroscopic, would be valuable. The epoch is T0 calculated from the time of minimum given by Struve et al. (some photometric observers have reversed the designations of primary and secondary minima). The magnitudes are estimated from information in the photometric papers and are only approximately on the V scale. The system is a W UMa system displaying complete eclipses. It is the brighter component of A.D.S. 3559: companion 12.3m at 3.8". System259Orbit1End System260Orbit1Begin Both Luyten and Lucy & Sweeney have computed elements for this system under the assumption that the orbit is circular. System260Orbit1End System261Orbit1Begin The epoch is T0. The minimum magnitude is an approximate one drawn from the photometric observations. Light curves in B and V were published by M. Parthasarathy and M.B.K. Sarma (Astrophys. Space Sci., 72, 477, 1980) and analyzed by G. Giuricin and F. Mardirossian (Astron. Astrophys., 97, 410, 1981) who believe the invisible secondary to be a subgiant not in contact with the Roche lobe. They find an orbital inclination of 90 deg and a fractional luminosity (in V) of 0.97. Somewhat different results are published by A. Dumitrescu and R. Dinescu (Inf. Bull. Var. Stars, No. 1740, 1980) but their full analysis is not available. System261Orbit1End System262Orbit1Begin Another spectroscopic binary in the Hyades. System262Orbit1End System263Orbit1Begin Luyten gives different elements based on these observations. Petrie(II) found Delta m=1.91. System263Orbit1End System264Orbit1Begin Abt and Levy completely revised the earlier elements by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961), changing the period from 251 d to just under 39 d. They say that the new elements `must still be considered as marginal'. They consider a reported occultation component to be identical with the spectroscopic secondary. In Abt's first study, features in the spectrum were tentatively identified as arising from the secondary; they are not mentioned in the new work. Abt and Levy give the spectral types as A2, A7, A7 from the K line, hydrogen lines and metallic lines respectively. Together with sigma 2 Tau, the star forms a common-proper-motion pair which may belong to the Hyades. System264Orbit1End System265Orbit1Begin Another spectroscopic binary in the Hyades. Griffin et al. themselves describe these orbital elements as preliminary. The secondary spectrum is strong enough to affect the observed `dip' profile, but the available material is not yet sudegcient either to define the secondary velocity-curve or to guarantee that the primary velocity-curve is correctly determined. The authors suggest that the system consists of a K3 V and K7 V star with Delta V about 1.5m. System265Orbit1End System266Orbit1Begin The first investigation was by T.H. Parker (Report of the Chief Astronomer of Canada, 1, 166, 1910) which R.W. Tanner (Publ. David Dunlap Obs., 1, 473, 1949) showed to be based on an incorrect value for the period. Petrie and Ebbighausen rediscussed Parker's observations and presented new ones. Their values for the elements have been largely confirmed by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 36, 241, 1978) although possibly the orbit should be regarded as circular. The secondary spectrum is seen only on nine Victoria spectrograms and measurements of it are rather less certain than those of the primary. Petrie and Ebbighausen found Delta m=1.5 (by Petrie's method). The star has been resolved by speckle interferometry (H.A. McAlister et al., Astrophys. J. Supp., 51, 309, 1983). Two companions are listed in I.D.S.: 8.9m at 0.1" and 8.6m at 62.8". System266Orbit1End System267Orbit1Begin Although this star was investigated by Griffin and Gunn in the course of their study of Hyades radial velocities, they conclude that it is not a member of the cluster. It does share a common radial velocity and proper motion with H.D. 29836. System267Orbit1End System268Orbit1Begin Another spectroscopic binary in the Hyades. Griffin et al. are unable to confirm a companion reported by Luyten. System268Orbit1End System269Orbit1Begin The orbit was assumed to be circular and the epoch is T0. The star is the brighter member of A.D.S. 3409: companion is 6.8m at 9.2". The magnitude given in the Catalogue (taken from the paper by Lucke and Mayor) must refer to the combined light of these two stars. Other sources give 6.70m for A.D.S. 3409 A. System269Orbit1End System270Orbit1Begin The spectrum of the secondary component is seen during the total primary eclipse and appears to be that of a subgiant with H and K in emission. B. Gronbech (Comm. 27, I.A.U. Inf. Bull. Var. Stars, No. 956, 1975) finds the photoelectric colours are consistent with a K giant spectrum. The colours of the primary correspond to an F5 giant or an Am star. J. Gadomski (Acta Astron., 7, 83, 1957) discussed all available photographic observations and found i=83 deg. Gronbech gives Delta V=0.45. System270Orbit1End System271Orbit1Begin Although this star is included in the study of Hyades binaries by Griffin et al., it is definitely recognized not to be a member of the cluster. System271Orbit1End System272Orbit1Begin This set of elements supersedes that published earlier by A. Blaauw and T.S. van Albada (Astrophys. J., 137, 791, 1963). System272Orbit1End System273Orbit1Begin This is a Cepheid variable that is also a spectroscopic binary. In view of the long period, the orbital elements should be considered preliminary. Observations with IUE indicate an effective temperature of 12,000 K for the unseen secondary. To reconcile this with the mass-function, Welch and Evans suggest that the secondary itself is double. System273Orbit1End System274Orbit1Begin Binary nature of star was discovered by W.P. Bidelman (Astrophys. J., 111, 333, 1950), who first drew attention to the star's very unusual spectrum. Heard also published a preliminary report on the orbital elements in collaboration with O. Boshko (Astron. J., 60, 162, 1952). The elements seem to be well-determined from the David Dunlap observations for the epoch 1951-6. However, Heard found evidence that some sudden change apparently occurred in the orbital elements about the time that his observations began. Thus, although the elements are well determined, the question of how far they represent the orbital motion is still open. This should be borne in mind when interpreting the quality (b) assigned to this orbit. The light of the star is variable, but there are apparently no eclipses. System274Orbit1End System275Orbit1Begin Luyten derives similar elements from these observations. Lucy & Sweeney adopt a circular orbit. Bertaud and Floquet give the spectral type as A7 from the K line and F2 from the metallic lines. Fekel (private communication) has detected the secondary spectrum in the red. System275Orbit1End System276Orbit1Begin System276Orbit1End System277Orbit1Begin Another spectroscopic binary in the Hyades, which is the more important because both spectra are visible. The period given is the apparent period and the epoch is T0, the orbit being assumed circular. There is evidence for a slight variation in magnitude (of a few hundredths) which Griffin et al. attribute to spots on at least one component. The spectral type is not known directly, but is estimated from the photometric properties and the relative strengths of the two `dips' in the radial-velocity traces. The two spectral types are probably closely similar and Delta V is estimated to be 0.14m. The orbital inclination is probably below 30 deg. System277Orbit1End System278Orbit1Begin Another spectroscopic binary in the Hyades. One half of the velocity-curve is exceedingly well defined by observations of high precision. The other half, however, is only sketchily defined. From the relative depths of the `dips' in the radial-velocity traces, Delta V is estimated to be 0.31m. The minimum masses are close to those expected for stars of their spectral type and eclipses are possible. Griffin and Gunn also suggest that the system could be resolved interferometrically. A slightly different value of T is derived from the velocity-curve of the secondary component. System278Orbit1End System279Orbit1Begin This star is thought to be a `runaway' from N.G.C. 1502 (Cam OB1). Velocity variation has long been suspected, but the amplitude is small and the scatter of observations fairly large. The proposed period is very short for a binary containing a supergiant. Other periods have been suggested, including one of 46.8d (with a semi-amplitude nearly twice the value given in the Catalogue -- B. Bohannan and C.D. Garmany, Astrophys. J., 223, 908, 1978) but there is as yet no agreement amongst these investigators and others. System279Orbit1End System280Orbit1Begin Another Hyades spectroscopic binary. No spectral type is given by Griffin and Gunn (that given here is from the H.D. Catalogue). They do remark on a rotational broadening of the radial-velocity traces. System280Orbit1End System281Orbit1Begin This is another star included in the survey of the Hyades binaries that definitely does not belong to the cluster and is probably much further away. The primary velocity-curve is well defined but the observations of the secondary are few and (relatively) scattered. The spectral types are once again derived by fitting the observed magnitude difference and combined colours, rather than by direct classification. The period given is the apparent period. The magnitude difference between the components is estimated to be Delta V=1.92m (from the depths of the two `dips' in the radial-velocity traces). System281Orbit1End System282Orbit1Begin This is a dwarf nova of the SU UMa type. The magnitude, of course, is variable -- the value given appears to be that of the comparison star. No spectral type is given but the spectrum is said to be characterized by broad Balmer absorption lines. A circular orbit was assumed. The epoch is superior conjunction of the primary star. The systemic velocity is variable. System282Orbit1End System283Orbit1Begin Epoch is T0. Original observations were by R.H. Baker (Publ. Allegheny Obs., 1, 107, 1909). Luyten's computation has been preferred because Baker had to fix T in order to obtain a solution. Later observations by R. Bouigue and A. Castanet (J. Observateurs, 37, 1, 1954) tend to confirm these elements and give P=9.5201d. Lucy & Sweeney adopt a circular orbit. System283Orbit1End System284Orbit1Begin Although this binary, also in the Hyades, was included in the study by R.F. Griffin et al. (Astron. J., 90, 609, 1985) the investigation by Turner et al. gives results that seem preferable, although the latter group themselves suggest that the true period may be between the value they give and that (0.26d less) given by Griffin et al. whose formal uncertainties are smaller. The differences in V0 may arise partly from differences in velocity systems and partly from motion in a long-period orbit. The chief difficulty with this system arises from its membership in a visual binary (A.D.S. 3483) with a known orbit and a period of about 100 years. During the intervals covered by both sets of observations, the components of the visual binary could not be resolved on the spectroscope slit. The maximum separation is about 1" and there appears to be no fully reliable estimate of the magnitude difference, which is probably around 1.6m. For similar reasons there is uncertainty about the spectral types: those given in the Catalogue result from the modelling technique applied by Griffin et al. also to several other Hyades binaries. They also estimate G4 V for the visual secondary and raise the possibility that it, too, is double. Turner et al. point out the similarity in shape between the visual orbit and the spectroscopic orbit and suggest that they may also be coplanar (inclination about 50 deg). There is some evidence for apsidal motion in the spectroscopic orbit. Besides the orbital companion, there is also one of 12.7m at 44.9" listed in I.D.S. System284Orbit1End System285Orbit1Begin Epoch is T0. System285Orbit1End System286Orbit1Begin The orbit was assumed circular and the epoch is T0. The magnitude difference between the components is estimated from the `dips' in the radial-velocity traces to be Delta B=2.6m. Although the system was investigated because of its possible connection with the Hyades, its systemic velocity makes clear that it does not belong to the cluster. System286Orbit1End System287Orbit1Begin No new study has been made of the radial-velocity curve since the one published by Struve. Undoubtedly the velocity-curve is distorted in the way typical for Algol systems and masses or dimensions computed from it are unreliable. There has been a good UBV light-curve published (D.S. Hall, R.O. Cannon and C.G. Rhombs, Astron. J., 89, 559, 1984) on which the magnitude values given in the Catalogue are based. T.W. Stuhlinger, J.S. Shaw and D.S. Hall (Astron. J., 89, 562, 1984) attempted to solve this, allowing for the effects of a disk surrounding the hotter star. They found an inclination of about 88 deg and a fractional luminosity (in V) for the brighter star of 0.7. The other important discussion of this star is by M.J. Plavec and J.J. Dobias (Astron. J., 92, 171, 1987), who fit model atmospheres to IUE and optical scans of the system to derive the spectral types given in the Catalogue. The photometric and spectroscopic observers agree on the spectral type of the secondary, but the former derive A5 III for the primary. This is not consistent with the observed spectrum. Plavec and Dobias comment on the emission lines, appreciably stronger than in many Algol systems. They estimate masses of 2.4 MSol and 0.4 MSol for the two components. System287Orbit1End System288Orbit1Begin A later investigation by G.R. Miczaika (Z. Astrophys., 27, 247, 1950) confirms these elements; the differences between the two sets are not greater than the uncertainties. Miczaika found an appreciable eccentricity (0.073) with omega=161.8 deg. He also found P=3.700373d, which is probably to be preferred to Lee's value. Epoch given by Lee is T0. Star is an ellipsoidal variable with a range of about 0.05m. System288Orbit1End System289Orbit1Begin The revision of W.E. Harper's orbit (J. Roy. Astron. Soc. Can., 5, 115, 1911) by Lucy & Sweeney was adopted because they have modified the period by including some earlier observations. The epoch is T0. Harper could detect no trace of the secondary spectrum. The star is the brightest component of A.D.S. 3536: companions 7.8m at less than 1" (sometimes not resolved) and 11.3m at 25.8". System289Orbit1End System290Orbit1Begin A Ba II star of the type that McClure has shown are probably all binaries. System290Orbit1End System291Orbit1Begin The recent eclipse (1982-5) of this long-period system has led to a spate of publications, but there is still no orbital study to improve on Wright's, which is itself a revision of one by S.C. Morris (J. Roy. Astron. Soc. Can., 56, 210, 1962). These superseded earlier studies by E.B. Frost, O. Struve and C.T. Elvey (Publ. Yerkes Obs., 7, 81, 1932) and G.P. Kuiper, O. Struve and B. Stromgren (Astrophys. J., 86, 570, 1937). It is impossible to do justice to recent work, stimulated by the eclipse, in a short note. Surveys of both photometric and spectroscopic work are given in Highlights in Astronomy, 7, 1986 (R.E. Stencel, p. 143, D.L. Lambert, p. 151). See also the report of Commission 42 in Volume XXA of Trans. Inter. Astron. Union, p. 588, 1988. It is probably true to say that no consensus yet exists on a model for the system. The tendency is away from treating the 0.8m dip in the light-curve as a simple stellar eclipse. There are suggestions that the component stars are of much lower mass than previously thought (M. Saito et al., Publ. Astron. Soc. Japan, 39, 135, 1987; D.L. Lambert and S.R. Sawyer, Publ. Astron. Soc. Pacific, 98, 389, 1986). The value of K2 given by Wright is not directly observed and should not be used to calculate masses. It has also been suggested that the secondary component is triple (P.P. Eggleton and J.E. Pringle, Astrophys. J., 288, 275, 1985). K.Aa. Strand (Astron. J., 64, 346, 1959) finds i=72 deg from astrometric data. The star is the brightest component of A.D.S. 3065; of four faint companions, the closest is at 21". System291Orbit1End System292Orbit1Begin Although this system continues to attract observers, especially during eclipses, the best orbit, as with the previous entry, remains that derived by Wright, the elements of which are very similar to those derived by W.E. Harper (see E.K. Lee and K.O. Wright, Publ. Dom. Astrophys. Obs., 11, 339, 1960). Wright improved the value of K2, bringing the masses into closer agreement with those estimated by D.M. Popper (Astrophys. J., 134, 835, 1961) and indicating that the earlier value derived by W.H. Christie and O.C. Wilson (Astrophys. J., 81, 426, 1935) is too high. Lee and Wright estimated Delta m=1.9, by spectrophotometric measures; Popper derived Delta m=2.2 from the light-curve. The orbital inclination is probably close to 90 deg. The major development since the publication of the Seventh Catalogue is the availability of UV observations from space. A summary of results for zeta Aur systems in general is given by R.D. Chapman (Highlights in Astronomy, 7, 169, 1986). See also K.- P. Schroder (Astron. Astrophys., 170, 70, 1986). These papers give references to most of the other recent spectrophotometric studies. System292Orbit1End System293Orbit1Begin The system is of interest because the H and K lines are seen in emission. The emission is not associated with the secondary component. Its strength varies with time but not in correlation with the orbital phase. System293Orbit1End System294Orbit1Begin Preliminary spectroscopic elements and photoelectric observations were published by C. Bartolini et al., Asiago Contr., No. 168, 1965. Photoelectric observations have also been published by H. Schneller (Astron. Nachr., 286, 97, 1961), but it is those published by G. Mannino et al. (Mem. Soc. Astron. Ital., 35, 371, 1964) that have been subjected to most analysis. Mammano et al. believed these observations showed the system to be in contact. Working from the same data, however, D.P. Schneider, J.J. Darland and K.-C. Leung (Astron. J., 84, 236, 1979) found the system to be semi-detached, possibly with the more massive component filling the Roche lobe. They find the orbital inclination to be about 85 deg and the brighter component gives 0.59 of the light in all colours. (The primary eclipse is about 0.74m deep.) System294Orbit1End System295Orbit1Begin Epoch is T0. Star is brightest component of A.D.S. 3675. There are four faint companions of which the closest is 12.2m at about 5". System295Orbit1End System296Orbit1Begin The elements by Young supersede those obtained in the earlier study by E.B. Frost and O. Struve (Astrophys. J., 60, 313, 1924). Young emphasizes the apparent difference in chemical constitution of the two components: the secondary (more massive) star is a `mercury star', the primary is not. Although there have been some reports of light variation, Young has looked for an eclipse and failed to observe any variation at all. He concludes i<80 deg. Petrie(II) found Delta m=0.19. Epoch is T0. System296Orbit1End System297Orbit1Begin Brightest component of A.D.S. 3709: companions 12.0m at 13.3" and 8.6m at 35.3". System297Orbit1End System298Orbit1Begin This system has attracted considerable attention in recent years. The new spectroscopic discussion by Wachmann et al. supersedes the older one by A.H. Joy and B.W. Sitterly (Astrophys. J., 73, 77, 1931) and is confirmed by recently published new work (S.A. Bell, A.J. Adamson and R.W. Hilditch, Mon. Not. Roy. Astron. Soc., 224, 649, 1987). The orbit is assumed to be circular, in accordance with the photometric evidence. The epoch is the time of primary minimum. Wachmann et al. stress that their values of K1 and K2 are lower limits, because of the dependence of their measures on the diffuse helium lines. This is the chief reason for the d quality. From the photometric measurements, the individual spectral types are estimated as B1 and B2.5. Although other photometric studies have been published, the two cited here (i.e. Wachmann et al. and Bell et al.) are probably the best. They agree fairly well. The orbital inclination is about 86 deg, the luminosity ratio (L2/L1) is 0.6 to 0.7 in V. The cooler, less massive component approximately fills its Roche lobe and is the larger. System298Orbit1End System299Orbit1Begin Despite earlier observations of a varying magnetic field associated with this star Conti was unable to find evidence of any field at all. The star is classified as A2 from the K line and F2 from the metallic lines. Two companions are listed in I.D.S., both faint and distant: they are 12.2m and 9.9m at 88.6" and 168" respectively. System299Orbit1End System300Orbit1Begin Bell et al. obtained a small number of new observations that they combined with those previously obtained and analyzed by D.M. Popper (Astrophys. J., 97, 394, 1943). The results do not indicate any great change to the orbital elements that Popper derived. The spectral type is uncertain: Bell et al. suggest that it should be one or two subclasses earlier. The orbit is assumed circular and the epoch is the time of primary minimum. From new photometric observations in the B band, they deduce an orbital inclination of about 83 deg and a luminosity ratio of 0.35. The fainter, less massive probably fills its Roche lobe. There are conflicting statements in the literature about whether or not the period varies (C.R. Chambliss, Inf. Bull. Var. Stars, No. 1278, 1977; J.M. Kreiner and J. Tremko, Acta Astron., 28, 179, 1978). System300Orbit1End System301Orbit1Begin Epoch is T0. Struve remarked that the period used is too short: there is photometric evidence for period variations (K.K. Kwee, Bull. Astron. Inst. Netherl., 14, 131, 1958; L. Binnendijk, Astron. J., 67, 86, 1962). Several photometric solutions have been made, but the agreement between them is not good. Good modern BV light-curves have been published by P.P. Rovithis and H. Rovithis-Livaniou (Astron. Astrophys., 155, 46, 1986) but the solutions from the two minima are not entirely consistent. The range of magnitudes given is taken from this paper, but there may be a zero-point error, since the maximum magnitude is that given by M. Huruhata, T. Nakamura and M. Kitamura (Ann. Tokyo Obs., Series 2, 5, 3, 1957). G. Russo et al. analyzed Binnendijk's light-curves to obtain an orbital inclination of 81 deg and a fractional luminosity (in V) for the brighter component of 0.63. Several photometric investigators emphasize the need for new spectroscopic observations. System301Orbit1End System302Orbit1Begin System302Orbit1End System303Orbit1Begin The orbit was assumed circular and the epoch is time of passage through the ascending node (which coincides with T0 when the orbit is exactly circular). This is one of very few systems, however, for which Lucy & Sweeney recommended adopting a significant eccentricity (0.14) that was not postulated by the original investigators. The light-curve requires a circular orbit (Y. Kondo, Astron. J., 71, 46, 1966) but since the system is of the Algol type, a spurious spectroscopic eccentricity may well be observable. IUE observations of the system (F.C. Bruhweiler, W.A. Feibelman and Y. Kondo, Astron. J., 92, 441, 1986) reveal evidence of a shell surrounding the binary. New BV light-curves have been published by O. Gulman, C. Sezer and N. Gudur (Astron. Astrophys. Supp., 60, 389, 1985). They find an inclination close to 79 deg and a fractional luminosity (in V) for the brighter star of 0.99. Although the differential magnitudes are on the V scale the zero point for the apparent magnitude of the system is uncertain. The system differs from other Algol-type systems in that the secondary is the smaller star. Reference: A.Mammano \etal , Asiago Contr.,, No. 192, 1967 System303Orbit1End System304Orbit1Begin Brightest component of A.D.S. 3797: companions 8.4m at 7", and 11.8m at 182". System304Orbit1End System305Orbit1Begin The elements by Lucy & Sweeney are preferred over the originals by W.E. Harper (Publ. Dom. Obs., 3, 221, 1916) because he fixed T to obtain a solution and because Lucy & Sweeney used some later observations of Harper's. The epoch is T0. The star is the brightest component of A.D.S. 3824: of its three companions, the brightest is 7.4m at 14.6". System305Orbit1End System306Orbit1Begin First, we introduce a matter of terminology. It is usual to refer to the component of Capella whose spectrum is most readily seen as the `primary'. R. Griffin and R. Griffin (J. Astrophys. Astron., 7, 45, 1986) have raised strong arguments for supposing that the primary star (in the sense of the brighter one at optical wavelengths) is the other component, whose spectral lines are broadened by rotation. As a result, individual lines are not easily seen and measured, but the radial-velocity trace of this component can be measured with photoelectric spectrometers. We shall follow the example of Griffin and Griffin (who were themselves following the example of H.F. Newall, Mon. Not. Roy. Astron. Soc., 60, 418, 1900) in calling this component the `Procyon' component and the other star (with the sharp-lined, easily measurable spectrum) the `solar' component, even though these terms are not entirely in accord with our modern knowledge. The conclusion reached by the Griffins has recently been supported by W. Bagnuolo and J.R. Sowell (Astron. J., 96, 1056, 1988). The new orbit by Shen Liangzhao et al. certainly supersedes all previous discussion (including A.H. Batten and V. Erczeg, Mon. Not. Roy. Astron. Soc., 171, 47P, 1975; O. Struve and F. Kilby, Astrophys. J., 117, 272, 1953; W. Struve, Z. Astrophys., 17, 61, 1939 -- for even earlier studies see Table I in Shen Liangzhao et al.). The epoch is T0. The velocity-curve of the solar component is now very well known and fully deserves the a quality. There is, however, still room for doubt about the amplitude of the velocity variation of the Procyon component. The value to be deduced for the mass-ratio from the Catalogue elements is 1.18+/-0.02 -- the solar component being the more massive. K.O. Wright (Astrophys. J., 119, 471, 1954 and Publ. Dom. Astrophys. Obs., 10, 1, 1954) derived 1.05 and this value has found some support from F.C. Fekel, T.J. Moffet and G.W. Henry (Astrophys. J. Supp., 60, 551, 1986) who derive 1.07+/-0.02. Thus, more than sixty years after Eddington first used this system as an anchor for the mass-luminosity relation we may still have to make revisions to the masses. Ever since J.A. Anderson (Astrophys. J., 51, 263, 1920) first published interferometric observations of the system, it has been possible also to study the orbit in the plane of the sky. Two modern studies are by H.A. McAlister (Astron. J., 86, 795, 1981 -- see also H.A. McAlister and W.G. Bagnuolo, Publ. Astron. Soc. Pacific, 95, 992, 1983) and by W.S. Finsen (Comm. 26, I.A.U. Circ. d'Inf., No. 66, 1975). The former solution gives P=104.0237d, a=0.0547", i=136.64 deg and is based on an assumed circular orbit. Finsen's solution is closely similar. How close the resulting parallax is to the trigonometrically determined one depends, of course, on the value assumed for the mass-ratio. The components of Capella are chromospherically active (T.R. Ayres and J.L. Linsky, Astrophys. J., 241, 279, 1980) and the system is sometimes referred to as an RS CVn binary, although this seems to be stretching the original definition of the class. It is now known to be a radio source (S.A. Drake and J.L. Linsky, Astron. J., 91, 602, 1986) and an X-ray source (G.S. Varana et al., Astrophys. J., 245, 163, 1981). According to the Bright Star Catalogue, Capella is also an infrared source, although R.P. Verma et al. suggest that its flux is deficient in the J, H and K bands (Proc. 3rd Cambridge Workshop on Cool Stars Stellar Systems and the Sun, 1984, eds. S.L. Baliunas and L.W. Hartmann pp.270-2). The star is known to be slightly variable. The abundance of lithium is very different in the two components (G. Wallerstein, Astrophys. J., 143, 823, 1966). Capella is the brightest member of A.D.S. 3841: all the other components are faint and distant from the primary, but one -- itself double -- appears to be physically associated with the bright star (W.D. Heintz, Astrophys. J., 195, 411, 1975). System306Orbit1End System307Orbit1Begin Fainter component (BC) of beta Ori (A.D.S. 3823, at least a quadruple system). Separation from beta Ori A is 9.5" and the pair seems to be a common-proper-motion pair. This fainter component has been suspected of visual duplicity (separation always less than 0.2"), but since its two subcomponents are apparently equal in magnitude, it is difficult to reconcile these observations with the failure to observe any spectrum of C. Star C cannot be identified with the star producing the secondary spectrum of the spectroscopic pair. The bright component, beta Ori A, has been suspected of being a binary and an orbit was derived by J.S. Plaskett (Astrophys. J., 30, 26, 1909). In view of the small amplitude (3.8 km/s), however, and the known tendency of supergiants to display random atmospheric motions, it seems unlikely that this star is a real binary (see R.F. Sanford, Astrophys. J., 105, 222, 1947). System307Orbit1End System308Orbit1Begin Pearce predicted eclipses from his spectroscopic elements and they were found by S. Gaposchkin (Publ. Astron. Soc. Pacific, 55, 192, 1943). Ironically, the high minimum masses that led Pearce to this conclusion are now questioned. D.M. Popper (Astrophys. J., 220, L11, 1978) argues that the double lines are not properly resolved and that the star with the weaker spectrum may be as early as O9. Two studies of the light-curve have been published since the Seventh Catalogue. One (M. Ramella et al., Astrophys. Space Sci., 70, 461, 1980) is a new analysis of the light-curve obtained by H. Schneller (Astron. Nachr., 287, 49, 1962). The other is an analysis of a new V light-curve by P. Hartigan (J. Amer. Assoc. Var. Star Obs., 10, 13, 1981). They agree fairly well on the luminosities of the stars (primary fractional luminosity 0.88 in V) but differ on the orbital inclination (73 deg and 83 deg respectively) and the radius of the secondary star. The photometric results are not consistent with Petrie's(II) derivation of Delta m=0.45. System308Orbit1End System309Orbit1Begin Brighter component of A.D.S. 3872: companion 10.6m at 4.2". System309Orbit1End System310Orbit1Begin Popper's elements are in quite good agreement with earlier ones derived by R.F. Sanford (Astrophys. J., 68, 42, 1928), which is why the system is given a b rating. A circular orbit was assumed and the epoch is the time of primary minimum. Several light-curves and photometric analyses have been published in recent years. That by G. Russo et al. (Astrophys. Space Sci., 79, 359, 1981) gives references to most of the others. The orbital inclination is fairly well determined at close to 87 deg. Estimates of the fractional luminosity of the primary star are less accordant, but that star gives about half the total light in V. The system is the brightest component of A.D.S. 3866: companion is 9.9m at 10.2"). System310Orbit1End System311Orbit1Begin A circular orbit was assumed and the epoch is T0. Wyse measured only the lines at lambda lambda 4482 and 4549. A misprint in his paper for the values of m sin^3 i is corrected on p.313 of the same volume of Publ. Astron. Soc. Pacific. W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 311, 1937) found very similar elements. The confirmation of each investigation by the other (within their uncertainties) merits the b classification. Petrie(I) found Delta m=0.14. Analysis of a uvby photoelectric light-curve by K.T. Johansen (Astron. Astrophys., 4, 1, 1970) gives an orbital inclination close to 88 deg and a fractional luminosity for the primary star (in all colours) of 0.54. These results were not much changed by a new analysis of the same observations (B. Cester et al., Astron. Astrophys. Supp., 33, 91, 1978). The hotter star is now recognized as an HgMn star (S.C. Wolff and G.W. Preston, Astrophys. J. Supp., 37, 371, 1978) although the cooler component apparently is not (Y. Takeda, M. Takada and M. Kitamura, Publ. Astron. Soc. Japan, 31, 821, 1979). The system belongs to the Aur OB1 association. Its common proper motion with H.D. 34452 appears first to have been pointed out by W.P. Bidelman and is discussed by W.L.W. Sargent and O.J. Eggen (Publ. Astron. Soc. Pacific, 77, 461, 1965). Observed period changes may indicate a third body in AR Aur itself (S.J. A delman and D.M. Pyper, Astron. Astrophys., 118, 313, 1983). System311Orbit1End System312Orbit1Begin Epoch is an arbitrary zero, T0 is about 3.6d later. Only the descending branch of the velocity-curve is covered. System312Orbit1End System313Orbit1Begin This investigation supersedes Stilwell's own earlier work (J. Roy. Astron. Soc. Can., 30, 212, 1936). The scatter of the observations is large, and K, in particular, is poorly determined. System313Orbit1End System314Orbit1Begin Epoch is T0. An earlier investigation by J.B. Cannon (Publ. Dom. Obs., 4, 185, 1918) was based on an incorrect value of the period. Petrie(II) found Delta m=0.36. System314Orbit1End System315Orbit1Begin Photometric and spectroscopic observations of this late-type dwarf eclipsing binary are discussed by Popper et al. The eccentricity, although small, is real -- as is shown by the light-curve. The epoch, nevertheless, is the time of primary minimum. Only the spectral type of the primary is given, but the photometric solution shows the secondary to be only a little redder. From the light-curve, Delta V is found to be 0.32m and the orbital inclination is very close to 90 deg. The importance of the system is that it contains unevolved late-type stars that show no signs of chromospheric activity. System315Orbit1End System316Orbit1Begin These orbital elements are described as `marginal' by Abt and Levy themselves. System316Orbit1End System317Orbit1Begin There are hardly any observations on the ascending branch of the velocity-curve and the elements are described as `very preliminary' by Morrell and Levato themselves. The system is a member of the Orion OB1 association. System317Orbit1End System318Orbit1Begin Hilditch has also discussed the photometric properties of this system (Observatory, 89, 143, 1969 and Mem. Roy. Astron. Soc., 76, 1, 1972). His observations have been rediscussed by G. Giuricin et al. (Astron. Astrophys. Supp., 39, 255, 1980) and by H.M.K. Al-Naimiy (Astrophys. Space Sci., 59, 3, 1978). New photometric observations have been published by T.D. Padalia and R.K. Srivastava (Astrophys. Space Sci., 38, 87, 1975) and by Kh.F. Khaliullin and V.S. Kozyreva (Astrophys. Space Sci., 94, 115, 1983). These last present evidence for apsidal motion with a period of 2,250 years, compared with a theoretically expected 825 years. There is not complete agreement amongst all photometric investigators about the light-curve, but the magnitude difference in V seems to be about 1 m, the spectral types are similar and the orbital inclination close to 88 deg. System318Orbit1End System319Orbit1Begin The computation of the short-period orbit by Lucy & Sweeney is based on observations by W.S. Adams (Astrophys. J., 17, 68, 1903) and is preferred to Adams' purely graphical derivation of the elements. A circular orbit was assumed and the epoch is T0. Later observations by A. Hnatek (Astron. Nachr., 217, 53, 1922) and R.F. Sanford (Astrophys. J., 64, 172, 1926) confirm Adams' results. Allegheny observations showed the secondary spectrum (F. Schlesinger and R.H. Baker, Publ. Allegheny Obs., 1, 135, 1910) measures of which give K2=153 km/s, m1 sin^3 i=11.2 MSol, m2 sin^3 i=10.6 MSol. Petrie(II) found Delta m=0.47. Observations by G.R. Miczaika (Z. Astrophys., 29, 105, 1951) gave K1=103.7 km/s. The Allegheny work first indicated that V0 is variable and the system is triple. A.F. Beal (Publ. Am. Astron. Soc., 3, 117, 1915) estimated the long period to be between nine and ten years. Sanford confirmed this and Pogo found P=9.2y, T=1900.0 and the other elements given in the Catalogue. Ultraviolet spectrograms have been obtained from above the atmosphere by T.H. Morgan et al. (Astrophys. J., 197, 371, 1975) and T.J. Herczeg, Y. Kondo and K.A. van der Hucht (Astrophys. Space Sci., 46, 379, 1977). Detection of the third spectrum (also type B) has been claimed by R. Zizka and W.R. Beardsley (Bull. Am. Astron. Soc., 8, 362, 1976), also on Allegheny spectrograms. The same component, presumably, has been resolved by speckle interferometry (H.A. McAlister and E.M. Hendry, Astrophys. J. Supp., 49, 267, 1982). The star is listed as an eclipsing binary, but no analysis of the light-curve has been published. The primary component may be intrinsically variable (R.H. Koch, B.J. Hrivnak and D.H. Bradstreet; W.R. Beardsley and E.R. Zizka, Bull. Am. Astron. Soc., 12, 452, 1980). The triple system is the brightest member of A.D.S. 4002: two other companions are 4.8m at 1.5" and 9.4m at 115.1". System319Orbit1End System320Orbit1Begin The computation of the short-period orbit by Lucy & Sweeney is based on observations by W.S. Adams (Astrophys. J., 17, 68, 1903) and is preferred to Adams' purely graphical derivation of the elements. A circular orbit was assumed and the epoch is T0. Later observations by A. Hnatek (Astron. Nachr., 217, 53, 1922) and R.F. Sanford (Astrophys. J., 64, 172, 1926) confirm Adams' results. Allegheny observations showed the secondary spectrum (F. Schlesinger and R.H. Baker, Publ. Allegheny Obs., 1, 135, 1910) measures of which give K2=153 km/s, m1sin^3i=11.2 MSol, m2sin^3i=10.6 MSol. Petrie(II) found Delta m=0.47. Observations by G.R. Miczaika (Z. Astrophys., 29, 105, 1951) gave K1=103.7 km/s. The Allegheny work first indicated that V0 is variable and the system is triple. A.F. Beal (Publ. Am. Astron. Soc., 3, 117, 1915) estimated the long period to be between nine and ten years. Sanford confirmed this and Pogo found P=9.2y, T=1900.0 and the other elements given in the Catalogue. Ultraviolet spectrograms have been obtained from above the atmosphere by T.H. Morgan et al. (Astrophys. J., 197, 371, 1975) and T.J. Herczeg, Y. Kondo and K.A. van der Hucht (Astrophys. Space Sci., 46, 379, 1977). Detection of the third spectrum (also type B) has been claimed by R. Zizka and W.R. Beardsley (Bull. Am. Astron. Soc., 8, 362, 1976), also on Allegheny spectrograms. The same component, presumably, has been resolved by speckle interferometry (H.A. McAlister and E.M. Hendry, Astrophys. J. Supp., 49, 267, 1982). The star is listed as an eclipsing binary, but no analysis of the light-curve has been published. The primary component may be intrinsically variable (R.H. Koch, B.J. Hrivnak and D.H. Bradstreet; W.R. Beardsley and E.R. Zizka, Bull. Am. Astron. Soc., 12, 452, 1980). The triple system is the brightest member of A.D.S. 4002: two other companions are 4.8m at 1.5" and 9.4m at 115.1". System320Orbit1End System321Orbit1Begin The binary nature of this system was rediscovered by A. Blaauw and T.S. van Albada (Astrophys. J., 137, 791, 1963) who were apparently unaware of Duflot's work. Although they find a smaller eccentricity, their values of P, K1 and V0 are closely similar to Duflot's. The scatter of their observations is less than that of hers. Her elements have been preferred, since they result from the fuller investigation. System321Orbit1End System322Orbit1Begin The spectral lines are very broad and difficult to measure, as the large residuals from the velocity- curve show. Mammano et al. discussed the possibility of a variation in V0, but the radial-velocity measurements are too uncertain to be used to deduce the existence of a third body. On the other hand, photometric observations show both eclipses to be getting deeper and this seems best explained as a change in orbital inclination. The most plausible way to explain that, is to suppose that the system is triple and that the orbital plane of the eclipsing pair is precessing (J.A. Eaton, Acta Astron., 28, 63, 1978; G. Giuricin et al., Astron. Astrophys. Supp., 37, 513, 1979). According to the latter paper, the primary gives about 0.65 of the total light in V (the amount of third light is uncertain) and the orbital inclination in 1967-70 was close to 84 deg. Discovery of the eclipses was made by P. Mayer (Publ. Astron. Soc. Pacific, 77, 436, 1965) whose values of the V magnitudes are used in the Catalogue -- the star must now be fainter at minimum. The spectra were classified as O9.5 V by G. Hill et al. (Mem. Roy. Astron. Soc., 79, 101, 1975). System322Orbit1End System323Orbit1Begin Since the Sixth Catalogue, two spectroscopic investigations have been published: the one whose results are given here and that by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 36, 241, 1978). They supersede the earlier investigations (J.A. Pearce, Publ. Astron. Soc. Pacific, 65, 209, 1953; J.S. Plaskett, Astrophys. J., 28, 266, 1908 and M. Chopinet, J. Observateurs, 36, 34, 1953). Neither of the last two investigators detected the secondary spectrum. Pearce found a higher value of K2 than Lu Wenxian has found; the value obtained by Abt and Levy falls in between. Thus, some uncertainty still remains about the mass-ratio, but the elements of the primary component are now well determined. The orbital eccentricity, although small, is statistically significant. All available values of omega could be satisfied by a period of about 40 years for apsidal rotation, which appears to be close to the theoretically expected value. However, some of the earlier determinations of e and omega should be looked on with caution and it is premature to be certain about the apsidal period, which D.G. Monet (Astrophys. J., 237, 513, 1971) believes to be longer. The light of the star varies slightly because the system is an ellipsoidal variable. J.B. Hutchings and G. Hill (Astrophys. J., 167, 137, 1971) determined i=58 deg from the light-curve, but this value was partly chosen to conform with the expected masses. They also found Delta m=0.95, in good agreement with Lu Wenxian's spectrophotometric value of 1.09 (not strongly dependent on wavelength). The spectral types are those deduced spectrophotometrically by Lu Wenxian. The star is the brighter component of A.D.S. 4039: companions are 10.3m at 2.7" and 12.3m at 83.4". System323Orbit1End System324Orbit1Begin Epoch is T0. Elements have also been computed by Lucy & Sweeney. System324Orbit1End System325Orbit1Begin The elements obtained by Andersen, Batten and Hilditch, being in good agreement with unpublished ones obtained by D.M. Popper are preferred over those of R. Margoni, R. Stagni and A. Mammano (Astrophys. Space Sci., 79, 145, 1981). However, Popper (Astrophys. J., 262, 641, 1982) has given reasons for supposing that even the Victoria and Lick observations may be affected by systematic error. In particular, he believes that the primary spectrum may be affected by blending with the spectrum of the visual companion (A.D.S. 4072 B, 8.9m at 0.6"). In that case, the masses given in the Catalogue are too large and the mass-ratio is closer to unity. The epoch is T0 and was fixed with respect to the observed time of primary minimum. The eclipses were discovered by P. Mayer and the first solution of the light-curve was by P. Mayer and T.B. Horak (Bull. Astron. Inst. Csl, 22, 327, 1971). Several photometric studies have been published since. The most recent, which cites all the earlier studies is by Yang-Feng Li and Kam-Ching Leung (Astrophys. J., 298, 345, 1985). The orbital inclination is about 88 deg and the fractional luminosity of the primary component in V is between 0.5 and 0.6 (third light is about 0.1). There is doubt whether or not the components are in contact. System325Orbit1End System326Orbit1Begin This is Nova Aur 1891. Eclipses were first discovered by M.F. Walker (Astrophys. J., 138, 313, 1963). The period and epoch (time of minimum) given in the Catalogue are taken from the linear ephemeris given by G.S. Mumford (Astrophys. J., 210, 416, 1976). Bianchini is not explicit about the ephemeris used. There is some possibility that the period is decreasing. System326Orbit1End System327Orbit1Begin System327Orbit1End System328Orbit1Begin This is an early-type system in the Large Magellanic Cloud. The `primary' elements are from the absorption lines in the O4f spectrum (the helium emission gives a larger K and a more positive V0 ). The `secondary' elements are from the O6 absorption lines. A circular orbit was assumed and the epoch is the time of superior conjunction of the star of earlier type. Niemela and Morrell estimate a Delta V of about 1 m. They report a faint companion at about 5". System328Orbit1End System329Orbit1Begin Velocity-curve well covered, but Struve himself described the elements as approximate. No photometric elements appear to have been derived. Only one spectrum is visible, even in eclipse. System329Orbit1End System330Orbit1Begin This is one of the few eclipsing cataclysmic systems in which the spectra of both components are visible. The G-band of the absorption-line spectrum can be seen and measured. The study by Schlegel et al. supersedes the preliminary one by K. Horne, H.H. Lanning and R.H. Gomer (Astrophys. J., 252, 681, 1982). The star is also known as Lanning 10. A circular orbit was assumed and the epoch is the time of primary eclipse. The upper line gives the elements obtained from the He II lambda 4686 emission in the white-dwarf spectrum. The value of K depends on the portions of the emission profile measured. The value given is based on measurement of the wings only; if the whole profile were considered, the value would be 200 km/s. Schlegel et al. estimate an orbital inclination of 70 deg. The magnitude given is an approximate B magnitude. The star flickers outside eclipses and the minima are about 0.7m deep in V. System330Orbit1End System331Orbit1Begin Despite a new study of the velocity-curve by M. Singh (Astrophys. Space Sci., 87, 269, 1982) we see no reason to revise our opinion that Curtiss' discussion of the velocity-curve is the best yet available. Neither are we fully convinced by Singh's claim that the orbital elements (especially K) are changing, partly because the error analysis needed to assess this claim is missing from his paper. His work did lead us to consider whether or not our b classification for the orbit in previous catalogues was somewhat optimistic for a star known to be losing mass (D.C. Morton, Astrophys. J., 150, 535, 1967) and whose spectral lines, according to several investigators, are diffuse and hard to measure. Nevertheless, one criterion for giving the b rating is agreement among different determinations. Apart from orbital elements found by G.R. Miczaika (Z. Astrophys., 30, 299, 1951) whose work often differs from that of other observers, and those of Singh himself, other determinations of orbital elements (J. Hartmann, Astrophys. J., 19, 268, 1904; F.C. Jordan, Publ. Allegheny Obs., 3, 125, 1914; W.J. Luyten, O. Struve and W.W. Morgan, Publ. Yerkes Obs., 7, Pt. IV, 256, 1939; P. Pismis, G. Haro and O. Struve, Astrophys. J., 111, 509, 1950; V. Natarajan and K. Rajamohan, Kodaikanal Bull., No. 208, 1971) do give accordant values of K. Differences in V0 are probably at least partly explicable as the results of wavelength selections, but the possibility of a long-period variation cannot be ruled out (see below). The existence of apsidal motion is perhaps not yet completely settled, but Natarajan and Rajamohan favour an apsidal period somewhat in excess of 200 years, which is confirmed by D.G. Monet (Astrophys. J., 237, 513, 1971) and seems to be in accord with the light-curve (R.H. Koch and B.J. Hrivnak, Astrophys. J., 248, 249, 1981). Interpretation of the latter is difficult because eclipses are shallow and possibly complicated by an intrinsic variation. Koch and Hrivnak find an orbital inclination of 68 deg and estimate Delta V to be 1.4m. There now seems general agreement that the primary star is of O-type, but divergent luminosity classes are found in the literature. The spectrum is discussed by P.S. Conti (Astrophys. J., 179, 161, 1973) and P.S. Conti and E.M. Leep (Astrophys. J., 193, 113, 1974). A thorough spectrophotometric discussion has been published by T.S. Galkina (Izv. Krym. Astrofiz. Obs., 54, 128, 1976). Besides Morton's observations, results from above the Earth's atmosphere have been published by T.H. Morgan et al. (Astrophys. J., 197, 371, 1975). The star is the brightest member of A.D.S. 4134: companions are at 14.0m at 32.8" and 6.6m at 52.6". The proper motion of the brighter `companion' differs from that of deg Ori. W.D. Heintz (Astrophys. J. Supp., 44, 111, 1980) has observed a companion (Delta m=0.1) at 0.15" separation. System331Orbit1End System332Orbit1Begin Duerbeck's spectroscopic observations are the most extensive yet made of the system; his photometric ones have been superseded. Earlier spectroscopic observations (Z. Daniel, Publ. Allegheny Obs., 3, 179, 1915; O. Struve and W.J. Luyten, Astrophys. J., 110, 160, 1949; G. Beltrami and P. Galeotti, Mem. Soc. Astron. Ital., 41, 167, 1970) all agree on the existence of a periodic variation in V0 with a period of about 120 days. Beltrami and Galeotti give rather different elements from Duerbeck, whose results have been preferred because they are based on more observations at higher dispersion. Nevertheless, the elements of the long-period orbit must be considered very uncertain. The invisible third body contributes very little to the total light of the system. C.R. Chambliss (Astrophys. Space Sci., 89, 15, 1983) suggests that the third star is probably of spectral type A3 V. The short- period orbit is probably also known only uncertainly. Many of Duerbeck's conclusions were criticized by J. Andersen (Astron. Astrophys., 47, 467, 1976, see also Duerbeck's reply immediately following). It is certainly worrying that his value for K1 is less than any of the values obtained earlier (which range from 132 km/s to 140 km/s). Andersen suggested that Duerbeck's velocities were systematically affected by incomplete resolution of the secondary spectrum. Since the dispersion Duerbeck used is appreciably higher than that used by any other investigator, one would not expect such incomplete resolution to be the source of the problem. Popper has found that lower values of K1 and K2 are often obtained when double-lined late-type spectra are measured at higher dispersions. Duerbeck, however, found a much larger value of K2 than that found by Struve and Luyten (138 km/s) -- although it is still smaller than the value found by Beltrami and Galeotti (320 km/s). Thus different investigators disagree on the semi-amplitudes of the velocity variations of both components and this, rather than any incompleteness of individual investigations, accounts for the d rating. The epochs are T0 for the long-period orbit and primary minimum for the short-period orbit. Although no further spectroscopic investigations have been made since the publication of the Seventh Catalogue (high-dispersion spectrograms measured by cross- correlation might tell us much) the system has almost been over-analyzed photometrically. Light-curves are now available in the UV (J.A. Eaton, Astrophys. J., 197, 379, 1975) and at H-alpha (C.R. Chambliss and B.M. Davan, Astron. J., 93, 950, 1987) with the fullest data at more conventional wavelengths being those first published by C.R. Chambliss and K.-C. Leung, (Astrophys. J. Supp., 49, 531, 1982) and subsequently at least twice reanalyzed. All investigators agree that the brighter component gives at least 0.90 of the total light in V and the orbital inclination is probably around 85 deg. The third body gives at most 0.01 to 0.02 of the total light at any wavelength. Not everyone agrees on whether the system is detached. System332Orbit1End System333Orbit1Begin Duerbeck's spectroscopic observations are the most extensive yet made of the system; his photometric ones have been superseded. Earlier spectroscopic observations (Z. Daniel, Publ. Allegheny Obs., 3, 179, 1915; O. Struve and W.J. Luyten, Astrophys. J., 110, 160, 1949; G. Beltrami and P. Galeotti, Mem. Soc. Astron. Ital., 41, 167, 1970) all agree on the existence of a periodic variation in V0 with a period of about 120 days. Beltrami and Galeotti give rather different elements from Duerbeck, whose results have been preferred because they are based on more observations at higher dispersion. Nevertheless, the elements of the long-period orbit must be considered very uncertain. The invisible third body contributes very little to the total light of the system. C.R. Chambliss (Astrophys. Space Sci., 89, 15, 1983) suggests that the third star is probably of spectral type A3 V. The short- period orbit is probably also known only uncertainly. Many of Duerbeck's conclusions were criticized by J. Andersen (Astron. Astrophys., 47, 467, 1976, see also Duerbeck's reply immediately following). It is certainly worrying that his value for K1 is less than any of the values obtained earlier (which range from 132 km/s to 140 km/s). Andersen suggested that Duerbeck's velocities were systematically affected by incomplete resolution of the secondary spectrum. Since the dispersion Duerbeck used is appreciably higher than that used by any other investigator, one would not expect such incomplete resolution to be the source of the problem. Popper has found that lower values of K1 and K2 are often obtained when double-lined late-type spectra are measured at higher dispersions. Duerbeck, however, found a much larger value of K2 than that found by Struve and Luyten (138 km/s) -- although it is still smaller than the value found by Beltrami and Galeotti (320 km/s). Thus different investigators disagree on the semi-amplitudes of the velocity variations of both components and this, rather than any incompleteness of individual investigations, accounts for the d rating. The epochs are T0 for the long-period orbit and primary minimum for the short-period orbit. Although no further spectroscopic investigations have been made since the publication of the Seventh Catalogue (high-dispersion spectrograms measured by cross- correlation might tell us much) the system has almost been over-analyzed photometrically. Light-curves are now available in the UV (J.A. Eaton, Astrophys. J., 197, 379, 1975) and at H-alpha (C.R. Chambliss and B.M. Davan, Astron. J., 93, 950, 1987) with the fullest data at more conventional wavelengths being those first published by C.R. Chambliss and K.-C. Leung, (Astrophys. J. Supp., 49, 531, 1982) and subsequently at least twice reanalyzed. All investigators agree that the brighter component gives at least 0.90 of the total light in V and the orbital inclination is probably around 85 deg. The third body gives at most 0.01 to 0.02 of the total light at any wavelength. Not everyone agrees on whether the system is detached. System333Orbit1End System334Orbit1Begin P=8.4y, T=1908.3. System334Orbit1End System335Orbit1Begin System335Orbit1End System336Orbit1Begin Variability of the velocity of this star was discovered by D.P. Hube (Mem. Roy. Astron. Soc., 72, 233, 1970). The orbital elements are derived from observations made at several different observatories, but systematic differences do not seem to have caused a major problem. Dworetsky suggests that careful observation from space could lead to the determination of an astrometric orbit. The star is the brighter member of A.D.S. 4181: companion is 9.8m at 2.9". System336Orbit1End System337Orbit1Begin Lucy & Sweeney confirm Neubauer's orbital elements. System337Orbit1End System338Orbit1Begin Possibility of a period less than one day not eliminated by these observations. System338Orbit1End System339Orbit1Begin Epoch is an arbitrary zero: T0 is about 8.4d later. System339Orbit1End System340Orbit1Begin Lohsen himself describes this orbit for a member of the Trapezium as `tentative'. It depends heavily on old observations from two different sources. The period proposed is a submultiple of the photometric period first derived by Lohsen (Inf. Bull. Var. Stars, No. 1129, 1976). Subsequent photometry by M.M. Zakirov (Peremm. Zvezdy, 21, 223, 1979) tends to confirm the period as 65.4325d. Zakirov deduces an orbital inclination of 88.9deg and a fractional luminosity (in V) for the primary component of 0.58. Eclipses are about a magnitude deep. System340Orbit1End System341Orbit1Begin There are two other published spectroscopic studies of this system, one by O. Struve and J. Titus (Astrophys. J., 99, 84, 1944) and the other by C. Doremus (Publ. Astron. Soc. Pacific, 82, 745, 1970). The failure of Doremus to detect the secondary spectrum even during an apparently total eclipse led to the proposal of a number of competing and unusual models for the system. V.S. Shevchenko and M.M. Zakirov (Peremm. Zvezdy, 20, 361, 1977) were also unable to detect the secondary spectrum. Popper and Plavec have detected a weak secondary spectrum with a spectral type in the range A5 IV-V to F2 III-IV. This result favours the model proposed by D.S. Hall (Kl. Veroff. Remeis-Sternw. Bamberg, 9, 217, 1971) of a flattened disk-like secondary star. Popper and Plavec, however, do not find the star so flattened as Hall did. It is overluminous and presumably in a state of pre-main-sequence contraction. From the photometric data of D.S. Hall and L.M. Garrison (Publ. Astron. Soc. Pacific, 81, 771, 1969), Popper and Plavec deduce i=83 deg and M_V=1.0. The period quoted is from the work of Hall and Garrison, and the epoch is their time of primary minimum. The star is a member of A.D.S. 4186 (the Trapezium system). System341Orbit1End System342Orbit1Begin Attention was drawn to this star by the possibility that it might be associated with the weak X-ray source 3U 0527 05. Aikman and Goldberg found no evidence for identifying these two objects, but they did find that the orbital period of 21.03d used by O. Struve (Astrophys. J., 60, 159, 1924) and G. Munch (Astrophys. J., 98, 228, 1943) was wrong. They found some evidence for a weak secondary spectrum (Delta m=1.5) and estimated a mass-ratio of 0.57. They believe the orbital inclination to be close to 90 deg. The star is the brightest member of A.D.S. 4188: the principal companion is 6.5m at 52.5". System342Orbit1End System343Orbit1Begin In addition to the elements given here, based on coude spectrograms and first published in ESA-SP 263, 1986 (not available to the compilers when this note was written), Stickland has also published elements (except V0) derived from measurements of IUE spectrograms. The two sets are closely similar. Apparently, Pearce's detection of the secondary spectrum (Astron. J., 58, 223, 1953) is not confirmed although the observations do show some systematic trends reminiscent of the `secondary wave' that bothered J.S. Plaskett and W.E. Harper, (Astrophys. J., 27, 272,, and 28, 275, 1908 and 30, 373, 1909). Stickland's values for K1 are lower than those of Plaskett and Harper or Pearce, but still higher than the 99 km/s found by G.R. Miczaika (Z. Astrophys., 29, 305, 1951). There is evidence for apsidal motion. This is a system about which we feel less certain now that we know more omega. The star is the brightest component of A.D.S. 4193: one companion is 7.0m at 11.3" and another companion is at 49.5" System343Orbit1End System344Orbit1Begin This star is well known as a shell star which apparently erupts (see A.B. Underhill, Astron. J., 70, 148, 1965). The present elements were derived by Underhill from observations published by O. Struve and J.A. Hynek (Astrophys. J., 96, 425, 1942). The elements must be considered uncertain because of the superposed effects of the shell on the spectrum. A study of circumstellar lines in the UV spectrum of this star has been published by D.N. Dawanas and R. Hirata (Astrophys. Space Sci., 99, 139, 1984). System344Orbit1End System345Orbit1Begin Lunt commented that further observations are needed in order to determine the period more accurately. System345Orbit1End System346Orbit1Begin The binary nature of this star (also known as LB 3459) was discovered photometrically by D. Kilkenny, R.W. Hilditch and J.E. Penfold (Mon. Not. Roy. Astron. Soc., 183, 523, 1978). The maximum and minimum V magnitudes are taken from that paper, although there appear to be small variations in the depth of eclipse. The epoch is the time of minimum as given in the same paper. Later, the same authors published an improved analysis of the light-curve (Mon. Not. Roy. Astron. Soc., 187, 1, 1979) and hypothesized that the system is composed of an O-type subdwarf and a white dwarf. A preliminary discussion of the velocity-curve (D. Kilkenny, A.E. Lynas-Gray and R.W. Hilditch, I.A.U. Colloq. No. 53, p. 255, 1979) was superseded by the discussion cited in this Catalogue. In this latest paper, the idea of a white-dwarf secondary is abandoned and the fainter component is considered as a core remnant of an evolved star that had earlier been in a common envelope with the primary. The orbit was assumed circular after elliptical solutions had shown that the derived eccentricity was not statistically significant. The precise value found for V0 depends on the subset of observations analyzed and the method of solution for the orbital elements. The orbital inclination is certainly close to 90 deg and the brighter component gives around 0.9 of the total light in V. A few new observations and a somewhat different interpretation are offered by P.S. Conti, D. Dearborn and P.S. Massey (Mon. Not. Roy. Astron. Soc., 195, 165, 1981) who also draw attention to a fainter companion some 30" away. System346Orbit1End System347Orbit1Begin This star is the X-ray source A0535+26. The period has been fixed at 111 d since one of about this length is indicated by the X-ray observations (F. Nagase et al., Astrophys. J., 263, 814, 1982) even though it did not show up in the first spectroscopic discussion by J.B. Hutchings et al. (Astrophys. J., 223, 530, 1978). Hutchings gives several sets of elements, derived from different subsets of the observations or with the eccentricity constrained to agree with the X-ray results. The set given in the Catalogue has the value of K that he regards as most likely. The orbital eccentricity was constrained to be in the middle of the range permitted by the X-ray observations. Somewhat different elements have been published by E. Janot-Pacheco, C. Morch and M. Mouchet (Astron. Astrophys., 177, 91, 1987) who also adopted the 111 d period. The scatter of observations around each of the velocity-curves is large and it seems that, at most, we know no more than the approximate period and range of velocity. O.E. Aab (Bulletin Abastumani Obs., No. 58, 282, 1985 and Soviet Astron. J. Lett., 10, 386, 1984) has derived orbital elements K approx 35 km/s, V0 approx -5 km/s for a period of 35 d, which is about one-third of 111 d period. The scatter about this velocity-curve is also very large. System347Orbit1End System348Orbit1Begin The orbital elements given are those derived from the absorption lines of neutral helium. The hydrogen lines give a lower amplitude, probably because of blending with lines of He II. The emission line of He II at lambda 4686 gives a much higher amplitude (nearly 500 km/s). The circular orbit was adopted and T is fixed at 0.25mag after the middle of the X-ray eclipse. The secondary component (the X-ray source) may be a neutron star. A study of the radial velocities was also published by C. Chevalier and S.A. Ilovaisky (Astron. Astrophys., 59, L9, 1977), and the magnitude given is the approximate mean of their measurements -- the star is slightly variable. System348Orbit1End System349Orbit1Begin System349Orbit1End System350Orbit1Begin E.B. Frost, S.B. Barrett, and O. Struve (Publ. Yerkes Obs., 7, Pt. 1, 1929) reported double lines in the spectrum of this star. System350Orbit1End System351Orbit1Begin At the time of writing the discussion by J. Andersen, J.V. Clausen and P. Magain is still unpublished, but it represents such an improvement over the earlier study by M. Imbert (Astron. Astrophys., 32, 429, 1974) that we have included it. The masses are now known to better than one percent. W. Strohmeier (Inf. Bull. Var. Stars, No. 191, 1967) discovered the eclipses and Imbert showed that the system contained two nearly equal stars and that the orbital period was double Strohmeier's value. The minimum magnitude given is an estimate only. The epoch is the time of deeper minimum. The orbit is assumed circular, since the light-curve shows any orbital eccentricity to be negligibly small. The difference between the two values of V0 is well within the observational uncertainty. Andersen et al. re-analyzed the ubvy light-curves published by J.V. Clausen and B. Grnbech (Astron. Astrophys., 48, 49, 1976). They find that the orbital inclination is very close to 90 deg (although the eclipses are not total) and that the two stars differ in V by 0.08m. They also discuss atmospheric abundances. System351Orbit1End System352Orbit1Begin The variable velocity of this star, which is a member of the Aur OB 1 association, was first noted by R.M. Petrie and J.A. Pearce (Publ. Dom. Astrophys. Obs., 12, 1, 1961). The epoch is the time of inferior conjunction. System352Orbit1End System353Orbit1Begin This is an X-ray source in the Large Magellanic Cloud. The epoch is the time of periastron and coincides closely with X-ray maximum. Other orbital elements have been published by R.H.D. Corbet et al. (Mon. Not. Roy. Astron. Soc., 212, 565, 1985). Although they also derive a high eccentricity, their value of omega (330 deg) indicates that the observed velocity is relatively positive at periastron, whereas Hutchings et al. find it to be relatively negative (i.e. compared with velocities observed at other phases). Although the elements found by Hutchings et al. are preferred here, the paper by Corbet et al. gives a much more detailed account of the spectroscopic properties of the system. System353Orbit1End System354Orbit1Begin Other investigations by J.S. Plaskett and W.E. Harper (Astrophys. J., 30, 373, 1909) and M. Barbier-Brossat (J. Observateurs, 37, 119, 1954). Barbier `confirmed' the secondary oscillation found by Plaskett and Harper. (The system is very similar to iota Ori). Pearce detected the secondary spectrum and found no oscillation. He found Delta m=1.14, using Petrie's method, and estimated i=52 deg from the mass-luminosity relation. There is considerable divergence between the three values of K1. System354Orbit1End System355Orbit1Begin This orbit is based on exactly the same observations as that computed by G.A. Radford and R.F. Griffin (Observatory, 95, 289, 1975). It is a rare case of an orbit that was originally assumed to be circular being more correctly represented as slightly eccentric. The new elements were computed by Bassett, after he had applied his statistical tests to show that an elliptical orbit fits the observations better. System355Orbit1End System356Orbit1Begin This is the optical counterpart of an X-ray source in the Large Magellanic Cloud. The epoch is T0. No eclipses are observed in the X-ray flux, from which it is deduced that the orbital inclination is less than about 70 deg. If the B3 V star has a normal mass, that of the companion must exceed 7 MSol. Since its optical spectrum is invisible but it does emit X-rays, they deduce that the companion is degenerate and therefore necessarily a black hole. System356Orbit1End System357Orbit1Begin This is a Wolf-Rayet binary in the Large Magellanic Cloud. The spectral types are given by Moffat and Seggewiss, but it appears doubtful that the B-type supergiant is the secondary component of the spectroscopic binary, since the absorption lines in its spectrum give an almost constant velocity of about 255 km/s. If this star were the secondary, the masses would be unusual. The orbital elements are derived from measures of the emission line of ionized helium at lambda 4686. The systemic velocity derived from this line is variable. It is not known whether the variation is periodic or not. Probably, the true systemic velocity is close to that of the B-type supergiant. The epoch is the time of inferior conjunction of the Wolf-Rayet component. There is no appreciable variation in the apparent magnitude of the system. Although the star has been tentatively identified with an Einstein X-ray source, the identification is now considered less likely. System357Orbit1End System358Orbit1Begin The star for which this orbit is derived is thought to be the optical counterpart of LMC X-1, but is not certainly known to be so. The orbital elements given are derived from measures of the absorption lines; emission lines give somewhat different elements. The epoch is T0. A circular orbit was assumed: an eccentricity of up to 0.21 is formally possible, but it does not appear to improve the representation of the observations. The scatter of the observations is large. System358Orbit1End System359Orbit1Begin The recomputation of elements by Lucy & Sweeney is based on the original observations by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 159, 1924) who fixed T to obtain a solution. They also included some later observations by Harper and that is why their solution is preferred to Luyten's. The epoch is T0. Lucy & Sweeney adopted a circular orbit although the previous investigators found a small eccentricity. There is also an elliptical orbital solution by G. Mannino (Asiago Contr., No. 53, 1954) which is based on new observations. The two sets of elements agree well except for a large difference in V0, which may be partly the result of the wavelengths adopted. New spectroscopic observations by I. Yavuz have been reported (Astron. Gesells. Mitt., 26, 60, 1969) but have not yet been published. Two-colour (BV) photoelectric observations of this system have been obtained by R.M. West (Bull. Astron. Inst. Netherl. Supp., 2, 259, 1968) who finds no displacement of the secondary minimum and an inclination i=77.7 deg. He also finds that the primary star gives 0.95 of the total V light of the system. These results were not much changed in a new analysis of the same observations by M. Mezzetti et al. (Astron. Astrophys. Supp., 42, 15, 1980) who suggest spectral types of A0 IV and F0. System359Orbit1End System360Orbit1Begin Luyten's recomputation is again preferred over the original work by J.B. Cannon (Publ. Dom. Obs., 2, 105, 1915) who had to fix T. Luyten's epoch is T0. The value of K2 depends on only four plates and is rather uncertain. Petrie(I) found Delta m=1.51. System360Orbit1End System361Orbit1Begin The observations by J.A. Pearce (Publ. Dom. Astrophys. Obs., 6, 65, 1932) were used by Hill, together with material from other sources to revise Pearce's elements. Since Petrie(II) found Delta m=2.18, measures of the secondary spectrum must be rather uncertain. It probably is of somewhat later spectral type than the primary: Pearce gave B3k + B5. The introduction of observations from various sources has increased the scatter compared with that of Pearce's more limited but homogeneous data: nevertheless, the revision to the period represents a real improvement. The fit of the observations of the secondary star can be improved if it is allowed to have a different value of V0 from the primary. System361Orbit1End System362Orbit1Begin The spectroscopic and photometric investigation by Andersen et al. completely supersedes the earlier spectroscopic work by D.H.P. Jones (Mon. Notes Astron. Soc. South Africa, 28, 5, 1969) and the light-curve observed by H.C. Lagerweij (Mon. Notes Astron. Soc. South Africa, 27, 17, 1968) and analyzed by G. Giuricin and F. Mardirossian (Astron. Astrophys., 94, 204, 1981). Although the secondary spectrum is seen, it is too faint to classify accurately, even at primary minimum. Judging from the results of the light-curve analysis, it is a main-sequence star of late A or early F type. Although the small eccentricity is judged to be real (and is required by the light-curve) the epoch given is the time of primary minimum. The values of K1 and V0 agree well with Jones' values; that of K2 is distinctly smaller than his (uncertain) value. Apsidal motion has not been detected and would not be expected to be detectable over the short interval in which the system has been observed. The stars rotate slowly and this may account for earlier classification of the primary as a giant star. The orbital inclination is close to 89 deg and the light-curve shows that Delta V is close to 2 magnitudes. System362Orbit1End System363Orbit1Begin Epoch is T0. According to H. Shapley (Princeton Obs. Contr., No. 3, 1915) i=83 deg and the light-ratio is about 0.07. Velocities obtained from the calcium lines differ from all the rest. System363Orbit1End System364Orbit1Begin Epoch is arbitrary zero: T0 about 2.15d later. System364Orbit1End System365Orbit1Begin Although these are the first orbital elements determined for the system, the duplicity was first noticed by R.K. Young (Publ. David Dunlap Obs., 1, 309, 1945). A circular orbit was assumed and the epoch is T0. The two spectra are nearly but not quite equal, the more massive component showing the slightly stronger spectrum. Beavers and Griffin suggest that the system might prove to share some of the characteristics of the RS CVn group. System365Orbit1End System366Orbit1Begin Smith's orbit remains the best and is in agreement with the results of R.H. Baker (Publ. Allegheny Obs., 1, 163, 1910) who also summarized earlier work. P. Galeotti and G. Guerrero (Mem. Soc. Astron. Ital., 39, 268, 1968) published appreciably lower values of K1 and K2 (100.3 km/s and 102.5 km/s respectively) but D.M. Popper and R. Carlos (Publ. Astron. Soc. Pacific, 82, 762, 1970) confirm the older values. Smith assumed zero eccentricity after a preliminary solution by Sterne's method gave e=0.011. The epoch, therefore, is T0. Petrie(I) found Delta m=0.13. Light curves in B and V and in four other filters by K.T. Johansen (Astron. Astrophys., 12, 165, 1971) show the two stars to be closely similar in luminosity and give i=77.8 deg. The precise value of the relative luminosity depends on the adopted ratio of the radii. Johansen's solution is in satisfactory agreement with the earlier one by S.L. Piotrowski (Astrophys. J., 108, 510, 1948). The far UV spectrum of this system has been discussed by D.J. Stickland and K.A. van der Hucht (Astron. Astrophys., 44, 139, 1975). J.D. Landstreet (Astrophys. J., 258, 369, 1982) failed to find a magnetic field in the system. O.J. Eggen (Astron. J., 88, 642, 1983) assigns the star to a `super cluster' that includes the Ursa Major cluster. The star is the brightest component of A.D.S. 4556: companions are 10.6m at 184.6" and 14.1m at 12.8". System366Orbit1End System367Orbit1Begin Lucy & Sweeney adopt a circular orbit. The star is said to be Am in the Bright Star Catalogue, but is not listed by Curchod and Hauck. The star is the brighter component of A.D.S. 4555: companion is 9.7m at 36.7". System367Orbit1End System368Orbit1Begin The new elements derived by Abt and Levy probably do represent some improvement on those found by C.T. Elvey (Astrophys. J., 60, 320, 1924) since the former were able to refine the period. The differences between the two sets of elements are not great. Abt and Levy give the spectral type as A3, A8, F2 from the K line, hydrogen lines and metallic lines, respectively. Elvey measured a faint secondary spectrum, apparently, of the same spectral type as the primary, on five plates to obtain a very tentative mass-ratio of 0.86. Abt and Levy made one measurement of the secondary spectrum, but do not report the velocity. Fekel (private communication) has detected the secondary spectrum in the red. System368Orbit1End System369Orbit1Begin The circular orbit obtained by Lucy & Sweeney, based on observations by O. Struve (Astrophys. J., 102, 74, 1945) seems preferable to Struve's original solution even though the nominal eccentricity is quite high (0.16). The epoch is T0. The spectral type of the primary is uncertain: Struve describes it as B2 or B3. Although this star is listed as an eclipsing binary, no good light curve has been published. According to B.S. Whitney (Astron. J., 64, 258, 1959) no eclipse of greater than 0.2m depth (photographic) was observable between 1953 and 1958. The variability of the star should be checked. System369Orbit1End System370Orbit1Begin Amplitude of the primary curve is very small, and gaseous streams may be distorting the observed spectrum. Smak's work is based both on his own observations and on two investigations by O. Struve (Astrophys. J., 104, 253, 1946 and 106, 92, 1947). S. Gaposchkin (Harvard Obs. Bull., No. 919, p. 29, 1949) found i=85.5 deg and the light ratio to be 0.42. Epoch is T0. System370Orbit1End System371Orbit1Begin Epoch is T0, the light-curve indicates that the orbit is circular. The secondary spectrum is visible only during primary eclipse. The minimum magnitude is estimated from the plot of a V light-curve obtained by J. Tremko and M. Vetesnik (Bull. Astron. Inst. Csl, 25, 331, 1974). They found an orbital inclination of 89 deg and a fractional luminosity for the primary of 0.76. From the same observations H.M.K. Al Naimiy (Astrophys. Space Sci., 46, 261, 1977) found 88 deg and 0.85, respectively. Although the star is not listed in I.D.S., there is a faint companion close enough to affect the photometry. System371Orbit1End System372Orbit1Begin This well-known visual binary is now recognized to be a quadruple system. The brighter component was long known to be a single-spectrum binary and Fekel has shown that the fainter component is a two-spectra binary -- and has thus removed its apparent discrepancy with the mass-luminosity relation. There is not yet available a homogeneous and completely satisfactory set of spectroscopic elements for the visual pair. Those derived by P. Bourgeois (Astrophys. J., 70, 256, 1929) are no longer acceptable since it has become clear that the period he adopted (17.5y) is too short, as first suggested by D.M. Popper (Astrophys. J., 109, 100, 1949). The visual orbit by V. Osvalds (Publ. McCormick Obs., 11, 175, 1964) at present appears to come closer than any others to representing the spectroscopic data. Fekel has performed a simultaneous solution on the observed velocities of A for the two orbital motions, having first derived the period, eccentricity and longitude of periastron from the motion of the centre of mass of B. (These quantities and V0 for the whole system were fixed in the final solution). He combined his data with that published by H.A. Abt, N.B. Sanwal and S.G. Levy (Astrophys. J. Supp., 43, 549, 1980). C.D. Scarfe also has unpublished observations of the system. Accurate spectral types are not given for the components of B, but they are estimated to be F-type dwarfs. The orbit was assumed circular and the epoch is T0. The value of V0 given for B is that appropriate to the epoch of observation. The two components are approximately equal in mass and luminosity. The elements for the brighter component of A are in fairly good agreement with earlier studies (C.D. Scarfe, Publ. Astron. Soc. Pacific, 79, 414, 1967; P. Bourgeois, op. cit.; E.B. Frost and O. Struve, Astrophys. J., 60, 197, 1924). The orbit is taken as circular, since the combined solution yields a very small negative eccentricity. From the K line, hydrogen lines and metallic lines, A. Slettebak (Astrophys. J., 109, 547, 1949) gives spectral types of A3, A8 and A7, respectively. The visual pair is A.D.S. 4617; a 14.0m star at 18.2" does not, however, appear to be physically associated with the multiple system. Reference: F.C.Fekel,,,, (Unpublished) System372Orbit1End System373Orbit1Begin This well-known visual binary is now recognized to be a quadruple system. The brighter component was long known to be a single-spectrum binary and Fekel has shown that the fainter component is a two-spectra binary -- and has thus removed its apparent discrepancy with the mass-luminosity relation. There is not yet available a homogeneous and completely satisfactory set of spectroscopic elements for the visual pair. Those derived by P. Bourgeois (Astrophys. J., 70, 256, 1929) are no longer acceptable since it has become clear that the period he adopted (17.5y) is too short, as first suggested by D.M. Popper (Astrophys. J., 109, 100, 1949). The visual orbit by V. Osvalds (Publ. McCormick Obs., 11, 175, 1964) at present appears to come closer than any others to representing the spectroscopic data. Fekel has performed a simultaneous solution on the observed velocities of A for the two orbital motions, having first derived the period, eccentricity and longitude of periastron from the motion of the centre of mass of B. (These quantities and V0 for the whole system were fixed in the final solution). He combined his data with that published by H.A. Abt, N.B. Sanwal and S.G. Levy (Astrophys. J. Supp., 43, 549, 1980). C.D. Scarfe also has unpublished observations of the system. Accurate spectral types are not given for the components of B, but they are estimated to be F-type dwarfs. The orbit was assumed circular and the epoch is T0. The value of V0 given for B is that appropriate to the epoch of observation. The two components are approximately equal in mass and luminosity. The elements for the brighter component of A are in fairly good agreement with earlier studies (C.D. Scarfe, Publ. Astron. Soc. Pacific, 79, 414, 1967; P. Bourgeois, op. cit.; E.B. Frost and O. Struve, Astrophys. J., 60, 197, 1924). The orbit is taken as circular, since the combined solution yields a very small negative eccentricity. From the K line, hydrogen lines and metallic lines, A. Slettebak (Astrophys. J., 109, 547, 1949) gives spectral types of A3, A8 and A7, respectively. The visual pair is A.D.S. 4617; a 14.0m star at 18.2" does not, however, appear to be physically associated with the multiple system. System373Orbit1End System374Orbit1Begin This well-known visual binary is now recognized to be a quadruple system. The brighter component was long known to be a single-spectrum binary and Fekel has shown that the fainter component is a two-spectra binary -- and has thus removed its apparent discrepancy with the mass-luminosity relation. There is not yet available a homogeneous and completely satisfactory set of spectroscopic elements for the visual pair. Those derived by P. Bourgeois (Astrophys. J., 70, 256, 1929) are no longer acceptable since it has become clear that the period he adopted (17.5y) is too short, as first suggested by D.M. Popper (Astrophys. J., 109, 100, 1949). The visual orbit by V. Osvalds (Publ. McCormick Obs., 11, 175, 1964) at present appears to come closer than any others to representing the spectroscopic data. Fekel has performed a simultaneous solution on the observed velocities of A for the two orbital motions, having first derived the period, eccentricity and longitude of periastron from the motion of the centre of mass of B. (These quantities and V0 for the whole system were fixed in the final solution). He combined his data with that published by H.A. Abt, N.B. Sanwal and S.G. Levy (Astrophys. J. Supp., 43, 549, 1980). C.D. Scarfe also has unpublished observations of the system. Accurate spectral types are not given for the components of B, but they are estimated to be F-type dwarfs. The orbit was assumed circular and the epoch is T0. The value of V0 given for B is that appropriate to the epoch of observation. The two components are approximately equal in mass and luminosity. The elements for the brighter component of A are in fairly good agreement with earlier studies (C.D. Scarfe, Publ. Astron. Soc. Pacific, 79, 414, 1967; P. Bourgeois, op. cit.; E.B. Frost and O. Struve, Astrophys. J., 60, 197, 1924). The orbit is taken as circular, since the combined solution yields a very small negative eccentricity. From the K line, hydrogen lines and metallic lines, A. Slettebak (Astrophys. J., 109, 547, 1949) gives spectral types of A3, A8 and A7, respectively. The visual pair is A.D.S. 4617; a 14.0m star at 18.2" does not, however, appear to be physically associated with the multiple system. Reference: F.C.Fekel,,,, (Unpublished) System374Orbit1End System375Orbit1Begin Although this bright star has long been recognized to be at least binary, Fekel and Scarfe have produced the first study of its orbits. The higher multiplicity was first discovered by occultation observations (J.L. Africano et al., Astron. J., 81, 650, 1976) and speckle interferometry (H.A. McAlister and F.C. Fekel, Astrophys. J. Supp., 43, 327, 1980). Fekel and Scarfe estimate individual apparent (V) magnitudes of 5.92, 6.66 and 6.67 for Aa, Ab and B, respectively. They suggest that the two components of A are evolved giants. Certainly those two stars are slow rotators and yet show no sign of spectral peculiarities. The value of V0 for the short period pair is variable. There are not yet sudegcient interferometric observations for a determination of the 13-year orbit in the plane of the sky, but Fekel and Scarfe quote a preliminary estimate by M. Halliwell that i=45 deg. It appears that the two orbits are not coplanar. System375Orbit1End System376Orbit1Begin Although this bright star has long been recognized to be at least binary, Fekel and Scarfe have produced the first study of its orbits. The higher multiplicity was first discovered by occultation observations (J.L. Africano et al., Astron. J., 81, 650, 1976) and speckle interferometry (H.A. McAlister and F.C. Fekel, Astrophys. J. Supp., 43, 327, 1980). Fekel and Scarfe estimate individual apparent (V) magnitudes of 5.92, 6.66 and 6.67 for Aa, Ab and B, respectively. They suggest that the two components of A are evolved giants. Certainly those two stars are slow rotators and yet show no sign of spectral peculiarities. The value of V0 for the short period pair is variable. There are not yet sudegcient interferometric observations for a determination of the 13-year orbit in the plane of the sky, but Fekel and Scarfe quote a preliminary estimate by M. Halliwell that i=45 deg. It appears that the two orbits are not coplanar. System376Orbit1End System377Orbit1Begin The new elements by Griffin and Radford are closely similar to those obtained by H.A. Abt and V.K. Kallarakal (Astrophys. J., 138, 140, 1963) who, however, adopted a slightly longer value for the period. The epoch is T0. An earlier investigation by R.K. Young (Publ. Dom. Astrophys. Obs., 1, 119, 1919), who found K1=11.74 km/s, was apparently vitiated by his inability to resolve the two spectra of the visual binary (separation 0.22", Delta m=0.3). The spectroscopic binary is the fainter member of the visual pair, whose period is estimated by Griffin and Radford to be about 14 years. Although Abt and Kallarakal discussed the velocity variation of the visual pair, there are as yet insufficient observations to reach any conclusion. The brighter component is of spectral type K0 III. There is also a 13.0m star at 96.6". System377Orbit1End System378Orbit1Begin Epoch is the time of superior conjunction of the Be star, whose spectrum is the only one visible. Peters estimates the secondary to be a star of solar mass. Shell spectra seen at definite phases are ascribed by Peters to gas streams conveying mass within the system. For an account of the far UV spectrum, see the same author (Publ. Astron. Soc. Pacific, 90, 494, 1978). System378Orbit1End System379Orbit1Begin Because omega is close to 180 deg and the eccentricity is high, the two spectra were resolved by Young at only one node. This may explain why he found omega1 and omega 2 are different. Petrie(II) found Delta m=0.39. The spectrum is variously classified as A4m or A5 from the K line and F2 from the metallic lines. System379Orbit1End System380Orbit1Begin Cowley's observations and elements clearly supersede the earlier results of K.G. Widing (Astrophys. J., 143, 121, 1966). The value given for K1 refers to the M-type star. Widing gave a value for K2 ; Cowley does not attempt to do so, but she infers a mass-ratio (B-type star.M-type star) of between 3 and 4 to 1, and an orbital inclination of around 24 deg. The early-type spectrum is difficult to classify, being associated with a shell spectrum. The early-type star is subject to outbursts whose occurrences appear to be correlated with orbital phase. System380Orbit1End System381Orbit1Begin These elements confirm those found by W.E. Harper (J. Roy. Astron. Soc. Can., 5, 16, 1911). Some slight evidence of the secondary spectrum was found on some of the spectrograms. A provisional value of 0.16 results for the mass-ratio. System381Orbit1End System382Orbit1Begin Both components display marginal Am characteristics in their spectra. Curchod and Hauck classify the primary as A4 and F0 from the K line and metal lines, respectively and give only A5 from the K line for the secondary. The visual magnitude difference is estimated to be between 0.22m and 0.24m. The authors themselves describe these elements as provisional. System382Orbit1End System383Orbit1Begin These new elements undoubtedly supersede the earlier determinations by R.P. Kraft (Astrophys. J., 135, 408, 1962) and by R.P. Kraft and W.J. Luyten (Astrophys. J., 142, 1041, 1965). In particular the period now seems to be unambiguously defined. As Shafter and Harkness point out, however, it is not clear how far velocities derived from the emission lines arising in the accretion disk reflect the actual motion of the white-dwarf component. In addition, the systemic velocity has not been determined from these observations (Kraft and Luyten gave +33 km/s). The orbit was assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The velocity-curve is well covered. System383Orbit1End System384Orbit1Begin Variability of the velocity of this star has been suspected for a long time. K. Kodaira (Publ. Astron. Soc. Japan, 23, 159, 1971) included the star in a list of `suspected velocity-variables' for which he gave orbital elements derived from heterogeneous published velocities. Abt and Levy find a different period. Two faint companions, 4" apart and 40" from the bright star, are listed in I.D.S. The star is also a member of the association Cas-Tau OB1. System384Orbit1End System385Orbit1Begin Although the observations show a relatively large scatter, there are many of them and the elements are probably well determined. The epoch is an arbitrary zero. Thackeray estimated the spectral type of the secondary to be between B0.5 and B3 and he estimated K2=1.89K1 (about 316 km/s). This value was used by J.A. Eaton and C.-C. Wu (Publ. Astron. Soc. Pacific, 95, 319, 1987) in their solution of far ultraviolet light curves, and led them to postulate that the system is an Algol system in the sense that the secondary fills its Roche lobe. Other UV light-curves were obtained by R.G. Evans (Mon. Not. Roy. Astron. Soc., 167, 517, 1974) and a visual light-curve was also obtained by A.J. Cousins (Mon. Not. Roy. Astron. Soc., 131, 443, 1966). R.E. Wilson and J.B. Rafert (Astrophys. Space Sci., 76, 23, 1981) re-analyzed these data. All photometric solutions seem to agree on an orbital inclination of around 66 deg, a fractional luminosity for the primary star of about 0.8 and fairly similar spectral types for the two components. The behaviour of the lambda 4686 He II line suggests that there may be a hot spot on the surface of the primary star. Y. Kondo, G.E. McCluskey and W.A. Feibelman (Publ. Astron. Soc. Pacific, 92, 688, 1980) find evidence in the UV spectrum for mass loss from the primary star. System385Orbit1End System386Orbit1Begin The variability of the velocity of this star is probably established, but the elements are very uncertain since none of the observations lie on the ascending branch or at either node. According to I.D.S. there is a companion at about 0.5" with Delta m=0. System386Orbit1End System387Orbit1Begin These elements supersede those determined by W.H. Christie (Astrophys. J., 83, 433, 1936). The system may show shallow eclipses, but the intrinsic variations of the M-type star make it difficult to be sure of this. It might be possible to determine an astrometric orbit. Star is brighter component of A.D.S. 4841: companion 8.8m at 1.4". A.J. Deutsch (Sky Telesc., 21, 261, 1961) indicates that all three stars are surrounded by a gaseous envelope. System387Orbit1End System388Orbit1Begin This is a cataclysmic variable and known X-ray source, and the orbital elements are difficult to determine and to interpret. Those given in the Catalogue are derived from measures of the wings of the H-alpha emission line. The orbit was assumed to be circular and the epoch is the time of superior conjunction of the emission-line source. The spectrum cannot readily be classified: the underlying star is assumed to be a white dwarf. Different elements, based on the H-beta emission line were published almost simultaneously by J.B. Hutchings, R. Link and D. Crampton (Publ. Astron. Soc. Pacific, 95, 264, 1983). The unusual photometric behaviour of this star is described by M.D. Popova (Peremm. Zvezdy, 15, 534, 1965). System388Orbit1End System389Orbit1Begin The chief evidence for the early-type component is the composite K line. Precise spectral classification is therefore difficult. If the secondary is B8 or B9, then Petrie found Delta m=1.5. The system violates the mass-luminosity relation. The velocities of the secondary component are based only on the K line. The semi-amplitude K2 is, therefore, very uncertain, but it would seem to be impossible to reverse the mass-ratio. System389Orbit1End System390Orbit1Begin System390Orbit1End System391Orbit1Begin The spectral type is suggested by Griffin on the basis of the colours of the star and the depths of the radial-velocity traces. The H.D. type is K0. System391Orbit1End System392Orbit1Begin Luyten and Lucy & Sweeney both adopt a circular orbit for this system. System392Orbit1End System393Orbit1Begin The star is the fainter member of A.D.S. 4924; the brighter component is H.D. 43931. Radford and Griffin point out that the two stars are more than a minute of arc apart in the sky and a physical relationship is unlikely to exist between them. While an eccentric orbit appears to satisfy the observations better than a circular one, the latter possibility cannot be entirely ruled out. The values of T and omega are correspondingly uncertain. System393Orbit1End System394Orbit1Begin A slightly shorter period is derived for the secondary component. The orbit is assumed circular and the epoch is the time of inferior conjunction of the more massive component. The coverage of the velocity-curve is incomplete. System394Orbit1End System395Orbit1Begin A 7.7m companion at 157.5" is listed in I.D.S. Although the proper motions of the companion and zeta CMa are both small, they are not similar. Reference: A.Colacevich, Oss. e Mem. Arcetri, 59, 15, 1941 System395Orbit1End System396Orbit1Begin The visible spectrum is that of a late K dwarf, with emission lines assumed to arise in an accretion disk around a compact object. Only half the velocity-curve is covered. The orbit is assumed circular and the epoch is T0. The observed light variation can be largely accounted for by the ellipticity of the K dwarf. Because the minimum mass of the compact object, as deduced from the amplitude of the velocity variation of the K dwarf, is 3.2 MSol, McClintock and Remillard deduce that the compact object is a black hole. Other spectroscopic and spectrophotometric studies include J.B. Oke and J.L. Greenstein (Astrophys. J., 211, 872, 1977), J.B. Oke (Astrophys. J., 217, 181, 1977), F. Ciatti, A. Mammano and A. Vittone (Astron. Astrophys., 56, 311, 1977), J.A.J. Whelan et al. (Mon. Not. Roy. Astron. Soc., 180, 657, 1977) and P. Murdin et al. (Mon. Not. Roy. Astron. Soc., 192, 709, 1980). System396Orbit1End System397Orbit1Begin Popper's spectroscopic study supersedes the earlier one by W.E. Harper (Publ. Dom. Obs., 2, 167, 1915) as well as his own preliminary studies (D.M. Popper, Publ. Astron. Soc. Pacific, 74, 129, 1962, B.C. Douglas and D.M. Popper, ibid., 75, 411, 1963). Values of e and omega are taken from the last-cited paper. The epoch is the time of primary minimum. The value of K2 is obtained from the D lines, although the secondary component of H-alpha is also visible. (The same lines were also detected by T.M. Rachkovskaja, Izv. Krym. Astrofiz. Obs., 52, 35, 1974). The secondary spectrum appears to be early F. A combined spectroscopic and photometric discussion by M. Kondo (Ann. Tokyo Obs., 16, 1, 1976) was not included in the Seventh Catalogue. His value of K2 (83.1 km/s) is somewhat smaller than Popper's and he is able to satisfy the observations of both components with only one value of V0 (11.6 km/s) rather than the two discrepant values that Popper needed and could not fully explain. Nevertheless, Popper's results appear to be the more self-consistent, possibly because of his greater selectivity in the choice of lines to be measured. The minimum masses derived from the two investigations agree within their quoted uncertainties. A.P. Linnell (Astron. J., 71, 458, 1966) and E. Budding (Astrophys. Space Sci., 30, 433, 1974) could not solve the light-curve without assuming possibly variable third light. Kondo did not have that problem. All agree on an orbital inclination close to 87 deg. Kondo gives a fractional luminosity (in blue) for the primary component of 0.73, which is about the middle of the range of other estimates. M.I. Lavrov and N.V. Lavrova (Astron. Tsirk., No. 1165, 3, 1980) quote similar results and propose that the line of apsides rotates in about 2,000 years. Budding noted a faint companion at 50" from the eclipsing pair. It is not listed in I.D.S. and cannot account for the third light. System397Orbit1End System398Orbit1Begin The star appears to be an early-type contact binary: the period may be slightly variable and the small orbital eccentricity found by Pearce is probably not physically significant. Petrie(II) found Delta m=1.31. B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) analyzed Gum's unfiltered photometric observations to obtain an orbital inclination of 65 deg and a fractional luminosity for the primary star of 0.92. Although they emphasized the uncertainty of the photometric solution, their results suggest that the measures of the secondary spectrum should be treated with caution -- especially in view of Pearce's own remarks on the difficulty of measuring both components. System398Orbit1End System399Orbit1Begin These results confirm and improve the elements found by R.E. Wilson and C.M. Huffer (Lick Obs. Bull., 10, 15, 1918). System399Orbit1End System400Orbit1Begin Although the variability of this star's velocity has been long known, these elements are the first to be determined. The mean spectrum is either K1 III or K2 III. The difference (if any) between the spectra of both components is unknown. Griffin estimates Delta m=1.24, if both components are of the same spectral type. He deduces that both components are giants. System400Orbit1End System401Orbit1Begin The elements were determined graphically and the epoch is T0. A closely similar set of elements was computed by Lucy & Sweeney, who also assumed a circular orbit. There is some evidence of a rotation effect during primary minimum. All earlier discussions of the light-curve are superseded by that by R.W. Hilditch, D.M. Harland and B.J. McLean (Mon. Not. Roy. Astron. Soc., 187, 797, 1979). They find that the system consists of a G3 V primary and a K4 V secondary. The latter component is an intrinsic (BY Dra) variable, which accounts for the difficulties previous investigators experienced in analyzing the light-curve. Hilditch et al. estimate that the orbital inclination is 80 deg and Delta V (at quadratures) is over three magnitudes. They also produce evidence (from times of minima) that the close pair revolves around a third body in a period of about 64 years. System401Orbit1End System402Orbit1Begin All the elements are taken from the study by Griffin and Emerson, except K2 which they could not determine since they did not detect the secondary spectrum. The value of K2 comes from the observations made by J. Tomkin (Astron. J., 85, 294, 1980) who detected the secondary spectrum with a Reticon. Although he published new orbital elements for both components, the older elements are preferred for the primary because they are based on considerably more observations. The two sets of elements agree well except for V0. The apparent change observed in that element may be real but could easily be a result of the different ways in which the individual velocity measurements were standardized. Tomkin thought the minimum masses to be high enough to justify a search for eclipses. None were observed. The star has been identified as a BY Dra variable by S.S. Vogt, D.R. Soderblom and G.D. Penrod (Astrophys. J., 269, 250, 1983) who also classify the spectrum as dK2e. The star is the brighter component of A.D.S. 5054: companion is 13.7m at 1.3". System402Orbit1End System403Orbit1Begin The spectral type is based on the observed colours and radial-velocity traces. System403Orbit1End System404Orbit1Begin Lu and Hutchings give two possible periods, 0.1553d and 0.1390d, and two solutions for each period -- one from measures of the emission-line wings and one from measures of the emission peak. A circular orbit is assumed in each case and the epoch is T0. Values of V0 range from 66 km/s to 82 km/s, and of K1 from 65 km/s to 72 km/s. The system is thought to be an old nova. System404Orbit1End System405Orbit1Begin Velocity variation with a period of about 235 d was first suspected by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 4, 1, 1926). An orbit was derived by P.W. Merrill (Astrophys. J., 116, 498, 1952) very similar to the one derived graphically by Cowley and given in the Catalogue. Lucy & Sweeney have recomputed the orbit from Cowley's observations and adopt a circular orbit. The value of K given refers to the late-type component. Another recent spectroscopic study, from which no elements were derived, is that by A.A. Boyarchuk and I.I. Pronik (Izv. Krym. Astrofiz. Obs., 37, 236, 1967). They give spectral types of B1 IV+K0 III. A.P. Cowley et al. (Astron. J., 71, 851, 1966) report on the suppression of H-epsilon absorption in the system and suggest flares are responsible. Photoelectric light curves have been published by N.L. Magalashvili and Ya.I. Kumsishvili (Bulletin Abastumani Obs., No. 37, 3, 1969). M. Plavec and P. Harmanec (Inf. Bull. Var. Stars, No. 613, 1972) have emphasized the correlation of the appearance of the shell spectrum with orbital phase. The possible evolutionary state of the system has been discussed by P. Harmanec (Bull. Astron. Inst. Csl, 25, 236, 1974). For a description of the UV spectrum and a model, see J. Sahade and E. Brandi (Rev. Mex. Astron. Astrofis., 10, 229, 1985). System405Orbit1End System406Orbit1Begin The new orbit by Kitamura et al. is based on many more spectrograms than the earlier one by L.T. Slocum (Lick Obs. Bull., 19, 147, 1942), which is also derived from high-dispersion spectrograms, and entirely supersedes the orbit derived by A.H. Joy (Publ. Astron. Soc. Pacific, 30, 253, 1918). Both components are Am stars; according to D.M. Popper (Astrophys. J., 169, 549, 1971) the combined spectrum is A2 from the K line of Ca II and A5 from the metallic lines. Kitamura et al. find some evidence for a variation of apparent metallicism with phase. The orbit was assumed circular, and the epoch is the time of primary minimum adopted by M. Kiyokawa and M. Kitamura (Ann. Tokyo Obs. 2nd Ser., 15, 117, 1975) in their companion study of the UBV light-curves of the system. The magnitudes given are taken from this second paper. Their analysis gives i=87.6deg and the fractional luminosity of the bright component (in V) as 0.54. A new analysis of the same observations by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) did not change these figures substantially. Petrie(I) found Delta m=0.28. System406Orbit1End System407Orbit1Begin The epoch is T0. A barium star. System407Orbit1End System408Orbit1Begin The star is faint and the spectral lines broad and it was difficult to obtain good spectrograms of the system. Modern observations might lead to a considerable improvement in our knowledge of it. The spectral types are estimated from UBV photometry. The epoch is T0. The best light-curves are those obtained in the region of 7000 A by R. Brukalska et al. (Acta Astron., 19, 257, 1969) who found an orbital inclination of 90 deg and a fractional luminosity (near 7400 Angstroms) of 0.72. M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 273, 1980) from the same material found 86 deg and 0.92. System408Orbit1End System409Orbit1Begin Lucy & Sweeney adopt a circular orbit for this system. System409Orbit1End System410Orbit1Begin The star was included in the Catalogue on the strength of the abstract cited. A more detailed paper by the same authors (Astron. J., 94, 1302, 1987) arrived just before this note was written. The values of K1 and V0 come from the abstract, those of e and omega from the paper, which also gives P=12.6315y and T=1954.0631. The orbital inclination is 101.3 deg and the parallax is 0.0326". The star is an astrometric binary; the secondary component has not yet been seen, nor even detected interferometrically. Without the astrometric observations, one might doubt the reality of the velocity variation, since the scatter of individual observations is comparable to the range of variation. The best observations lie close to the curve, however, and the consistency of spectroscopic and astrometric observations leave little doubt that the values of the elements are close to those found. System410Orbit1End System411Orbit1Begin Stickland derived a new orbital solution from all available material, including IUE observations. He adopted a circular orbit after finding only a small eccentricity. The epoch is T0. The value of V0 is somewhat arbitrary since all series of observations have been reduced to the value of V0 found by Plaskett. There is no sign of the secondary spectrum and Stickland treated the system as a one-spectrum system. The orbit of the primary component now seems fairly well known. The system (Plaskett's star) is probably still the most massive known, since the mass-function is high. So far no eclipses have been detected (although there is a possible small variation in the light) so the orbital inclination is probably appreciably different from 90 deg. Earlier estimates of K2 should, however, be treated with caution. The orbit was originally determined by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 2, 147, 1922) and other studies have been published by O. Struve (Astrophys. J., 107, 327, 1948), K.D. Abhyankar (Astrophys. J. Supp., 4, 157, 1959), J.Sahade (La Plata Symp. Stellar Evolution, 185, 1962) and J.B. Hutchings and A.P. Cowley (Astrophys. J., 206, 490, 1976). A brief study of the H-alpha profile has also been published by R. Rajamohan (Astrophys. Space Sci., 99, 153, 1984). Although Petrie(II) found Delta m=0.78, this value should be also treated with caution in view of the uncertainties in the interpretation of the secondary spectrum. Abhyankar found Delta m varied with phase. System411Orbit1End System412Orbit1Begin The spectral type assigned to the secondary is approximate. The orbit was assumed to be circular after a preliminary solution showed the eccentricity to be negligibly small. The epoch is T0. The orbital inclination is estimated to be about 35 deg. System412Orbit1End System413Orbit1Begin Only one spectrum is visible, and the type of the secondary is deduced from the light-curve. Two photoelectric light curves have been published, one in B and V by C. Bartolini (Mem. Soc. Astron. Ital., 38, 311, 1967), the other by A.J. Harris (Astron. J., 73, 164, 1968). The results are in good agreement and Bartolini finds i=76.9 deg; the fractional luminosity of the primary star (in V) is 0.93. The V magnitude given in the Catalogue is an isolated observation of unknown phase, but probably close to maximum light. The depth of primary eclipse is about 0.45m in V. System413Orbit1End System414Orbit1Begin This is the former Nova Mon (1939). A photometric study (from which the value for the period has been taken) was published by E.L. Robinson, R.E. Nather and S.O. Kepler (Astrophys. J., 254, 646, 1982). Although they give no spectral types explicitly, they find that the system contains a white dwarf and a late-type component (which gives about 0.06 of the total light). They find the accretion disk to be exceptionally large and luminous. Seitter's velocity-curve is derived from measures of emission lines and is appreciably better than many published for cataclysmic variables. There is, however, a prominent distortion near the time of eclipse, strongly reminiscent of that seen in Algol-type systems. The orbit was assumed circular and the epoch is the time of primary minimum. No value is given for V0. The velocities were determined by cross-correlation and V0 has apparently been arbitrarily set at zero. System414Orbit1End System415Orbit1Begin D. Chochol and A. Kucera (Inf. Bull. Var. Stars, No. 1998, 1981) showed this star to be an eclipsing variable with a period of either 26.9d or 53.8d. Stagni et al. have shown clearly that the longer period is correct. The spectrum displays shell features (including emission at H-alpha) and Chochol and Kucera classify it as B3 II-III. The B4 classification is taken from R.M. Petrie and J.A. Pearce (Publ. Dom. Astrophys. Obs., 12, 1, 1962). The measures of the secondary component show a very wide scatter. Taken at their face value, they imply the high masses given in the Catalogue. Observations made at Victoria, at higher dispersion and on superior emulsion, do not show the secondary spectrum, but they do confirm the longer period and the approximate elements of the primary star's orbit. System415Orbit1End System416Orbit1Begin P=50.04y, T=1894.133. The elements P, T, e, omega are from the visual orbit derived by Aitken (who also gives i=43.31 deg). The elements K1 and V0 are given by E.B. Frost, J.H. Moore, and H.S. Jones in Trans. Inter. Astron. Union, 3, 175, 1928. Since omega is taken from the visual orbit, it must be, in accordance with convention, the value of omega for the secondary component: omega 1, presumably, is 325.69 deg. Several attempts have been made to find short-period perturbations in the elliptical motion. Aitken dismissed those made up to the time of his paper. Some evidence of a 4.55y period was put forward by N. Voronov (Tashkent Bull., 1, No. 4, 1934) but it is not convincing. A discussion of the spectrum of Sirius B has been published by E. Bohm-Vitense, T. Dettmann and S. Kaprinidis (Astrophys. J., 232, L189, 1979). Besides the two stars considered here, the system A.D.S. 5423 contains a 14.0m star at 31.6" and a possible companion to Sirius B at about 1.5". System416Orbit1End System417Orbit1Begin This is a cataclysmic variable observed during outburst. The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The period found is close to one of two values previously identified as probable by J.B. Hutchings, A.P. Cowley and D. Crampton (Publ. Astron. Soc. Pacific, 93, 741, 1981). The magnitude given is an isolated measurement by T. Chlebowski, J.P. Helpern and J.E. Steiner (Astrophys. J., 247, L35, 1981); the brightness varies by 2-3 magnitudes. The last-named authors also find some evidence for a magnetic field in the system. System417Orbit1End System418Orbit1Begin This is a cataclysmic variable of the SU UMa type. The minimum magnitude given is only approximate. The only visible spectral features are emission lines and the orbital elements are based on measures of them. The orbit is assumed circular and the epoch is superior conjunction of the emission-line source. The orbital inclination is estimated to lie between 45 deg and 65 deg. System418Orbit1End System419Orbit1Begin System419Orbit1End System420Orbit1Begin The spectral types are from J.J. Dobias and M.J. Plavec (Publ. Astron. Soc. Pacific, 99, 274, 1987) and are obtained from fitting model atmospheres in the UV rather than from traditional classification. The luminosity class of the primary (which may be a giant) is uncertain and the spectral subclass of the secondary is uncertain by two divisions either way. The epoch is the time of minimum given by D.S. Hall and K. Walter (Astron. Astrophys. Supp., 20, 227, 1975) since it is unclear precisely what epoch Gaposchkin used. The only orbital elements ever determined are Gaposchkin's although A.B. Wyse (Lick Obs. Bull., 17, 37, 1934) also studied the system spectroscopically. It is now clear that Gaposchkin's elements are seriously affected by the presence of circumstellar matter, the effects of which show up in the work of Dobias and Plavec and in the solution by Hall and Walter (Astron. Astrophys., 38, 225, 1975) of their own light-curve (op. cit.). The latters' `conventional' solution gives an orbital inclination of 85 deg and a fractional luminosity in V for the primary component of 0.75. System420Orbit1End System421Orbit1Begin The epoch is the time of primary minimum. The orbit was assumed circular, in accordance with the light-curve. To judge from the colour indices of the two stars (as obtained from a solution of the light-curve) the two spectra are closely similar. The primary is found to give 0.60 of the total light in V (Delta V=0.34m). The orbital inclination is very close to 90 deg. System421Orbit1End System422Orbit1Begin The star appears to be a hot sub-dwarf. The elements given in the Catalogue were derived by Thackeray after omitting certain of the observations. There is some evidence of the secondary spectrum, but no reliable measures could be made. Neither eclipses nor ellipsoidal light-variations could be found. For details of the atmospheric structure of the primary component and the possible evolutionary status of the system, see R.P. Kudritzki and K.P. Simon (Astron. Astrophys., 70, 653, 1978). System422Orbit1End System423Orbit1Begin Lucy & Sweeney adopt a circular orbit. System423Orbit1End System424Orbit1Begin Epoch is T0. This is one of the few graphically determined sets of elements that seem to deserve a quality classification better than d. Lucy & Sweeney adopt a circular orbit and give very similar values of K1 and V0. System424Orbit1End System425Orbit1Begin The spectral type is uncertain. The hydrogen lines are too strong for B9 but the absence of a K line suggests a type earlier than A0. Struve thought the primary may be sub-luminous. In a recent paper, D. Ya. Martynov and A.I. Khaliullina (Astron. Zh., 63, 288, 1986) suggest spectral types of B7 V and B8 V for the two stars. They find that the primary gives 0.53 of the light in V (Delta m=0.11) and that the orbital inclination is close to 89 deg. These results are consistent with Struve's belief that the values of K1, e and omega were affected by blending of the two spectra. No new complete investigation of the velocity-curve has been made since Struve, but Martynov and Khaliullina report a few new spectrograms that appear to support their conclusion (from photometry) that the system displays apsidal rotation in a period close to 300 years. Observed changes in the orbital period, however, seem to be more complex than those expected from simple apsidal motion. System425Orbit1End System426Orbit1Begin The composite nature of the spectrum leaves little doubt that the star is a binary, and the proposed mass-ratio is probably not far wrong. The remaining elements can only be considered as preliminary, as Hendry herself points out. The important node is not covered by observations at all. The emission-line strength in the early-type spectrum apparently varies. The period (as given by Hendry) is 58 years. System426Orbit1End System427Orbit1Begin The ground-based and IUE observations on which the study by Sahade and Ferrer is based supersede those studied by J. Sahade and C.U. Cesco (Astrophys. J., 101, 235, 1945). Nevertheless, the scatter of individual velocities is still large. The epoch is the time of minimum as derived by L. Lorenzi (Astron. Astrophys., 85, 342, 1980; see also Astron. Astrophys. Supp., 40, 271, 1980 and Acta Astron., 32, 431, 1982). The orbital elements given by Sahade and Ferrer are derived from the mean of the absorption lines of helium and H9 to H11, except that the value for V0 is derived from helium lines only. Different lines give different elements. A circular orbit was assumed. D.M. Popper (Publ. Astron. Soc. Pacific, 74, 129, 1962) detected the D lines of the secondary spectrum and emission at H-alpha. Lorenzi found evidence for a periodic intrinsic variation in the light of the system, as well as the variation due to eclipses. He deduced an orbital inclination of 82 deg and a fractional luminosity for the primary star of 0.93. Circumstellar matter in the system is briefly discussed by G.J. Peters (Bull. Am. Astron. Soc., 19, 713, 1987). System427Orbit1End System428Orbit1Begin The orbit is assumed circular and the epoch is T0. Burki and Mayor draw attention to the combination of the luminosity class assigned to the spectrum and the relatively short period -- the shortest known for an F-type supergiant, if the luminosity classification is correct. System428Orbit1End System429Orbit1Begin The orbit was assumed circular and the epoch is the inferior conjunction of the primary star. The star is the brightest member of A.D.S. 5705: companions are 15.1m at 2.5" and 9.2m at 23.2". System429Orbit1End System430Orbit1Begin The short-period pair is an eclipsing system consisting of two nearly identical early-type stars. The eclipse ephemeris shows a periodic term which is ascribed to a third body. There are not yet any direct determinations of K1 and V0 for the long-period system, and the orbital elements given are derived from the observed effects of light-time. They correspond to values of a sin i of about 3E8 km, and of K of about 48 km/s. The minimum magnitude given for the eclipsing pair is an estimate -- the light-curve is variable. The epoch in the short-period orbit is the time of primary minimum; the value of V0 must, of course, be variable. Double lines in the spectrum were first reported by F.J. Neubauer (Astrophys. J., 98, 300, 1943) and eclipses were discovered by A.F.J. Moffat and N. Vogt (Astron. Astrophys., 30, 381, 1974). Solution of the light-curve allowing for third light gives an orbital inclination for the eclipsing pair of about 88 deg. It is estimated that the third body is a B4 giant and is in fact somewhat brighter than either component of the eclipsing pair -- but its spectrum is difficult to distinguish from theirs. Apparent visual magnitudes of 9.40, 9.52 and 9.03 are estimated for A, B and C respectively. System430Orbit1End System431Orbit1Begin The short-period pair is an eclipsing system consisting of two nearly identical early-type stars. The eclipse ephemeris shows a periodic term which is ascribed to a third body. There are not yet any direct determinations of K1 and V0 for the long-period system, and the orbital elements given are derived from the observed effects of light-time. They correspond to values of a sin i of about 3E8 km, and of K of about 48 km/s. The minimum magnitude given for the eclipsing pair is an estimate -- the light-curve is variable. The epoch in the short-period orbit is the time of primary minimum; the value of V0 must, of course, be variable. Double lines in the spectrum were first reported by F.J. Neubauer (Astrophys. J., 98, 300, 1943) and eclipses were discovered by A.F.J. Moffat and N. Vogt (Astron. Astrophys., 30, 381, 1974). Solution of the light-curve allowing for third light gives an orbital inclination for the eclipsing pair of about 88 deg. It is estimated that the third body is a B4 giant and is in fact somewhat brighter than either component of the eclipsing pair -- but its spectrum is difficult to distinguish from theirs. Apparent visual magnitudes of 9.40, 9.52 and 9.03 are estimated for A, B and C respectively. System431Orbit1End System432Orbit1Begin This is an eclipsing member of the RS CVn group; H and K emission are seen in the spectrum. Imbert identifies the cooler component as the more massive one. The spectral type of the hotter component is uncertain. The orbital eccentricity is probably not significant. The period was taken from P. Ahnert (Inf. Bull. Var. Stars, No. 1150, 1976) but F. Scaltriti (Astron. Astrophys. Supp., 35, 291, 1979) proposes a slightly different value. Scaltriti analyzes the light-curve to obtain an orbital inclination of 86 deg and a fractional luminosity (approximately in V) of 0.64 for the cooler component. Imbert's estimates of the spectral types should be preferred to his. System432Orbit1End System433Orbit1Begin A circular orbit was assumed although more recent photometric work (C.D. Kandpal, Astrophys. Space Sci., 40, 3, 1976) suggests that the orbit may be eccentric. The epoch given is the time of primary minimum as determined by Scaltriti, since Struve arbitrarily took one of the nearly equal minima as phase zero. The elements are based on velocities derived only from the helium lines, since the hydrogen lines are often blended. Scaltriti found an orbital inclination of about 86 deg and a fractional luminosity (in V) of the larger component of 0.55. G. Giuricin et al. (Astron. Astrophys. Supp., 39, 255, 1980), using the same observations found 88 deg and 0.67. The star has sometimes been confused with H.D. 54003 (BD+04 1826). System433Orbit1End System434Orbit1Begin This dwarf M-type binary is also known as a flare star. Tomkin and Pettersen estimate the light ratio to be about 0.7 and the orbital inclination to be close to 90 deg. System434Orbit1End System435Orbit1Begin The elements agree quite closely with those derived by R.F. Sanford (Astrophys. J., 56, 446, 1922) and this agreement, rather than the quality of either determination separately, merits the b classification. The orbit was assumed circular after a preliminary solution showed the eccentricity to be very small. The epoch is T0. It is unclear whether or not a reported occultation component is the spectroscopic secondary. The system is the brightest component of A.D.S. 5827; B is 13.0m at about 23" and C is 7.7m at about 110". Proper motions indicate that C, at least, is unconnected with the spectroscopic pair. System435Orbit1End System436Orbit1Begin Spectrum may be variable. No analysis of the light-curve available. System436Orbit1End System437Orbit1Begin The spectral type is uncertain by one sub-class and the star may be a subgiant since the trigonometrically measured parallax is considerably smaller than would be expected for a main-sequence star of its spectral type. System437Orbit1End System438Orbit1Begin There are few observations of the secondary, but the primary velocity-curve is well observed. However, all Cambridge observations had to be corrected for blending of the two component spectra. Probably, both components are late-type giants. System438Orbit1End System439Orbit1Begin The primary (Ap) spectrum shows strong lines of the iron-group elements and of Sr II and Eu II. Only the K line and lambda 4481 of the secondary spectrum are visible. Of these, only the K line was measured for radial velocity. From those measures a mass ratio (Ap star companion) of 0.75 is found, giving minimum masses of 1.23 MSol and 1.65 MSol. The Ap star has a magnetic field that varies, but not with the orbital period. Instead, a period of 36.5d is suggested. Bonsack estimates that the Ap star produces about half the continuous flux in the blue region of the spectrum. System439Orbit1End System440Orbit1Begin System440Orbit1End System441Orbit1Begin This system consists of two similar early A-type stars that show marginal Am characteristics. The orbit is assumed circular, in accordance with the photometric observations. The epoch is primary minimum. The authors also analyze their uvby light-curve and find that the orbital inclination is close to 87 deg and Delta V=0.43m. System441Orbit1End System442Orbit1Begin Brighter component of A.D.S. 5983, for which a tentative orbit has been computed. (See J. Hopmann, Mitt. Sternw. Wien, 10, 191, 1960). The system may thus be at least triple. System442Orbit1End System443Orbit1Begin Earlier studies by W.E. Harper (Publ. Dom. Astrophys. Obs., 4, 115, 1917), J.A. Pearce (Publ. Dom. Obs., 6, 49, 1932), W.J. Luyten and E.G. Ebbighausen (Astrophys. J., 82, 246, 1955) and O. Struve and F. Sherman (Astrophys. J., 93, 84, 1941) are all in reasonable agreement with the elements given in the Catalogue except for V0. If V0 is genuinely variable, it is more likely to reflect the presence of a stellar wind than of a third body (J.B. Hutchings, Publ. Astron. Soc. Pacific, 89, 668, 1977). Hutchings finds a significantly larger value of K1 (243 km/s) but his observations are few. The value of K2 is much less well known, estimates vary from 288 km/s (Pearce) to 185 km/s (Struve et al.), but it seems likely that the secondary star is the more massive. The secondary component may also require a different value of V0. Observations in the UV provide evidence of gas streaming and mass loss (of about 1E-6 MSol/yr) through stellar winds (G.E. McCluskey, Y. Kondo and D.C. Morton, Astrophys. J., 201, 607, 1975; G.E. McCluskey and Y. Kondo, Astrophys. J., 208, 760, 1976). Both ultraviolet and BV light-curves have now been obtained. Analyses have been published by M. Parthasarathy (Mon. Not. Roy. Astron. Soc., 185, 485, 1978). K.-C. Leung and D.P. Schneider (Astrophys. J., 222, 924, 1978) and J.A. Eaton (Astrophys. J., 220, 924, 1978). Agreement is not good, but the orbital inclination is probably around 70 deg and the two stars are of comparable luminosity. Several authors give the primary's luminosity class as I. System443Orbit1End System444Orbit1Begin This confirms an earlier orbit by O. Struve and A. Pogo (Astrophys. J., 68, 335, 1928). Star is brightest component of A.D.S. 5977. Four companions are listed in I.D.S. System444Orbit1End System445Orbit1Begin Pearce assumed values of P, T, e, and omega from an earlier investigation by W.E. Harper (Publ. Dom. Obs., 4, 235, 1918). Harper obtained new observations (Publ. Dom. Astrophys. Obs., 6, 224, 1935) but did not revise his orbital elements except for deriving a mass-ratio of 0.6 (compare with Pearce's value of 0.53). A later investigation by G. Mannino and L. Cumis (Mem. Soc. Astron. Ital.(N.S.), 33, fasc. 2, 1962) resulted in a lower value of K1 (91 km/s) and a larger V0 (+26 km/s). Petrie(II) found Delta m=1.14. Star is brightest component of A.D.S. 6012: principal companion is 6.5m at 14.8". System445Orbit1End System446Orbit1Begin Many earlier investigations (F.C. Jordan, Publ. Allegheny Obs., 3, 49, 1913, B.W. Sitterly, Astron. J., 48, 190, 1940, O. Struve and B. Smith, Astrophys. J., 111, 27, 1950, P. Galeotti, Astrophys. Space Sci., 7, 87, 1970; and M. Kitamura, Astrophys. Space Sci., 3, 161, 1969) are superseded by Tomkin's study because he succeeded in detecting the secondary spectrum. The spectral type given for the primary is based partly on K. Sato's UBV photometry (Publ. Astron. Soc. Japan, 23, 335, 1971); that for the secondary comes from the photometric analysis by K.R. Radhakrishnan, M.B.K. Sarma and K.D. Abhyankar (Astrophys. Space Sci., 99, 229, 1984). The epoch is the time of primary minimum: Tomkin assumed a circular orbit in accordance with the photometric results. Besides those already mentioned, photometric studies have been published by E.F. Guinan (Astron. J., 82, 51, 1977) and B. Cester et al. (Astrophys. Space Sci., 36, 273, 1979). All analyses agree on an orbital inclination close to 80 deg and a fractional luminosity (in V) for the primary star of at least 0.90. The primary's velocity- curve is probably now well determined. The descending node of the secondary's curve is defined by only one observation. It is unlikely, however, that the mass-ratio will be much altered by future observations. The secondary is indeed undermassive -- Tomkin suggests that it has lost 80 percent of its mass -- but the primary component is not so seriously undermassive as it was once believed to be. System446Orbit1End System447Orbit1Begin Published spectral classification is K2 V. See Griffin's own paper for a discussion. System447Orbit1End System448Orbit1Begin Popper's observations supersede those of J. Sahade and C.U. Cesco (Astrophys. J., 100, 374, 1944) which were of too low a dispersion for those authors to be able to resolve the two components. Both components have Ca II emission in their spectra. The spectral types assigned correspond to the colours of the components. It is possible to estimate only the combined spectral type directly (between K0 and K2). Popper also gives the results of BV observations. He finds i=81 deg and that the two stars are approximately equal in light. He assumed a circular orbit, and the epoch is the time of primary minimum. System448Orbit1End System449Orbit1Begin The minimum magnitude is estimated from the light-curve. The orbit is assumed circular and the epoch is the time of primary minimum. R.M. Williamon (Astron. J., 81, 1134, 1976) published UBV light-curves and an analysis (later revised by M. Mezzetti et al. (Astron. Astrophys. Supp., 42, 15, 1980). Lacy adopted Williamon's own solution, which gives an orbital inclination very close to 83 deg and a visual magnitude difference of 0.3m. The minimum magnitude given is estimated from Williamon's plot. System449Orbit1End System450Orbit1Begin System450Orbit1End System451Orbit1Begin This is a symbiotic star whose light variation is not easy to interpret. The principal spectrum is that of a late-type giant (only approximately M5) with emission lines of H, He II and Fe II, presumably arising from the region around a hot component, estimated by some investigators as early F or late A spectral type. The period is uncertain within several days, the epoch is time of maximum light. The orbit is assumed circular. The elements, derived from the emission-line velocities, are described as tentative by Iijima himself. His model predicts a primary eclipse at the time when maximum light is observed. The binary nature of this object is not yet conclusively demonstrated. System451Orbit1End System452Orbit1Begin A mercury-manganese star that has long been suspected to be a spectroscopic binary; G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976) also believed the velocity to be variable. Only an approximate period can be derived, however, and the elements are correspondingly uncertain. The star is the brightest component of A.D.S. 6095; companions 10.5m and 10.2m at 1" and 16.6", respectively. System452Orbit1End System453Orbit1Begin The spectral types are taken from M.J. Plavec and J.J. Dobias (Astron. J., 93, 440, 1987) and are obtained by their technique of fitting model atmospheres. The value of K2 is from D.M. Popper (Publ. Astron. Soc. Pacific, 94, 945, 1982) and is preliminary. Plavec and Dobias report that observations now in progress will probably lead to a lower value of K1 than McKellar found. Meanwhile, McKellar's study is still to be preferred to the earlier one by S. Gaposchkin (Astrophys. J., 104, 383, 1946). Emission in the spectrum was first discovered by A.B. Wyse (Lick Obs. Bull., 17, 37, 1934). It arises from a typical Algol-type disk or ring, and the relatively long orbital period made it possible for McKellar to study the ring with some degree of time-resolution. This ring complicates photometric analyses. Recent such discussions include those by M. Kumsishvili (Bulletin Abastumani Obs., No. 55, 89, 1982), D.S. Hall et al. (Acta Astron., 32, 411, 1982) and I.B. Pustylnik and L. Einasto (Astrophys. Space Sci., 105, 259, 1984). They agree to the extent that they place the orbital inclination between 80 deg and 90 deg and the fractional luminosity of the primary star (in V) between 0.8 and 0.9. System453Orbit1End System454Orbit1Begin New observations by Abt and Levy confirm and improve the orbital elements derived by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 226, 1925) and (from the same observations) by Luyten. The epoch is T0. Petrie(II) found Delta m=0.53. The star is the brightest member of A.D.S. 6089: companions 9.5m at 42.9" and 10.5m at 145.9". System454Orbit1End System455Orbit1Begin One period (389 d) has been added to the time of periastron passage given by Christie to give a Julian Date after 2,400,000. System455Orbit1End System456Orbit1Begin Both components of this binary are late-type giants. From one Reticon spectrogram, no difference in spectral type was found between the two components. From that and from the radial-velocity traces observed with his spectrometer, Griffin estimates Delta m=0.71. The star is the brightest member of A.D.S. 6119. The 13.6m companion at 13" shares the proper motion of 65 Gem. One measure of the radial velocity by Griffin is close to but not identical with the systemic velocity of the spectroscopic pair. Nevertheless, Griffin believes that the two objects are probably physically associated. System456Orbit1End System457Orbit1Begin System457Orbit1End System458Orbit1Begin Earlier investigation by J. Lunt (Astrophys. J., 44, 261, 1916). Results are in good agreement with those presented here. D.S. Evans (Mon. Notes Astron. Soc. South Africa, 16, 4, 1957) finds that P=257.5d, but the other elements are not affected by this change. According to I.D.S. there is a 9.4m companion at 22.3". System458Orbit1End System459Orbit1Begin The epoch is superior conjunction of the secondary star. The orbit was assumed to be circular. The elements are very approximate: K1 is given as between 60 km/s and 90 km/s, no value at all is given for V0. The elements depend on measures of the emission lines in the spectrum of this cataclysmic variable. System459Orbit1End System460Orbit1Begin Spectroscopic coverage of this faint system remains quite inadequate as anything more than a rough indication of the velocity variation. New photoelectric light-curves in B and V by P. Broglia and F. Marin (Astron. Astrophys., 34, 89, 1974) have greatly improved our knowledge of the system. They find i=86 deg and the brighter star gives 0.92 of the total light in V. They identify the primary as a deg Sct star. A revised calculation by M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 265, 1980) led to a slightly lower fractional luminosity. These investigators suggest spectral types of A9 IV and K0. The epoch is the time of primary minimum but the period is variable. System460Orbit1End System461Orbit1Begin The fainter component of alpha Gem (the magnitude given applies to the combined light of alpha 1 and alpha 2). The spectrum is A1 from the K line and A5 from the metallic lines. Amongst the earlier investigations the most important are those of H.D. Curtis (Lick Obs. Bull., 4, 55, 1906) and D.A. Barlow (Publ. Dom. Obs.,9, 149, 1929). References to earlier work will be found in these papers. Barlow's value of K1 is lower and of e is higher than the Lick values. Vinter-Hansen gives e=0.002, Lucy & Sweeney adopt a circular orbit. Together with the next two entries in the Catalogue this star forms A.D.S. 6175 which is known to form a physical system. The I.D.S. also lists a fourth companion at 204.4". System461Orbit1End System462Orbit1Begin The same references given to earlier work on the immediately preceding system apply to this one. All investigations give results in good agreement. System462Orbit1End System463Orbit1Begin The observations by Bopp supersede earlier investigations by A.H. Joy and R.F. Sanford (Astrophys. J., 64, 250, 1926), O. Struve et al. (Astrophys. J., 112, 216, 1950) and O. Struve and V. Zebergs (Astrophys. J., 130, 783, 1959). A new discussion of the velocity-curve, based on measures of the emission lines, has been published by K. Kodaira and K. Ichimura (Publ. Astron. Soc. Japan, 32, 451, 1980). Their results agree well with Bopp's, which have the smaller formal errors. The elements given here are also based on emission-line measures: velocities derived from the absorption lines give a reversed mass-ratio and a different V0. The epoch is the time of mid-eclipse. The star then eclipsed is somewhat conventionally defined as the primary, the two minima being almost equal. Although Bopp and Struve and Zebergs refer to their epochs as the same as that adopted by H. van Gent (Bull. Astron. Inst. Netherl., 6, 99, 1931) they differ from him by an integral number of half periods. The period may be lengthening. Flares have been observed (T.J. Moffett and B.W. Bopp, Astrophys. J., 168, L117, 1971). There is both spectroscopic and photometric evidence for flares and G. Ferland and B.W. Bopp (Publ. Astron. Soc. Pacific, 88, 451, 1980) discuss the distribution of emitting regions over the surfaces of the stars. Photometric study is made difficult by the light from nearby (and physically associated) alpha Gem. Recent discussions of the light-curve have been published by E. Budding (Tokyo Astron. Bull, 2nd Series, No. 240, 1975) and K.-C. Leung and D.P. Schneider (Astron. J., 83, 618, 1978). Both agree on an orbital inclination close to 86 deg but whereas Budding finds the two components virtually equal in light, Leung and Schneider find Delta m(bol.)=0.35. The magnitudes given are Budding's out-of-eclipse measure, combined with a graphical estimate of the depth of minimum. System463Orbit1End System464Orbit1Begin Radial-velocity observations by O. Struve (Astrophys. J., 112, 184, 1950) appeared to require an orbital period of 9.7d, while photometric observations by E. Hertzsprung (Bull. Astron. Inst. Netherl., 4, 154, 1928) and M. Huruhata et al. (Ann. Tokyo Obs. 2nd Series, 5, 31, 1957) gave a W UMa light-curve with a period close to 0.58d. Van Houten has resolved the problem by showing that both Struve's observations and those of Huruhata et al. can be satisfied by the period given in the Catalogue. The epoch is the time of primary minimum, and the orbital elements are estimates from a plot of the velocity curve. G. Giuricin and F. Mardirossian (Astron. Astrophys., 99, 185, 1981) have analyzed the light-curves obtained by Huruhata et al. and find an orbital inclination between 75 deg and 80 deg and a fractional luminosity for the primary star (in yellow light) of 0.77. System464Orbit1End System465Orbit1Begin The system resembles VV Cep. The shell spectrum observed between 1947 and 1949, which reappeared (A.P. Cowley, Publ. Astron. Soc. Pacific, 83, 213, 1971) may be produced by an atmospheric eclipse. Observations of the UV spectrum have been discussed by A. Altamore, A. Giangrande and R. Viotti (Astron. Astrophys. Supp., 49, 511, 1982). System465Orbit1End System466Orbit1Begin Although no luminosity classification has been made of the spectrum, Griffin considers that the star is likely to be a giant. The orbit was assumed circular and the epoch is T0. System466Orbit1End System467Orbit1Begin Only the period (40.65y) has been assumed from the visual orbit. The time of periastron passage is 1927.20. Fletcher has combined modern Victoria observations with the older ones of H.S. Jones (Mon. Not. Roy. Astron. Soc., 88, 403, 1928) and those used by K.Aa. Strand (Astrophys. J., 113, 1, 1951) in his definitive study of the visual orbit. The quantity of radial-velocity data now available has made it possible to derive these elements without making use of the elements derived from visual observations. The results are in very good agreement with those obtained by Strand (who also found i=35.7 deg). The system is A.D.S. 6251: three other components (besides the white dwarf) are listed in I.D.S. Reference: J.M.Fletcher,,,, (Unpublished) System467Orbit1End System468Orbit1Begin Petrie(II) found Delta m=0.36. System468Orbit1End System469Orbit1Begin This star is the first of a series of early-type binaries discovered by Gieseking. Because all velocity measurements were made by objective prism, the systemic velocities given for all these objects are relative velocities. To convert them to absolute velocities, it is necessary to consult the same author's catalogue (Astron. Astrophys. Supp., 41, 245, 1980) to see which stars in the field were used as standards. The orbits were usually assumed to be circular and the epoch is the time of maximum velocity. System469Orbit1End System470Orbit1Begin Luyten's recomputation of the elements with an assumed circular orbit (epoch T0) is preferred to W.E. Harper's original solution (Publ. Dom. Obs., 1, 265, 1911) because Harper had to fix the value of T. Later, he revised the period to 19.603d (Publ. Dom. Astrophys. Obs., 6, 224, 1935). The star is now considered a non-eclipsing member of the RS CVn group and varies by nearly 0.2m in a period close to, but not identical with, the orbital period. Extensive photometric observations have been discussed and published by R.E. Fried et al. (Astrophys. Space Sci., 93, 305, 1983). The spectrum at H-alpha has been observed by S.E. Smith and B.W. Bopp (Astrophys. Letters, 22, 127, 1982) and by K.G. Strassmeier, S. Weichinger and A. Hanslmeier (Inf. Bull. Var. Stars, No. 2937, 1986). Variations in the spectrum have been noted by Z. Eker (Bull. Am. Astron. Soc., 17, 588, 1985). The star is a possible radio source (S.R. Spangler, F.N. Owen and R.A. Hulse, Astron. J., 82, 989, 1977) and a known X-ray source (J.P. Pye and I.M. McHardy, Bull. Am. Astron. Soc., 12, 855, 1980). There is a 10.8m `companion' at over 180" separation. System470Orbit1End System471Orbit1Begin Epoch is T0. Intensities of spectral lines seem to vary with phase. According to S. Gaposchkin (Ann. Harv. Coll. Obs., 113, No. 2, 1953) the light-curve implies Delta m=1.3. System471Orbit1End System472Orbit1Begin These elements supersede provisional elements previously published by Neubauer (Publ. Astron. Soc. Pacific, 44, 254, 1932). Estimation of quality of the orbit is difficult because of the little information given by the authors. The velocities were obtained with the Mills three-prism spectrograph, and it seems likely, therefore, that the orbit is above average quality. System472Orbit1End System473Orbit1Begin Although the system has a high velocity, Griffin comments that the metal lines and CN bands are not obviously weak for the spectral class. The star is designated as an occultation double in the Bright Star Catalogue and Griffin calls attention to the possibility of detecting the secondary during occultations. System473Orbit1End System474Orbit1Begin See note for HD 61926 System474Orbit1End System475Orbit1Begin Values of e and omega were assumed in accordance with the light-curve and the epoch is the time of mid-eclipse (the two minima are almost equal in depth). The spectroscopic elements are undoubtedly well determined; analysis of the light-curve is made difficult by the intrinsic variability of both components. This variability is periodic but the period is not related to that of the orbit. Despite the problems created by the variation, consistent elements have been derived. The stars are nearly equal both in surface brightness and in luminosity, the less massive component being a few percent less luminous. The orbital inclination is close to 83 deg. The star is the fainter component of A.D.S. 6348: the brighter (H.D. 2864) is 6.07m at 17". Vaz and Andersen believe the pair to be optical only. System475Orbit1End System476Orbit1Begin These elements supersede preliminary ones presented by V.S. Niemela, (I.A.U. Colloq. No. 59, p. 307, 1981). The orbit is assumed circular and the epoch is the time of inferior conjunction of the Wolf-Rayet star. The upper line of elements refers to the Wolf-Rayet component. Velocities derived for this star are from measures of the C III-C IV emission line at lambda 4652 (of uncertain rest wavelength) and the O VI emission line at lambda 3811. System476Orbit1End System477Orbit1Begin See note for HD 61926 System477Orbit1End System478Orbit1Begin Abt and Levy find a much lower value of K1 than did O. Struve (Astrophys. J., 58, 141, 1923). They believe that the spectrum may be a blend of those of both components of this visual binary (A.D.S. 6420): the secondary is about 0.6m fainter than the primary. The value of the magnitude given in the Catalogue corresponds to the combined light of both components. The period, time of periastron passage, longitude of periastron, and eccentricity are all taken from the visual orbit by R.v.d.R. Woolley and L.S.T. Symms (Mon. Not. Roy. Astron. Soc., 97, 438, 1937) and are well determined. The e classification simply reflects the doubt whether K1 has been reliably determined at all. System478Orbit1End System479Orbit1Begin The velocity curve of the primary star is derived from measures of the helium lines. D.M. Popper (Publ. Astron. Soc. Pacific, 79, 493, 1967) has obtained spectrograms at a higher dispersion than Deutsch used and has been able to measure the K line of the secondary spectrum free of blending with that of the primary. The value given for K2 is his value rather than Deutsch's value of 125 km/s (which Deutsch himself recognized might be too low). The system is thus removed from the `class' of R CMa systems. M. Kitamura (Astrophys. Space Sci., 2, 448, 1968) has obtained UBV light-curves from which he finds i=89.5 deg and the fractional luminosity of the brighter star (in V) is 0.82. He encounters some difficulties in his solution, however. B. Cester et al. (Astron. Astrophys., 61, 469, 1977), from the same observations, derived a fractional luminosity of 0.93. They give photometric `spectral types' of B5 V and F0 III and find problems in reconciling the masses, as deduced from the spectrographic data, with the luminosities. System479Orbit1End System480Orbit1Begin The emission lines in the spectrum of this `X-ray nova' are very broad and the velocity measures extremely uncertain. The uncertainty in K1 is nearly 50 percent of its value. Probably the observed velocities are not entirely orbital in origin. The light of the object is variable and the light-curve resembles that of an eclipsing binary. The epoch is the time of primary minimum. System480Orbit1End System481Orbit1Begin New observations by Parsons indicate that the period adopted by W.H. Christie (Astrophys. J., 83, 433, 1936) was a little too long. The new elements are not much different, but probably represent an improvement. System481Orbit1End System482Orbit1Begin The light of the star varies by less than 0.1m, as was first shown by E.H. Olsen. Probably the system is an ellipsoidal variable. The orbit was assumed circular and the epoch is primary minimum. Preliminary elements were presented by Haefner in Inf. Bull. Var. Stars, No. 2242, 1982. System482Orbit1End System483Orbit1Begin Smak's observations and results supersede all computations of elements based on the observations by R.P. Kraft (Astrophys. J., 135, 408, 1962). The values given for K1 and V0 are means derived from measures of all lines. Values derived from measures of individual lines differ quite considerably from these, but have large uncertainties. The value of K2 has been taken from R.A. Wade (Astrophys. J., 246, 215, 1981). The spectral classification is by J. Stauffer, H. Spinrad and J. Thorstensen (Publ. Astron. Soc. Pacific, 91, 59, 1979). Wade found that V0 for the secondary component is about +84 km/s. Smak adopted a circular orbit and the epoch is the time of primary minimum. Wade found a small eccentricity fitted observations of the secondary better, but it is not statistically significant and its introduction does not appreciably change the values he found for V0 and K2. The range of light variation is itself variable. The V magnitudes given in the text are the extreme values given by W. Krzeminski (Astrophys. J., 142, 1051, 1965). High-speed photometry by B. Warner and R.E. Nather (Mon. Not. Roy. Astron. Soc., 152, 219, 1971) showed that the hot spot on the accretion ring is a major contributor to the total light. Wade (and others) showed that spectroscopic conjunction does not coincide with primary minimum, thus demonstrating that the hot spot is displaced from the line joining the centres of the two components. The nature of the light-curve precludes accurate analysis; Smak estimates i=67 deg +/-8 deg. In the infrared, the light of the late-type component predominates and infrared light-curves have been studied by R.J. Panek and J.A. Eaton (Astrophys. J., 258, 572, 1982) and G. Berriman et al. (Mon. Not. Roy. Astron. Soc., 204, 1105, 1983) who confirm that the late-type component fills its Roche lobe. Spectroscopy in the UV is reported by R.J. Panek and A.V. Holm (Astrophys. J., 277, 700, 1984) and P. Henry et al. (Astrophys. J., 197, L117, 1975) who also discuss the soft X-ray flux. For studies of the structure and properties of the accretion disk, see B. Paczynski and A. Schwarzenberg-Czerny (Acta Astron., 30, 127, 1980) and J. Smak (Acta Astron., 34, 93, 1984). System483Orbit1End System484Orbit1Begin Epoch is an arbitrary zero of phase: maximum positive velocity (T0) is about 1 d later. Blaauw and van Albada suspect changes in the shape of the velocity-curve arising, possibly, from apsidal motion. System484Orbit1End System485Orbit1Begin The V magnitude is an estimate. Griffin adopted a circular orbit (the epoch is T0 ) while admitting that a small eccentricity might exist. He draws attention to the relatively short period for a system containing a giant and suggests that photometry might show an intrinsic variation in the star's light. System485Orbit1End System486Orbit1Begin The computed solution by Lucy & Sweeney is preferred to the graphical one from the same observations by Y.C. Chang (Astrophys. J., 106, 308, 1947). The epoch is T0. According to C. Yuin (Astrophys. J., 106, 303, 1947) the orbital inclination is 78.7 deg. System486Orbit1End System487Orbit1Begin The epoch is T0 and the G-type star is the more massive of the pair. A circular orbit was adopted. The light-curve is variable, as are the depths of minima. C.R. Lynds (Astrophys. J., 126, 81, 1957) found the A-type component to be intrinsically variable. This has been confirmed by F. Scaltriti (Mem. Soc. Astron. Ital., 44, 387, 1973) who believes the variation is of the deg Sct type. Lynds also found i=83.6deg (Publ. Astron. Soc. Pacific, 68, 339, 1956). There are earlier studies of the system by S. Gaposchkin (Astrophys. J., 105, 258, 1947) and J. Sahade (Astrophys. J., 111, 194, 1950). System487Orbit1End System488Orbit1Begin Petrie(I) found Delta m=0.32. System488Orbit1End System489Orbit1Begin The new results by Andersen et al. supersede those obtained by H.O. Frieboes (Astrophys. J., 135, 762, 1962), D.M. Popper (Astrophys. J., 97, 400, 1943) and A.C. Maury (Pop. Astron., 29, 22, 1921). Their photometric analysis likewise probably supersedes earlier ones by D.P. Schneider, J.J. Darland and K.-C. Leung (Astron. J., 84, 236, 1979), B. Cester et al. (Astron. Astrophys., 61, 275 and 469, 1977) and J.A. Eaton (Acta Astron., 28, 63, 1978). The orbit was assumed circular in agreement with the photometric evidence; the epoch is the time of primary minimum. The elements given are derived from measures of the helium lines only and have been corrected for the effects of tidal distortion. Andersen et al. believe the system to be semi-detached. They deduce an orbital inclination of 79 deg and find a difference in visual magnitudes of 1.34m. They show that the period varies but cast doubt on the previously assumed existence of circumstellar matter in the system. For discussions of the UV spectrum see D.G. York, B. Flannery and J. Bahcall (Astrophys. J., 210, 143, 1976) and R.H. Koch et al. (Publ. Astron. Soc. Pacific, 93, 621, 1981). Four companions are listed in I.D.S.: the closest is 11.5m at 6.8". System489Orbit1End System490Orbit1Begin The new observations supersede Popper's own older ones (Publ. Astron. Soc. Pacific, 68, 131, 1956). A circular orbit was assumed, and the epoch is the time of primary minimum. The hydrogen lines are too strong for the assigned spectral type, H-delta being more so than H-gamma. The hydrogen lines strengthen during primary minimum, indicating that the companion has an earlier spectral type rather than a later one -- yet the radial-velocity curve indicates that the visible component is eclipsed at primary minimum. Popper has measured the light of the system outside eclipse, but not within it. System490Orbit1End System491Orbit1Begin Epoch is T0 even though a small orbital eccentricity has been retained. Two faint and distant companions are listed in I.D.S.: 12.0m at 60.1" and 11.0m at 78.6". System491Orbit1End System492Orbit1Begin See note for HD 61936. A period of 0.8604d is also possible and more observations are needed to decide. The Durchmusterung number is from the C.P.D. System492Orbit1End System493Orbit1Begin Harper made arbitrary corrections to the velocities of his normal points in order to compensate for blending effects. Petrie(II) found Delta m=0.32. System493Orbit1End System494Orbit1Begin R.E. Wilson (Astrophys. J., 234, 1054, 1979) suggests, from a discussion of the photometric observations that the eccentricity is spurious. Light-curves were obtained both by Vetesnik and by J.K. Gleim (Astron. J., 72, 493, 1967) and have been re-analyzed by F. Predolin, G. Giuricin and F. Mardirossian (Inf. Bull. Var. Stars, No. 1801, 1980) and J. Kaluzny (Acta Astron., 35, 327, 1985). The light-curve is variable and no definitive solution has yet been made. The orbital inclination is probably around 80 deg, and the brighter component gives at least 0.9 of the (yellow) light. System494Orbit1End System495Orbit1Begin See note for HD 61936. The elements given here supersede preliminary results by the same author (Publ. Astron. Soc. Pacific, 90, 204, 1978). System495Orbit1End System496Orbit1Begin See note for HD 61936. A preliminary discussion of this system is also found in the reference given in the preceding note. The period is still uncertain. System496Orbit1End System497Orbit1Begin This star is a dwarf Cepheid and individual points on the velocity-curve are mean values for a pulsational cycle. The spectral type of the primary is described by Bardin and Imbert as consistent with either F0 IV-V or F2 II-III and the secondary is certainly cooler than F2 V. System497Orbit1End System498Orbit1Begin This study of this cataclysmic binary supersedes preliminary results obtained by two of the same authors (R.A. Wade and J.B. Oke, Bull. Am. Astron. Soc., 14, 880, 1982). The magnitude given is the mean quiescent magnitude: the object can be up to three magnitudes brighter. Velocities are derived from measures of the emission lines and the epoch (in an assumed circular orbit) is inferior conjunction of the emission-line source. The values given for the elements are those adopted by the authors. Different lines give quite widely differing values -- especially for V0. System498Orbit1End System499Orbit1Begin This star has long been suspected to be a binary but these are the first orbital elements to be derived. The spectral classification is by Hernandez and Sahade; other investigators have called the star a subgiant or even a main-sequence object. The elements given are from all the observations made by Hernandez and Sahade. There is some evidence for changes in the shape of the velocity-curve (e and omega) with time. Four visual companions are listed in I.D.S., the principal one, of course, being the Wolf-Rayet star gamma 2 Vel. The physical association of this pair is not clearly proven, but Hernandez and Sahade demonstrate the similarity of the space motions of the two stars (within the observational uncertainties) and suggest that a relationship is possible. System499Orbit1End System500Orbit1Begin Three orbital studies have been published since the Seventh Catalogue; the other two are by C.D. Pike, D.J. Stickland and A.J. Willis (Observatory, 103, 154, 1983) and A.F.J. Moffat et al. (Astron. J., 91, 1386, 1986). Considering the nature of the spectrum, the agreement between these is not bad, and all differ from the only previous set of elements by K.S. Ganesh and M.K.V. Bappu (Kodaikanal Obs. Bull., Series A, 183, 177, 1968). The upper line of elements is derived from the absorption lines of the O9 star. Pike et al. favour a slightly longer period (78.519d). The emission lines in the Wolf-Rayet spectrum give, of course, discordant values of V0. Since no eclipses are observed, an upper limit for the orbital inclination is around 70 deg. For a discussion of IUE observations of this star, see A.J. Willis et al., First Year of IUE, (University College, London, 1979). See preceding note for information on visual companions. System500Orbit1End System501Orbit1Begin New observations by Stickland and Weatherby do not fit the period derived by H.A. Abt and M.S. Snowden (Astrophys. J., 25, 137, 1973). There is still some doubt about the period, one near 475d also being possible, but the value given in the Catalogue is preferred. The star was considered as an Si, Cr object by Abt and Snowden, Stickland and Weatherby suspect that it is an Hg, Mn star. System501Orbit1End System502Orbit1Begin The secondary spectrum was thought to be visible on one spectrogram. If it is, the mass-ratio would appear to be 0.81. In I.D.S. an 8.1m companion is listed at 6".1. System502Orbit1End System503Orbit1Begin The magnitude is an estimate. Griffin calls attention to the mass-function, large for a system showing only one spectrum, and suggests that the secondary component itself is a short-period binary, perhaps containing two main-sequence stars of type about F4. System503Orbit1End System504Orbit1Begin The recomputation by Lucy & Sweeney based on observations by O. Struve (Astrophys. J., 104, 253, 1946) has been preferred to Struve's original solution (e=0.1) because a photoelectric (BV) light- curve (K.T. Johansen et al., Astron. Astrophys., 11, 20, 1971) shows e cos omega=0. The epoch is T0, and the orbit was assumed circular after a preliminary solution gave e=0.0. The two stars are nearly equal in size, but the primary gives 0.91 of the total light in V. The orbital inclination is about 89.7 deg. A new analysis of these observations by M. Mezzetti et al. gives very similar results. The depth of eclipse in V is just over 2.5m, but unfortunately the maximum and minimum V magnitudes cannot be deduced from the data given by Johansen et al.. In view of the excellent light-curve now available, the system would be worth re-observing spectroscopically. System504Orbit1End System505Orbit1Begin The magnitudes given are approximate and the star spends most of the time at the fainter magnitude. No epoch is given; the orbit is assumed circular. The values of K1 and V0 are derived from measures of the core of the H-alpha emission line. System505Orbit1End System506Orbit1Begin According to I.D.S. there is a 9.5m companion at 51.1". System506Orbit1End System507Orbit1Begin A few old Mount Wilson measures give velocities above the mean curve derived from recent CORAVEL observations. The authors believe this cannot be accounted for by systematic errors between observatories and suggest that V0 varies. System507Orbit1End System508Orbit1Begin The new observations add little to those of G.H. Herbig (Astrophys. J., 132, 76, 1960) but show that the elements deduced depend on the lines measured and may vary with time. The elements given in the Catalogue are based on measures of the peak of the He II emission. The orbit is assumed circular and the epoch is a photometric one (approximately maximum brightness) taken from the work of M.F. Walker (Mitt. Sternw. Budapest, 57, 1, 1965). The magnitudes given are an approximate indication of the range of the highly variable light-curve. Photometry of the system has been discussed by D.A. Allen and A.M. Cherepashchuk (Mon. Not. Roy. Astron. Soc., 201, 521, 1982) and P. Szkody, J.A. Bailey and J.H. Hough (ibid., 203, 749, 1983). The former investigators find that when the star is quiescent, the variation is caused primarily by the ellipticity of the M-type dwarf and they estimate that the orbital inclination is between 50 deg and 70 deg. A detailed model is discussed by J. Liebert et al. (Astrophys. J., 225, 201, 1978) and spectrophotometric observations are reported and interpreted by D.T. Wickramasinghe and N. Visvanathan (Mon. Not. Roy. Astron. Soc., 191, 589, 1980). System508Orbit1End System509Orbit1Begin This star (from the Cape Photographic Durchmusterung) was recognized as a cataclysmic variable by R.F. Garrison et al. (Astrophys. J., 276, L13, 1984). The magnitude given is the mean of their published results; the star flickers over a range of 0.1m and shows variations of about 0.5m over several years. Garrison et al. used this system, at present the brightest known cataclysmic variable, to estimate the space density of such stars. Two studies have been published by the authors cited in the Catalogue; the other is in Mon. Not. Roy. Astron. Soc., 204, 35P, 1983. A circular orbit is assumed and the epoch is the time of inferior conjunction of the emission-line source. The results are described as preliminary by the authors themselves. They estimate the orbital inclination at 63 deg. A brief account of the UV spectrum was published by H. Bohnhardt et al., I.A.U. Circ., No. 3749, 1982. System509Orbit1End System510Orbit1Begin This is another cataclysmic variable in which caution is needed in the interpretation of the `orbital elements'. The value of K1=193 km/s is derived from late-type absorption lines in the spectrum. That of K2 is derived from emission lines which, at least partially, arise from the disk surrounding the white dwarf. A circular orbit has been assumed, the epoch given is the time of spectroscopic conjunction with the red star in front. The two velocity curves are 180 deg out of phase. E.L. Robinson (Astrophys. J., 186, 347, 1973) has also obtained spectrograms of the red region. From the H-alpha emission he has derived K2=137 km/s, V0=45 km/s, and assumed the other elements were as derived by Kraft et al.. He found evidence that the system is losing mass. Robinson has also published high-speed photometry of the system (Astrophys. J., 180, 121, 1973). Although B. Warner and R.E. Nather (Sky Telesc., 43, 82, 1973) earlier reported grazing eclipses of the hot spot in this system, Robinson found no evidence for them. Kraft et al. estimate the orbital inclination to be in the range 50 deg to 60 deg. The B magnitudes given in the Catalogue are derived from data in their paper. A theoretical model for the system has been proposed by B.P. Flannery (Astrophys. J., 201, 661, 1975). A spectrophotometric study of this system has been published by A.L. Kiplinger (Astrophys. J., 236, 839, 1980). System510Orbit1End System511Orbit1Begin This is one of the few pulsars in a binary system with a known orbit -- an orbit of very different characteristics from those of the first known member of the class, PSR 1913+16. The epoch is an arbitrary reference epoch. The measured quantity, of course, is not radial velocity but pulsar period which is determined very accurately. From its variations, a sin i can be deduced. A compete orbital period has not yet been observed. No magnitude or spectral type are available, and V0 cannot be determined. A circular orbit was assumed. System511Orbit1End System512Orbit1Begin Lucy & Sweeney adopt a circular orbit. System512Orbit1End System513Orbit1Begin The epoch is the time of primary minimum (which is only slightly deeper than the secondary). The small eccentricity is in agreement with that found photometrically and the system displays apsidal motion in a period of approximately 3,200 years. The two stars are nearly equal and the orbital inclination is close to 88 deg. Both spectroscopic and photometric observations are affected by a visual companion. According to I.D.S. this is 1.1m fainter than the eclipsing pair and separated by 0.3". Andersen et al. believe the companion to be fainter and probably to be a spectroscopic binary itself. System513Orbit1End System514Orbit1Begin These systems compose A.D.S. 6828. The orbital period of the visual pair is 53y and its major semi-axis is 0.32". Each component is a spectroscopic binary. Fekel has also detected the secondary component of the 2.5-day pair (Bull. Am. Astron. Soc., 10, 660, 1978 and private communication) and believes its mass-ratio to be similar to that of the 6-day pair. Although Fekel has not yet published a complete study of this interesting multiple system, he has extensive data. He has published slightly different values for the eccentricities (Astrophys. J., 246, 879, 1981) and argues (Bull. Am. Astron. Soc., loc. cit.) that none of the orbits is coplanar. The eccentricity of the 6-day orbit is now found to be negligibly small and the epoch is T0. Orbital elements have been published by G.A. Bakos (J. Roy. Astron. Soc. Can., 79, 119, 1985) whose results are in general agreement with Fekel's except for values of V0 (which may be partly affected by systematic errors) and a somewhat larger eccentricity for the 6-day pair. Bakos has also shown that the 2.5-day pair is an eclipsing binary. He derives an orbital inclination of 86 deg and estimates that the primary gives 0.89 of the light in V. There is a faint companion (11.5m) at about 18" listed in I.D.S. and Fekel believes it to be physically associated with the quadruple system. Reference: F.C.Fekel,,,, (Unpublished) System514Orbit1End System515Orbit1Begin These systems compose A.D.S. 6828. The orbital period of the visual pair is 53y and its major semi-axis is 0.32". Each component is a spectroscopic binary. Fekel has also detected the secondary component of the 2.5-day pair (Bull. Am. Astron. Soc., 10, 660, 1978 and private communication) and believes its mass-ratio to be similar to that of the 6-day pair. Although Fekel has not yet published a complete study of this interesting multiple system, he has extensive data. He has published slightly different values for the eccentricities (Astrophys. J., 246, 879, 1981) and argues (Bull. Am. Astron. Soc., loc. cit.) that none of the orbits is coplanar. The eccentricity of the 6-day orbit is now found to be negligibly small and the epoch is T0. Orbital elements have been published by G.A. Bakos (J. Roy. Astron. Soc. Can., 79, 119, 1985) whose results are in general agreement with Fekel's except for values of V0 (which may be partly affected by systematic errors) and a somewhat larger eccentricity for the 6-day pair. Bakos has also shown that the 2.5-day pair is an eclipsing binary. He derives an orbital inclination of 86 deg and estimates that the primary gives 0.89 of the light in V. There is a faint companion (11.5m) at about 18" listed in I.D.S. and Fekel believes it to be physically associated with the quadruple system. Reference: F.C.Fekel,,,, (Unpublished) System515Orbit1End System516Orbit1Begin Brighter component of A.D.S. 6872: companion 9.8m at 1.8". System516Orbit1End System517Orbit1Begin There is obviously a misprint in the value of T as given by Stickland et al. The correct value is presumably either 2,430,730.51 or 2,443,730.51, the latter being the more likely. System517Orbit1End System518Orbit1Begin Popper's elements are in general agreement with those found by O. Struve (Astrophys. J., 102, 74, 1945). The epoch is T0. Slightly different values of V0 are found for each component. Several photometric investigations have been made (R.L. Walker, Astron. J., 75, 720, 1970, D.B. Wood, ibid., 76, 701, 1970, T.D. Padalia and R.K. Srivastava, Astrophys. Space Sci., 35, 249, 1975 and B. Cester et al., Astron. Astrophys. Supp., 32, 351, 1978). All agree that the orbital inclination is close to 89 deg. Values obtained for the fractional luminosity depend strongly on whether the primary eclipse is taken to be an occultation or transit. Popper (Astrophys. Space Sci., 45, 391, 1976) has shown that only the latter leads to a luminosity ratio in accord with the spectroscopic evidence. Cester et al., who adopt the transit hypothesis, found a fractional luminosity of 0.64 (in V) for the primary component. System518Orbit1End System519Orbit1Begin A circular orbit was assumed and the epoch is T0. The two stars are approximately equal in photographic (B) light and the spectrum is composite outside eclipse. D.M. Popper (Publ. Astron. Soc. Pacific, 60, 248, 1948) classified the secondary spectrum as A3 III-V: Wesselink's classification is based on UBV measures in totality and out of eclipse. He finds that the B star is 1.12m fainter than the K star in V, but 1.4m brighter than it in U. Primary eclipse is the total eclipse of the B star by the K giant. Wesselink assumed i=90 deg to derive relative radii for the two stars, but no complete photoelectric light-curve of the system has been published. Identification of the star is from the Cordoba Durchmusterung. System519Orbit1End System520Orbit1Begin Epoch is T0, based on an early time of minimum. All elements are very approximate. Sahade describes the two spectra as `of practically the same intensity'. Modern analysis of BV light-curves (D.A.H. Buckley, Astrophys. Space Sci., 99, 191, 1984) confirms that, giving a fractional luminosity in V for the primary component of 0.52 and an orbital inclination close to 88 deg. System520Orbit1End System521Orbit1Begin This is a cataclysmic variable and a known X-ray source. The magnitude is approximate. Very few details are given of the orbital solution. In particular, no epoch is given and V0 had to be inferred from a plot of the velocity-curve. The value of K1 is derived from measures of the emission-line wings and is also approximate. System521Orbit1End System522Orbit1Begin Investigation of this star was described as a `preliminary study' by Thackeray himself, and in view of the fairly large scatter of the observations the orbit has been classified as d. Thackeray commented on the complexity of the emission-line spectrum and compares the system with both beta Lyr and W Cru. There are variations in the light with the orbital period through a range of about 0.2m in V. Thackeray believed that the dominant cause of the variation is ellipticity of the components, but a partial eclipse of the region producing H emission may also be contributing. W. Strupat and C. Boehm report on some new spectra at 12 A/mm dispersion (Inf. Bull. Var. Stars, No. 2949, 1986). System522Orbit1End System523Orbit1Begin Brightest component of A.D.S. 6886: principal companion 7.2m at 10.3". System523Orbit1End System524Orbit1Begin Not known before the Palomar{Green survey, this object is presumably a cataclysmic variable and is possibly to be identified with the X-ray source 1H0832+488. The elements given are derived from measures of the bases of the emission lines. The secondary may be a dwarf of type about K5. Epoch is inferior conjunction of the emission-line source and the orbit was assumed circular. System524Orbit1End System525Orbit1Begin The elements obtained by Lucy & Sweeney have been preferred over those obtained from the same observations by O. Struve (Astrophys. J., 102, 74, 1945). The epoch given is T0. The only light curve available is one by J. Fetlaar (Bull. Astron. Inst. Netherl., 6, 29, 1930) from which he found i=89.5 deg and a light ratio of 0.33. System525Orbit1End System526Orbit1Begin The new results by Popper supersede his own earlier work (Astron. J., 62, 29, 1957; Publ. Astron. Soc. Pacific, 74, 129, 1962). The orbit was assumed circular and the epoch is the time of primary minimum. The spectral type of the secondary (cooler and less massive) star is derived from its UBV colours. Popper gives a photometric solution in which he derives an inclination of 87.5 deg and a light-ratio at quadratures of 0.78 in V (cooler.hotter star). P. Broglia and P. Conconi (Mem. Soc. Astron. Ital., 44, 87, 1973) obtain a very similar value for the inclination but make the fractional luminosity of the smaller star (in V) to be 0.37. B. Cester et al. (Astron. Astrophys., 61, 469, 1977), using the observations by Broglia and Conconi make the two stars nearly equal in luminosity, which appears contrary to the spectroscopic evidence. System526Orbit1End System527Orbit1Begin See note for HD 61936. Because most of the spectrograms of this object are only weakly exposed, Gieseking describes it as a suspected binary. System527Orbit1End System528Orbit1Begin Sanford reports `the two components have approximately the same brightness and spectral type'. The star is a member of Praesepe and is A.D.S. 6915 C; A is 6.9m at 45.2". System528Orbit1End System529Orbit1Begin This W UMa system has attracted much attention, partly because its membership of Praesepe helps to clarify the evolutionary status of contact systems. The observations by Whelan et al. supersede those by D.M. Popper (Astrophys. J., 108, 490, 1948). New observations have been published by B.J. McLean and R.W. Hilditch (Mon. Not. Roy. Astron. Soc., 203, 1, 1983) in the early development of cross-correlation methods for measuring this kind of spectrum. They find K1=96 km/s, K2=181 km/s. It seems to us, however, that the work of Whelan et al. should still be preferred, because of their better coverage of the velocity-curve, despite the potential of the newer method. The orbit was assumed circular and the epoch is the time of primary minimum. The minimum magnitude given in the Catalogue is an estimate from the plot of the V light-curve by Whelan et al. They find an orbital inclination of 63 deg and that the larger component gives 0.55 of the light of the system. Similar results for the orbital inclination have been obtained by A. Yamasaki (Astrophys. Space Sci., 77, 75, 1981) and R.W. Hilditch (Mon. Not. Roy. Astron. Soc., 196, 305, 1981). System529Orbit1End System530Orbit1Begin A standing reproach to spectroscopists has been removed with this publication of the first orbital elements for one of the longest-known eclipsing binaries. Fragmentary information about earlier observations had been available for some time, but inconsistencies in it were pointed out almost simultaneously by E.W. Weis (Observatory, 96, 9, 1976) and A.H. Batten (I.A.U. Symp. No. 73, p. 303, 1976). The spectral types are determined from photometric colours and spectrophotometry by P.B. Etzel and E.C. Olson (Astron. J., 90, 504, 1985) rather than from traditional spectral classification. The orbit was assumed circular and the epoch is the time of primary minimum. Values of V0 were determined separately for each component. Because the measures depend on different lines in different spectral regions, Popper and Tomkin do not consider the difference in V0 to be significant. A matching photometric study by Etzel and Olson has already been cited. They derive an orbital inclination close to 85 deg and a fractional luminosity in V for the primary star of 0.93. (Popper and Tomkin give Delta V=1.4m). Other recent analyses (M.I. Lavrov, Trudy Kazan Obs., 39, 42, 1973 and V.A. Caracatsanis, Astrophys. Space Sci., 47, 375, 1977) give similar results. Popper and Tomkin claim that the secondary has the lowest known stellar mass (0.18 MSol) derived directly from radial-velocity observations. There is a 10.8 m companion listed in I.D.S. at 76" separation. System530Orbit1End System531Orbit1Begin This object was recognized as a cataclysmic variable by N.E. Kurochkin and S.Yu. Shugarov (Astron. Tsirk., No. 1114, 1980) and the period and epoch (time of minimum) are taken from their paper. It is one of few cataclysmic variables in which the spectra of both components are measurable. The magnitude given is the approximate mean out-of-eclipse magnitude according to A. Yamasaki, A. Okazaki and M. Kitamura (Publ. Astron. Soc. Japan, 35, 423, 1983). Eclipses are about 1.5m deep in V. The variable may be associated with the X-ray source H 0850+13. The value of K for the white dwarf (upper line) is derived from emission lines of hydrogen and helium and one absorption line of helium. The measurable secondary lines include the G-band and lines of neutral metals. Schlegel et al. describe the spectrum as late G or early K, although photometric evidence might make it as late as K5. The orbit was assumed circular and the value of V0 is only approximately known. Schlegel et al. find a lower limit of 66 deg for the orbital inclination. A photometric study has also been published by A.V. Baidak and S.Yu. Shugarov (Astron. Zh., 63, 123, 1986). System531Orbit1End System532Orbit1Begin A.D.S. 6993, a well-known multiple system (it is at least quintuple). The magnitude refers to the combined light. This orbit is that of the visual pair AB (P=15.04y). Many other investigations of this star have been published. Those particularly concerned with the radial velocities of the components are: R.G. Aitken (Publ. Astron. Soc. Pacific, 24, 16, 1912); E. Slonin (Tashkent Bull., No. 5, 159, 1934); A. Abrami (Trieste Contr., No. 321, 1963). Radial velocities which confirm Adams' orbital elements have been published by A.B. Underhill (Publ. Dom. Astrophys. Obs., 12, 159, 1963). She suspected a secondary variation with a period of 70d. Adams also discussed the visual orbit, and found i=39.1 deg. The best visual orbit (adopted by W.S. Finsen and C.E. Worley Republic Obs. Circ., 7, 203, 1970) is that by A. Abrami (Publ. Oss. Trieste, No. 321, 1963). This has some differences from Adams' orbit. High-dispersion observations have been continued at Victoria by C.D. Scarfe, and it should be possible soon to give a definitive spectroscopic orbit of this system. System532Orbit1End System533Orbit1Begin Another member of A.D.S. 6993 at about 3" from AB. Some spectrograms may be contaminated by light from AB. System533Orbit1End System534Orbit1Begin See note for HD 61926 System534Orbit1End System535Orbit1Begin See note for HD 61926. The observations also admit a period of 14.75d. System535Orbit1End System536Orbit1Begin See note for HD 61926. These elements are based on a few rather weak spectrograms and even the period is uncertain. System536Orbit1End System537Orbit1Begin The orbit was assumed circular and the epoch is primary minimum. Whelan et al. gave ranges for the elements K1, K2 and V0, 100 -- 103 km/s, 138 -- 240km/s, and 6 to 15 km/s respectively; we have given the means. The orbital inclination is estimated (from the light-curve also obtained by Whelan et al.) at 68 deg. The minima are of nearly equal depth. The system is of interest because it belongs to the very old cluster M67 and yet is very similar to TX Cnc which belongs to the young Praesepe. System537Orbit1End System538Orbit1Begin Although this star has been known to be a two-spectra binary for some time (H.A. Abt and K.L. Moyd, Astrophys. J., 182, 809, 1973) these elements are the first to be determined. The orbital eccentricity is insignificantly small and the epoch is T0. The two spectra are described as very different in intensity. Abt and Levy classify the primary spectrum as A3, A8 and F0, from the K line, hydrogen lines and metallic lines respectively. System538Orbit1End System539Orbit1Begin A newly discovered eclipsing variable that has attracted much interest. Two independent spectroscopic orbits have been published before Andersen's: they are by C.R. Chambliss (Mon. Not. Roy. Astron. Soc., 142, 113, 1969) and D.H.P. Jones (Mon. Notes Astron. Soc. South Africa, 28, 5, 1969). Andersen's observations of are appreciably higher dispersion than either of the other two sets, and define beautifully all that part of the velocity curve over which the two components can be resolved. Agreement between the three sets of observations is not good, but this is probably because of the low dispersions employed in the earlier work, especially by Chambliss. The orbit was assumed circular and the epoch is primary minimum. The spectral classifications are by Jones, and were taken over by Andersen. Photoelectric observations in yellow and blue have been published by C.R. Chambliss (Astron. J., 72, 518, 1967) from whose paper the magnitude at minimum has been estimated. His solution has been rediscussed by H.G. Horak (Bull. Astron. Inst. Csl, 26, 257, 1975) and H.E. Jorgensen (Astron. Astrophys., 44, 459, 1975) who gives i=83 deg (approx.) and the fractional luminosity of the brighter star as 0.51 (in yellow). System539Orbit1End System540Orbit1Begin A recently discovered, interesting, and massive system. Thackeray pointed out its similarity to iota Ori and H.D. 37756. He stated that the two spectra are clearly unequal in intensity. The system is being observed photometrically to find out if there are any eclipses. System540Orbit1End System541Orbit1Begin Lucy & Sweeney adopt a circular orbit. System541Orbit1End System542Orbit1Begin The epoch is primary minimum (defined as the eclipse of the more massive star, since the two eclipses are almost equal in depth). The orbit was assumed circular, in accordance with the light-curve. Values of V0 derived from each component are slightly, but not significantly, different. The star was identified as an eclipsing and spectroscopic binary by T.D. Kinman (Mon. Notes Astron. Soc. South Africa, 19, 62, 1960), but only with the appearance of the paper by Bell and Malcolm has a reliable orbit become available. The paper includes photometric observations and analysis. The orbital inclination is found to be close to 89 deg. The less massive component gives about 0.89 of the light of the more massive (in V). The system is believed to be in contact, or nearly so. The period has been constant for at least 25 years. System542Orbit1End System543Orbit1Begin Brighter component of A.D.S. 7114: companion 9.5m, currently at 4.5". The companion is itself double, and a visual orbit has been computed for the pair BC. System543Orbit1End System544Orbit1Begin The elements given supersede those in an earlier note by Neubauer (Publ. Astron. Soc. Pacific, 42, 354, 1930). The appreciable eccentricity is unusual in a system of such short period. Neubauer also drew attention to the small mass-function. A 7.5m companion at 2.7" is listed in I.D.S. System544Orbit1End System545Orbit1Begin Orbital elements have also been published by J.L. Greenstein and A. Saha (Astrophys. J., 304, 721, 1986), who find an appreciably lower value of K1. This is probably because they did not resolve the secondary spectrum. Latham et al. report that they can see it in the cross-correlation function, but they have made no estimate of K2. Greenstein and Saha suggested that the companion of this high-velocity subdwarf -- one of the few Population II binaries with determined elements -- might be either a white dwarf or a subdwarf of late K or M spectral type. The detection of its spectrum by Latham et al. points towards the latter alternative. System545Orbit1End System546Orbit1Begin Abt and Levy assumed the values of P (21.85y), T, e and omega (adjusted to the primary component) from the most recent visual orbit by W.D. Heintz (Veroff. Sternw. Munchen, 7, 31, 1967). They find that their velocities and those obtained by Underhill (Publ. Dom. Astrophys. Obs., 12, 159, 1963) fit the predictions of Heintz' orbit quite well. Their value of V0 is in close agreement with Underhill's. Their preliminary value of K1 is higher than hers: the masses she deduced for the system were surprisingly low. The parallax is 0.074" and the inclination 134.8 deg. P. Baize (J. Observateurs, 38, 40, 1955) gives Delta m=2.0. Three other companions are listed in I.D.S. but all at large angular distances. The star was formerly known as 10 UMa, but it is no longer within the boundaries of that constellation. System546Orbit1End System547Orbit1Begin The magnitude at maximum has been measured photoelectrically; the value given for the minimum is estimated from plots of the light-curve. The spectral types are given by Andersen and Popper as G2-G5. The epoch is primary minimum (the eclipses are almost, but not quite, equal) and the orbit is assumed circular in agreement with the light-curve. Both components show H and K emission in their spectra and the system is regarded as one of the RS CVn group, although the distortion of the light-curve is very small. It is unusual, among members of that group, in having two components that are equal in all respects, within the observational errors. Two photoelectric light-curves have been published since the appearance of the Seventh Catalogue. J. Andersen et al. (Astron. Astrophys. Supp., 43, 141, 1981) have observed the binary in the uvby system and find an orbital inclination very close to 88 deg and that the (just) more massive component has a luminosity in y about 5 percent greater than the other. P.V. Rao and M.B.K. Sarma (Photometric and Spectroscopic Binary Systems, p. 361, 1981) observed in the UBV system. They agree with Andersen et al. on the inclination but make the primary component about 13 percent brighter (in V) than the secondary. Andersen et al. discuss the age of the binary (its high systemic velocity suggests that it is old) but they suspend judgment on the topic. System547Orbit1End System548Orbit1Begin System548Orbit1End System549Orbit1Begin Lucy & Sweeney adopt a circular orbit. System549Orbit1End System550Orbit1Begin Listed by Abt and Snowden as an Si, Sr, Cr star. Elements for such a long-period low amplitude binary must be regarded as provisional until they are confirmed. System550Orbit1End System551Orbit1Begin Andersen's observations are of higher dispersion than earlier ones by M.W. Feast (Mon. Not. Roy. Astron. Soc., 114, 246, 1954). Andersen's values of K1 and K2 have been preferred over Feast's slightly smaller ones because Andersen also carefully investigated sources of systematic error. The orbit was assumed circular (since confirmed by the light-curve) and the epoch is T0 for the `primary' component. (The two minima are almost equal and the spectra are indistinguishable in type, but one is about ten percent stronger than the other). J. Clausen and B. Gronbech (Astron. Astrophys., 58, 131, 1977) have published uvby photometry of this system (upon which the spectral types given in the Catalogue are based). They find an orbital inclination just under 87 deg and assign equal visual magnitudes to the two components. System551Orbit1End System552Orbit1Begin The star H.D. 77581 is the optical counterpart of the X-ray source 3U 0900 49 which, as one of the optically brightest known X-ray sources, has been much observed. It is impossible to list all references to the study of this system. Orbital studies include: E.J. Zuiderwijk et al. (Astron. Astrophys., 35, 353, 1975), L.O. Petro and W.A. Hiltner (Astrophys. J., 190, 661, 1974), J.B. Hutchings (Astrophys. J., 192, 685, 1974), G. Wallerstein (Astrophys. J., 194, 451, 1974), S. Rappaport et al. (Astrophys. J., 206, L103, 1976), J.A. van Paradijs et al. (Nature, 259, 547, 1976 and Astron. Astrophys. Supp., 30, 195, 1977) and P.E. Boynton et al. (Astrophys. J., 307, 545, 1986). The orbit of the X-ray pulsar, depending as it does on pulse timing, is very accurately determined (although, note that a sin i is the observed quantity and K1 the derived). The epoch is T0. The orbit of the visible star is less well determined, but better determined than those of the optical counterparts of other X-ray sources. Optical values of e and omega are in reasonably good agreement. Since the paper cited in the Catalogue gives only the elements of the X-ray pulsar, those of the visible star have been taken from the second reference above to van Paradijs et al., except for V0, which is not given by them, and comes from the paper by Rappaport et al. There is as yet no evidence for changes in omega. The epoch is the time at which the mean longitude of the X-ray source is 90 deg (in a circular orbit, that would be the time of superior conjunction). Van Paradijs et al. (1977) estimate minimum masses of 17 MSol (X-ray source) and 20.5 MSol and that the orbital inclination is certainly larger than 74 deg. System552Orbit1End System553Orbit1Begin Epoch is T0. A large deviation from the velocity-curve is noticed just after eclipse. This may be a rotation effect. R.S. Dugan found from the light-curve (Princeton Obs. Contr., 14, 1933) that i=85.6 deg and the light-ratio is about 0.07. System553Orbit1End System554Orbit1Begin Three earlier investigations (N. Ichinohe, Astrophys. J., 25, 318, 1907; J.A. Pearce and P. Riddle, Publ. Astron. Soc. Pacific, 10, 65, 1940; and O. Struve, Astrophys. J., 99, 210, 1944) give results in good agreement with those obtained by Aikman. The star is an Hg, Mn star. System554Orbit1End System555Orbit1Begin The star is listed in the H.D. Catalogue as having a composite spectrum. It is now considered to be an Am star. The types from the K line, hydrogen lines and metallic lines are A5, F0 and F6II, respectively. Bretz reports no trace of the secondary spectrum `apparent in lambda 4500 region'. Star is brighter component of A.D.S. 7211: companion 10.3m at 57.2". System555Orbit1End System556Orbit1Begin The new observations by Beavers and Salzer, revealing the presence of both spectra, supersede those of R.F. Sanford (Astrophys. J., 55, 30, 1922) on which the previously known single-spectrum orbit was based. The new value of K1 is somewhat larger than Sanford's -- a clear indication that he was measuring blended spectra. Beavers and Salzer find the magnitude difference of the two components (in blue) to be 1.0m (from the relative strengths of the dips in the radial-velocity traces) and they estimate that the individual spectral types are G2 and G6 to K0. System556Orbit1End System557Orbit1Begin Epoch is T0. Lucy & Sweeney adopt a circular orbit. A 6.2m companion at approximately 0.1" is listed in I.D.S. System557Orbit1End System558Orbit1Begin Abt and Levy use the observations obtained by R.K. Young (Publ. Dom. Astrophys. Obs., 2, 205, 1923) as well as their own to obtain these elements which are closely similar to those obtained by Young. Both Luyten and Lucy & Sweeney accept the reality of the orbital eccentricity. A companion at 49" is listed in I.D.S. System558Orbit1End System559Orbit1Begin These elements are described as preliminary by Griffin and Griffin themselves, primarily because of the limited number of observations at the node at which the velocities of the two components differ by relatively little. Nevertheless the elements of the spectroscopic orbit are in reasonable agreement with those it has in common with the interferometric orbit (W.S. Finsen, Republic Obs. Circ., 7, 116, 1966). The system has also been observed by speckle interferometry (e.g. H. McAlister Astrophys. J. Supp., 43, 549, 1980) and, as the Griffins point out, the prospects of eventually obtaining very accurate values for the masses of the components are high. Finsen estimated Delta m=0; judging from the radial-velocity traces, there is a small difference in magnitude. The orbital inclination is close to 55 deg. In I.D.S., two faint companions to the close pair are listed; one is 13.2m at 35.4" and the other (probably optical) is 10.6m at 222". System559Orbit1End System560Orbit1Begin This star was formerly known as 21 Hya. After the discovery that its light varies, the star received the designation KW Hya. In some catalogues, however, it was erroneously listed as KM Hya and appears under that name in the paper by Andersen and Vaz. These authors later drew attention to the error themselves (Astron. Astrophys., 175, 355, 1987). The new observations supersede the orbit formerly determined by M.-T. Chauville (Astron. Astrophys., 40, 207, 1975). There is general agreement that the primary spectrum is an Am spectrum. Curchod and Hauck give A5, A7 and A9 from the K line, hydrogen lines and metallic lines respectively, but Andersen and Vaz favour slightly earlier types. They do not give a precise classification for the secondary spectrum, which is certainly later than the primary. The epoch is the time of primary minimum. The orbital eccentricity and time of periastron derived from the velocity-curve are in good agreement with the same quantities derived from the light-curve. The latter values are given in the Catalogue, and the other elements were derived with those quantities fixed. Andersen and Vaz have found an appreciably larger value for K2 than did Chauville. The value given for V0 is that appropriate to the primary component. The small difference in the two values of V0 is probably not significant. Analysis of the light-curve leads to an orbital inclination close to 88 deg and a difference of visual magnitude, between the components, of 1.44m. Andersen and Vaz find it difficult to determine a unique evolutionary state for the two components of this system. System560Orbit1End System561Orbit1Begin These results confirm those obtained by H.D. Curtis (Lick Obs. Bull., 4, 153, 1907). Both sets of elements were obtained from graphical solutions. System561Orbit1End System562Orbit1Begin The minimum magnitude given is an estimate from the plot of the light-curve. The spectral classification of the primary is in disagreement with an earlier published one of A4. That of the invisible secondary is an estimate based on the photometric data. The epoch is the time of primary minimum and the orbit was assumed circular, in accordance with the light-curve. The orbital inclination is found to be 88 deg or 89 deg. The fractional luminosity of the primary component (in V) is 0.98. Although the system is of short period, the two stars are believed not to be in contact. System562Orbit1End System563Orbit1Begin Elements regarded as provisional by Harper. Later (Publ. Dom. Astrophys. Obs., 6, 225, 1935) he revised P to 15.990d and T to J.D. 2,420,750.851. System563Orbit1End System564Orbit1Begin Some of these spectra had earlier been used by J. Lunt to determine orbital elements which were not published. In I.D.S. an 11.0m companion is listed at 1.6". System564Orbit1End System565Orbit1Begin The orbit was assumed circular after an elliptical solution showed no great improvement in the representation of the observations. The epoch is T0. The star is probably a giant. There is an unusually large scatter (for photoelectric measures) of observations near the ascending node in phase. System565Orbit1End System566Orbit1Begin The orbit was assumed circular and the epoch is T0. The star is the brighter component of A.D.S. 7348 A. The companion is 8.5m at 1.4". System566Orbit1End System567Orbit1Begin Although the elements were determined by a graphical method, their values seem to be fairly well established. W. Buscombe and P.M. Morris (Mon. Not. Roy. Astron. Soc., 121, 263, 1960) obtained five new spectrograms, and suggest the following modifications to the elements: P=116.776d, T=J.D. 2,416,456.66 and omega=92.60 deg. System567Orbit1End System568Orbit1Begin The orbit is assumed circular and the epoch is T0. The elements given are derived from the base of the He II emission lines. Somewhat different values (even for the period) are derived from the peak. Cowley et al. estimate that the secondary star is a G-type giant of approximately solar mass. System568Orbit1End System569Orbit1Begin The orbit is assumed circular and the epoch is T0. The spectroscopic observations are few and heterogeneous, and were not made by Raveendran et al. The period is derived photometrically and the star probably belongs to the RS CVn group. System569Orbit1End System570Orbit1Begin This is a W-type W UMa system that has not previously been observed spectroscopically. The epoch is the time of primary minimum as given by B.B. Bookmyer and D.R. Faulkner (Publ. Astron. Soc. Pacific, 90, 307, 1978). However, King and Hilditch found it necessary to add 0.05m to the phases of their observations to bring them into agreement with the light-curve, which indicates that the period has changed in the intervening years. The velocities were determined by cross-correlation from Reticon observations. No solution of the light-curve appears to be available. System570Orbit1End System571Orbit1Begin Coverage of the velocity curve is very sketchy, but P (116.85y), T, e and omega are assumed from the visual orbit by P. Muller (Bull. Astron. Paris, 21, 131, 1957) for which i=64.5 deg. The system is A.D.S. 7390. System571Orbit1End System572Orbit1Begin Both components have Am spectra classed as A1 from the ratio of Ca to H lines, and F0 from the metallic lines. There must be some difference in temperature between the stars, however, since Heard and Hurkens found Delta m=0.38 from the Fe I lines, and Delta m=0.23 from the Fe II lines. The secondary star is thus the hotter. The other point of interest about the system is that it has largest minimum masses of any known system containing Am stars. System572Orbit1End System573Orbit1Begin Orbital elements have also been published by A.H. Joy (Astrophys. J., 64, 287, 1926). Joy thought he could detect the secondary spectrum, but Popper could detect only its effect on the wings of the lines of the primary component's spectrum. The value of V0 is uncertain because of uncertainty about the wave-lengths to adopt. Epoch is T0 computed from Popper's time of minimum. The magnitude of 6.28 at maximum is given by Popper on the V-scale. The range is estimated from his light-curve. The spectral type of the secondary star is an approximate estimate from the photometric data. A.R. Hogg and P.W.A. Bowe (Mon. Not. Roy. Astron. Soc., 110, 373, 1949) found from their photoelectric light-curve that i=70.1 deg and the light-ratio is approximately 0.3. Quite similar results were obtained from the same photometric observations by G. Russo et al. (Astron. Astrophys. Supp., 47, 211, 1982) who pointed out, however, that the radii derived are larger than for main-sequence stars. They suggest that new spectroscopic observations are needed. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System573Orbit1End System574Orbit1Begin Griffin suggests that the spectrum is probably K2 III (consistent with the observed colours). System574Orbit1End System575Orbit1Begin Brightest component of A.D.S. 7438: B is 8.0m at 24.7". Component C, 8.7m at 117.8", does not share the proper motion of A. Epoch is T0. Reference: R.J.Northcott, Private Comm.,,, 1965 System575Orbit1End System576Orbit1Begin Griffin believes the star to be a giant (there is no known luminosity classification) and suggests that the invisible secondary spectrum is that of an F or G dwarf. System576Orbit1End System577Orbit1Begin The spectrum has also been classified as A2 (G. Hill et al., Mem. Roy. Astron. Soc., 75, 131, 1975). The epoch is T0 and the orbit was assumed circular -- as it is now demonstrated to be by the light-curve. Early attempts to analyze the light-curve ran into difficulties (R.E. Wilson, Astron. J., 70, 368, 1965). Solutions could be obtained only by postulating an extended atmosphere or third light. P. Broglia and P. Conconi (Astron. Astrophys. Supp., 27, 285, 1977 -- the magnitudes in the Catalogue were taken from this paper) were able to solve their new BV light-curves by the Wilson-Devinney method without the help of such hypotheses. They find that the secondary (probably of mid-G spectral type) fills its Roche lobe, that the orbital inclination is close to 84 deg and the fractional luminosity (in V) of the primary star is about 0.94. These results were confirmed by F. Mardirossian et al. (Astron. Astrophys. Supp., 27, 285, 1977). System577Orbit1End System578Orbit1Begin Epoch is T0 : orbit assumed circular. Four-colour photoelectric observations by H.L. Johnson (Astrophys. J., 131, 127, 1960) yield i=85.17 deg, Delta m=4.85. Magnitudes given in catalogue are based on Johnson's V observations. A new study of Johnson's infrared light-curve by G. Giuricin, F. Mardirossian and F. Predolin (Inf. Bull. Var. Stars, No. 1786, 1980) does not significantly change these results. System578Orbit1End System579Orbit1Begin System579Orbit1End System580Orbit1Begin Epoch is T0. Eccentricity is less than 0.02 and was assumed to be zero. Very similar values for the elements were published by W. Zurhellen (Astron. Nachr., 173, 353, 1907). Plummer emphasizes the difficulties of measurement arising from the superposition of two spectra (the composite nature of the spectrum is the result of the blending of the spectra of the spectroscopic-binary components). The close agreement between Plummer's results and Zurhellen's, however, suggests that the elements are reasonably well determined. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements and justify the b rating. Parsons points out that the values of K1 and K2 were ascribed the wrong way around in the Seventh Catalogue. As is to be expected, the A-type star has the larger amplitude. He also gives T0 0.21d earlier. Star is brighter member of A.D.S. 7480: this pair, however, appears to be optical. System580Orbit1End System581Orbit1Begin Earlier spectroscopic observations have been published by W.S. Adams and A.H. Joy (Astrophys. J., 49, 189, 1919), O. Struve and H.G. Horak (Astrophys. J., 112, 178, 1950), D.M. Popper (Publ. Astron. Soc. Pacific, 62, 115, 1950), L. Binnendijk (Publ. Dom. Astrophys. Obs., 13, 27, 1967) and S.P. Worden and J.A.J. Whelan (Mon. Not. Roy. Astron. Soc., 163, 391, 1973). It is difficult to choose between the last of these and McLean's results. On the one hand, McLean's observations are of higher dispersion; on the other, as he himself points out, Worden and Whelan made more observations at higher time-resolution. The differences are not great. That in V0, if significant, is probably only a systematic error. The two values of K2 are nearly identical. McLean's somewhat lower value of K1 brings his determination of the mass-ratio somewhat closer to the photometric values; his elements have been preferred largely on this account. The orbit is assumed circular, in accord with the light-curve, and the epoch is the time of eclipse of the less massive component as deduced from the phases given by McLean. There is some evidence of variable emission in the K line. As already mentioned, synthetic light-curves (S. Mochnacki Bull. Am. Astron. Soc., 4, 339, 1972, J.B. Hutchings and G. Hill Astrophys. J., 179, 539, 1973) lead to a lower mass-ratio than is found spectroscopically. This is further confirmed by R.W. Hilditch (Mon. Not. Roy. Astron. Soc., 196, 305, 1981). A full discussion of the difficulties of analyzing the light-curve of this system has been published by A.P. Linnell (Astrophys. J., 316, 305, 1987), who criticizes the hypothesis of starspots as an explanation of some features of the light-curves. There seems general agreement that the orbital inclination is somewhat in excess of 80 deg, although lower values have been published (P.G. Niarchos, Astrophys. Space Sci., 58, 301, 1978, S.R. Jabbar and Z. Kopal, ibid., 92, 99, 1983). Hutchings and Hill ascribe 0.59 of the total light to the primary component. The system is the brighter member of A.D.S. 7494: the companion, probably optical, is 13.1m at 7.0". Worden and Whelan found that BD+55 1351 has the same radial velocity as the centre of mass of W UMa, while O.J. Eggen (Mem. Roy. Astron. Soc., 70, 117, 1967) has suggested that these two stars share a common proper motion. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System581Orbit1End System582Orbit1Begin The minimum magnitude is estimated from a plot of the light-curve by A. Okazaki (Publ. Astron. Soc. Japan, 29, 289, 1977). The spectrum may be as late as A3 (G. Hill et al., Mem. Roy. Astron. Soc., 71, 131, 1975). Epoch is T0 and the orbit was assumed circular. Okazaki obtained eleven coude spectrograms, but he did not publish new elements, noting that his measures of radial velocity agreed with Struve's velocity curve. (Therefore, we have upgraded the quality from e to d). Okazaki estimates that the secondary spectrum is about G5 and finds that the system is not an undermassive `R CMa' system. His light-curve yields an inclination of 86 deg and a fractional luminosity (in V) for the primary of 0.87. Similar results were obtained from the same observations by B. Cester et al. (Astron. Astrophys. Supp., 36, 273, 1979). System582Orbit1End System583Orbit1Begin Although this star has been known for a long time to have a variable velocity (J.S. Plaskett et al., Publ. Dom. Astrophys. Obs., 1, 163, 1920), this is the first set of orbital elements published for it. The epoch is T0 for the primary component and the orbit was assumed to be circular. The star is a visual binary (Kui 44); the separation of the two components is about 0.4" and has apparently remained unchanged for forty years. One component is the two-spectra binary and the other is a delta Sct variable. The V magnitude of the entire system varies by about 0.2m. According to Fekel and Bopp all three components are of the same spectral type (A8 IV) and of nearly equal luminosity. The members of the close pair may show some marginal Am characteristics in their spectra. The coverage of the velocity curve is not complete, and this accounts for the relatively low grade assigned to the elements. System583Orbit1End System584Orbit1Begin The orbit is assumed circular and the epoch is T0. Carquillat et al. estimate that the invisible secondary spectrum is at least as late as K1 and that the orbital inclination is greater than 27 deg. These elements have been in a large measure confirmed by D.W. Latham et al. (Astron. J., 96, 567, 1988). System584Orbit1End System585Orbit1Begin Preliminary results were published by Popper (Astrophys. J., 109, 100, 1949). Binary nature of star was discovered by Shajn (Pulkovo Obs. Circ., No. 2, 1932). Elliptical elements were also derived in the paper by Popper and Shajn, and e was found to be 0.014. Epoch is T0. Popper states that his contribution to the paper was limited to supplying Shajn with the Yerkes spectrograms. System585Orbit1End System586Orbit1Begin This is a system of the U Gem type and the motion of the white-dwarf component can be determined only from measures of the H-alpha emission. The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. Coverage of the velocity-curve is good, but the scatter of individual observations is large. No absolute value is given for the systemic velocity. System586Orbit1End System587Orbit1Begin Luyten's recomputation is preferred to the orbital elements derived by H.S. Jones, from these same observations (Cape Annals, 10, pt. 8, 53, 1938), because Jones had to fix T. Epoch given is T0. System587Orbit1End System588Orbit1Begin Despite the appreciable orbital eccentricity, the epoch is the time of primary minimum. The values of e and omega were fixed at those obtained from the light-curve. The system displays apsidal motion with a period of 354 years. The orbital inclination is found to be nearly 36 deg, and the stars are estimated to differ by 0.3m in V. System588Orbit1End System589Orbit1Begin The new elements supersede the original orbit by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 194, 1925) and the later one by Abt and Levy (Astrophys. J. Supp., 30, 273, 1976) primarily because Batten and Morbey succeeded in measuring the secondary spectrum. Although the new elements of the primary differ little from those derived by Abt and Levy, the new observations made it possible to reconcile all available observations on one period. A circular orbit was adopted, after consideration of both circular and elliptical solutions, and the epoch is T0. Batten and Morbey estimated from spectrophotometry that Delta V=0.92m and that the secondary spectrum is approximately G0. These results are consistent with the small trigonometrical parallax of 0.038". System589Orbit1End System590Orbit1Begin The magnitude may be slightly variable and there are discordant spectral (and luminosity) classifications in the literature. In particular, O.J. Eggen (Astrophys. J. Supp., 55, 597, 1984) gives B9 III. The orbital elements are derived from a heterogeneous set of observations and slightly different values can be found for each element (including the period) for different selections of the observations to be used. In particular, because of differences between observatories, the value of V0 is highly uncertain. System590Orbit1End System591Orbit1Begin This RS CVn binary (not yet known to eclipse) was recognized as a single-spectrum binary by C.T. Bolton et al. (Astron. J., 86, 1267, 1981) who derived orbital elements and found a discrepancy between their photometry of the system and the trigonometric parallax. Barden showed that the spectrum exhibits three sets of lines although there is, as yet, no orbit for the third body. The presence of the third body can account for discrepancy found by Bolton et al. The orbit was assumed circular and the epoch is T0 for the primary as determined by Bolton et al. There is some evidence of a small phase difference between the two sets of observations. Barden gives the spectral type of the secondary as `late K or M0 dwarf' and the third component is similar. System591Orbit1End System592Orbit1Begin See note for HD 61926. System592Orbit1End System593Orbit1Begin Two recent studies supersede that by O. Struve and V. Zebergs (Astrophys. J., 130, 137, 1959). The other is by B.J. Hrivnak et al. (Astrophys. J., 285, 683, 1984). This and Barden's study are of similar quality. The sums of K1 and K2 from the two investigations are nearly similar, but the mass-ratio is different, and the work of Hrivnak et al. may have been affected by the lines of the spectra of the companion (see note XY Leo B). The epoch is T0 and the orbit was assumed circular. The minimum magnitude given is an estimate based on the eclipse depth. Four recent photometric analyses (B. Hrivnak, Astrophys. J., 290, 696, 1985, J. Kaluzny and G. Pojmanski, Acta Astron., 33, 277, 1983, R.W. Hilditch, Mon. Not. Roy. Astron. Soc., 196, 305, 1981 and R.H. Koch and C.R. Shanus, Astron. J., 83, 1452, 1978) agree on an orbital inclination around 67 deg. The last named also give Delta V=0.2m. All these results, however, were obtained before the discovery of the companion which is the subject of the next note. Spectral types assigned to this system and the next must necessarily be imprecise. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System593Orbit1End System594Orbit1Begin The contact binary XY Leo has long been known to display period changes that were apparently themselves periodic. A third body has often been suspected, but never detected until Barden found the lines of two other spectra in the combined light of the system and derived orbital elements for another short-period pair. The presumption is therefore strong that these two pairs are revolving around their common centre of mass in about 20 years. Emission features at H-alpha and H and K are ascribed by Barden to this second binary which he believes to be of the BY Dra type. The orbit is assumed circular and the epoch is the time of superior conjunction of the primary component. Barden gives no direct estimate of the magnitude of the companion, which is not seen separately from the contact binary and the spectral types are estimates based on masses derived from an assumed orbital inclination (31 deg) for the new pair. Barden believes the orbits in the quadruple system are not coplanar. System594Orbit1End System595Orbit1Begin See note for HD 61926. A shorter period is also possible. An 11.5m companion at 9.1" is listed in I.D.S. System595Orbit1End System596Orbit1Begin The observations are few and define only the nodes of the velocity-curves. The epoch is the time of primary minimum and the orbit is assumed circular. Since McLean and Hilditch were not explicit about the ephemeris used, we have adopted that given by G. Hill (Publ. Dom. Astrophys. Obs., 15, 297, 1979). He found an orbital inclination close to 80 deg and that the primary gives about five times as much light as the secondary. System596Orbit1End System597Orbit1Begin See note for HD 61926. Other periods are still possible. Two companions are listed in I.D.S.: 13.8m at 16.6" and 10.2m at 22.4" System597Orbit1End System598Orbit1Begin The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The period is uncertain, a value of 0.525d is still possible. The primary spectrum shows only emission lines of hydrogen, helium and ionized calcium. There are absorption lines that appear to come from the secondary spectrum and correspond to K2 approx 70 km/s. Thorstensen estimates that the secondary component has a K or very early M spectral type and contributes about 30 percent of the light at lambda 5893. The system is a weak X-ray source. System598Orbit1End System599Orbit1Begin See note for HD 61926. Other periods are possible. System599Orbit1End System600Orbit1Begin This is another system of the U Gem type, which was shown to be an eclipsing variable with one of the shortest known periods by N. Vogt (I.A.U. Circ., No. 3357, 1979). The epoch is the time of primary minimum and the orbit was assumed circular. The only features in the spectrum are double emission peaks, of hydrogen and helium, flanking a central absorption. The value given for K1 is an approximate mean of that derived from each set of peaks and the absorptions separately. The value of V0 is approximately that derived from the central absorption. H. Ritter (Astron. Astrophys., 85, 362, 1980) derives an orbital inclination of 76 deg from the light-curve. N. Vogt et al. (Astron. Astrophys., 94, L29, 1981) also discuss the light-curve. System600Orbit1End System601Orbit1Begin The velocity variation is probably well established, but the scatter of individual observations is an appreciable fraction of the total range. System601Orbit1End System602Orbit1Begin Brightest component of A.D.S. 7671: B is 13.3m at 56.4", C is 11.5m at 112.2". Lucy & Sweeney adopt a circular orbit. System602Orbit1End System603Orbit1Begin The recomputation by Lucy & Sweeney is preferred over the original solution by A. Gilardini (Mem. Soc. Astron. Ital., 22, 33, 1952) partly because that publication is not available at Victoria. A. Krancj (Publ. Bologna Univ. Obs., 7, No. 11, 1959) also computed elements based on these observations. The epoch is T0. The standard deviation of a single observation, as computed by Lucy & Sweeney, is fairly large, and the d quality is assigned on that basis. System603Orbit1End System604Orbit1Begin The binary nature of this star was discovered by G. Shajn and V. Albitzky (Mon. Not. Roy. Astron. Soc., 92, 771, 1932), but these are the first orbital elements to be determined System604Orbit1End System605Orbit1Begin This is another eclipsing cataclysmic variable. The only measurable features in the spectrum are emission lines and the velocities are derived from measurements of the base of the H-gamma emission. The orbit was assumed circular and the epoch is the time of primary minimum. The value given for V0 is an estimate. Penning et al. also estimate that the orbital inclination is about 79 deg. The system is very similar to that of UX UMa. System605Orbit1End System606Orbit1Begin No spectral type is given for this nova-like variable. The spectrum shows very broad absorptions of hydrogen, helium and ionized calcium and weak emission of the first and last elements. The orbit is assumed circular and the epoch is T0. Individual measurements are very uncertain, as is the period. Even the binary nature of the object is not beyond doubt. System606Orbit1End System607Orbit1Begin Epoch is T0. Narrow emission lines are observed in the H and K lines. Lucy & Sweeney adopt a circular orbit. System607Orbit1End System608Orbit1Begin The old observations by R.H. Baker (Publ. Allegheny Obs., 2, 29, 1910) and F. Schlesinger (ibid., 139, 1912) are superseded by two modern high-dispersion sets of observations. The one not used in the Catalogue is by L. Oetken and R. Orwert (Astron. Nachr., 294, 261, 1972). These two modern determinations agree quite well. They both lead to a higher K1 and a lower e than Schlesinger found. Oetken and Orwert find a smaller K2 (60.5) than does Nariai. Neither of the modern sets of observations covers well the node of the orbit at which the spectral lines of the two components are more widely separated. The spectrum is classified as of the Hg, Mn type. System608Orbit1End System609Orbit1Begin Although the observations are at fairly high dispersion, the standard deviation of a single observation, as given by Popper, is fairly large and this has led to the d classification. The orbit was assumed circular and the epoch is the time of primary minimum. The H.D. spectral type is F5 but Popper estimates spectral types of F3 or F4. Photometry lends some support to the H.D. classification. K. Gyldenkerne et al. (Astron. Astrophys., 42, 303, 1975) have published uvby light-curves of the system. They have some difficulty in reaching a definitive solution for orbital elements, and a range of values is possible. The orbital inclination is about 85.1 deg and the brighter component contributes between 0.5 and 0.6 of the total light. The colours of the two stars are similar. There appear to be no UBV measures of the star: the depth of eclipse in y is about 0.54m. G. Giuricin et al. (Astron. Astrophys., 85, 259, 1980) re-examined the observations made by Gyldenkerne et al. and also encountered difficulties because it is not possible, from the light-curve alone, to decide whether primary eclipse is a transit or occultation. Their conclusions are similar to those of Gyldenkerne et al. System609Orbit1End System610Orbit1Begin The colour-index of the star is inconsistent with the G0 classification, unless the star is a supergiant -- which appears unlikely. Radford and Griffin suggest it may be a late-type giant. The epoch is T0. System610Orbit1End System611Orbit1Begin Although there is no luminosity classification of the spectrum available, Griffin believes the star to be a giant. System611Orbit1End System612Orbit1Begin The values of P, e, omega are adopted by Underhill from an unpublished visual orbit by G. van Biesbroeck. No value is quoted for T but it must be close to J.D. 2,437,000. The quality class refers only to the spectroscopic elements. There is some evidence for a secondary variation in the velocities. P. Baize (J. Observateurs, 33, 125, 1950 gives P=37.9y, T=1917.0, omega=42 deg, e=0.61, a=0.39" and i=82 deg). Recently, W.D. Heintz (Comm. 26, I.A.U. Circ. d'Inf., No. 84, 1981) slightly revised these elements. Observations are being continued and new solutions should probably make use of Baize's or Heintz' orbital elements although C.D. Scarfe (Astrophys. Space Sci., 11, 112, 1971) has shown that at present there is very little difference in the velocities predicted by them and by van Biesbroeck. The system is A.D.S. 7780. Assuming a parallax of 0.02", Underhill finds masses of 2.10 MSol and 0.54 MSol. System612Orbit1End System613Orbit1Begin This is listed by Abt and Snowden as a Cr, Sr star. The observations show very little variation in velocity, no velocities having been obtained near the predicted sharp peak of the curve. In view of the long period proposed (12,658.4d), the reality of the velocity variation should be confirmed. System613Orbit1End System614Orbit1Begin These new observations supersede the earlier results published by V.S. Niemela (Astrophys. Space Sci., 45, 191, 1976 and I.A.U. Symp. No. 88, p. 177, 1980). The upper line of the Catalogue gives elements derived from the emission lines of N V, and the lower those from the absorption (O-type) spectrum. Values of both K and V0, derived from other emission lines, are different. The epoch is the time of periastron passage, but the orbits probably should be regarded as circular. The light of the system varies by a few hundredths of a magnitude, with the orbital period. Niemela and Moffat suggest that the variation is caused by the electron-scattering envelope of the W-R star passing in front of the O-type star and, on that hypothesis, deduce an orbital inclination between 46 deg and 61 deg. System614Orbit1End System615Orbit1Begin The new paper by Hilditch and Lloyd-Evans contains no new spectroscopic observations that were not in the earlier paper (T. Lloyd-Evans, Mon. Not. Roy. Astron. Soc., 161, 15, 1973). It does contain a new discussion, however and a light-curve and photometric analysis. Hilditch and Lloyd-Evans adopt a circular orbit after some discussion, despite a small apparent displacement of primary minimum. The epoch appears to be an estimated time of primary minimum. Analysis of the light-curve leads to an orbital inclination of about 62 deg and a difference in visual magnitudes of the two components of 0.3m. The stars are nearly in contact and the system belongs to the cluster I.C. 2581. System615Orbit1End System616Orbit1Begin The magnitudes given are the extreme values measured by B.F. Madore (Astrophys. J. Supp., 29, 219, 1975). The star is a Cepheid variable which is also a member of a binary system. The orbital elements are described as `tentative' by Coulson himself. The secondary spectrum is not visible. Coulson believes its type to be between B5 and A5, if the star is on the main-sequence, and A, if the star is a giant. System616Orbit1End System617Orbit1Begin This is a double-mode Cepheid that is also a member of a binary system. The observations show a large scatter because the effects of pulsation have not been entirely removed. Theoretical models of double-mode Cepheids suggest a mass of 17 MSol for the primary; evolutionary models suggest 5.0 MSol. The corresponding values obtained for the secondary, from the mass function, are 0.6 MSol and 1.2 MSol. The secondary is probably a main-sequence star of F-type. System617Orbit1End System618Orbit1Begin The elements obtained by Chamberlin and McNamara are in good agreement with those obtained by O.C. Mohler (Astron. J., 45, 40, 1936) except for K1 for which Mohler found 55.4 km/s. Lucy & Sweeney accept the reality of the orbital eccentricity. Light-curves in B and V have been obtained by J.B. Srivastava and C.D. Kandpal (Bull. Astron. Inst. Csl, 19, 381, 1968). Solution is difficult since primary eclipse is less than 0.1m deep in both colours, the scatter of observations is large and the fainter component of the visual binary (the system is A.D.S. 7837) is 8.5m at 2.4" separation and interferes with the photometry. They derive an orbital inclination of 66.8 deg and a fractional luminosity of the brighter member of the eclipsing pair of about 0.9. System618Orbit1End System619Orbit1Begin The epoch is T0. The F6 V classification is offered as a tentative one. Although the systemic velocity indicates that this might be a Population II star, Gorza notes that there is not apparently anything unusual about its metal abundance. P.S. Goraya and T.D. Padalia (Inf. Bull. Var. Stars, No. 2542, 1984) find the light of the star to be slightly variable and believe the hydrogen lines to be filled in by emission. The star is the brighter component of A.D.S. 7855, companion 11.0m at 4.4". System619Orbit1End System620Orbit1Begin The new elements supersede those determined by W.H. Christie (Astrophys. J., 80, 181, 1934) and remove the grounds he had for postulating a secondary variation with a period of about 220 days. In general, the new observations confirm Christie's work, but lead to reduced values of K1 and e. The primary component is probably a giant. System620Orbit1End System621Orbit1Begin See note for HD 61926. System621Orbit1End System622Orbit1Begin An earlier spectroscopic study was published by S. Gaposchkin (Astrophys. J., 104, 370, 1946) whose values of K1 and K2 were unreliable because his observations did not cover the nodes. Popper's observations, on the other hand, were concentrated at the nodes. He assumed a circular orbit and the epoch is T0. The out-of-eclipse magnitude is from R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 79, 101, 1975) and the minimum magnitude is estimated from this on the assumption that the depths of the nearly equal eclipses are about 0.7m. The secondary spectrum may be slightly later in type. Several discussions of photometric observations have been published since the Seventh Catalogue (T.B. Horak, Bull. Astron. Inst. Csl, 26, 257, 1975, B. Cester et al., Astron. Astrophys. Supp., 32, 351, 1978, and G. Giuricin et al., Astron. Nachr., 304, 37, 1983). There seems agreement that the orbital inclination is close to 83 deg and that the two stars are nearly equal in luminosity. The last-named authors, however, identify the primary eclipse as an occultation -- which complicates the picture of the system. System622Orbit1End System623Orbit1Begin New observations by Evans have led to an improvement over his earlier work (Mon. Not. Roy. Astron. Soc., 116, 537, 1956) and the orbital elements obtained by R.F. Sanford (Lick Obs. Bull., 9, 181, 1918). The system is a triple one in which the brighter component of the visual binary of period 16.30y is a spectroscopic binary with the ten-day period. The magnitude given is for the combined light of all components. The epoch is T0. The value of K2 is taken from Evans' earlier work. The spectrum of the visual secondary cannot be clearly detected, but it is believed to be A6 V and the star appears to be sub-luminous. Although O.J. Eggen (Mon. Notes Astron. Soc. South Africa, 18, 15, 1959) questioned this conclusion when it was first published, further study appears to confirm it. Evans proposes absolute visual magnitudes of 2.15, 2.70 and 2.14 for the two spectroscopic components and the visual secondary respectively. Inclination of the visual orbit is 129.4 deg and he derives masses of 2.13 MSol, 1.81 MSol and 2.41 MSol for the three stars. System623Orbit1End System624Orbit1Begin Although the star is classified as G5p in the H.D. Catalogue, Ginestet et al. consider the F8 V classification to be preferable. The observations are from several observatories. System624Orbit1End System625Orbit1Begin See note for HD 61926. The period is fixed by the observation of shallow eclipses (J. Kordylewska and R. Szafraniec, Eclipsing Bin. Circ. Cracow, No. 39, 1960). Perhaps the star is only an ellipsoidal variable. System625Orbit1End System626Orbit1Begin See note for HD 61926. A shorter period near 1.2d is possible. System626Orbit1End System627Orbit1Begin Lucy & Sweeney adopt a circular orbit. System627Orbit1End System628Orbit1Begin See note for HD 61936. The spectrum displays shell features and one set of observations shows no significant velocity variation at all. The binary nature of this object is questionable. System628Orbit1End System629Orbit1Begin The new results have superseded those previously published by V.S. Niemela (Publ. Astron. Soc. Pacific, 85, 220, 1973) having shown them to be based on an incorrect value of the period. Values of V0 and, to a lesser extent, of K1 are dependent on the lines chosen for measurement. The elements given in the Catalogue are derived from what Conti et al. term the `Group 1' emission lines (narrow emissions of Si IV, N IV and N III). Some absorption features which may be part of the secondary spectrum have been detected and measured. If these features do indeed originate in the secondary component, K2 approx 2*K1 and the W-R component is the more massive. System629Orbit1End System630Orbit1Begin The orbit was assumed circular, in agreement with the light-curve, and the epoch is the time of primary minimum. Since, however, the two minima are equal in depth (within the accuracy of existing observations) the term `primary' is somewhat arbitrary, but the time given is that of the eclipse of the apparently more massive star. The eclipsing nature of the system was discovered by E. Hertzsprung (Bull. Astron. Inst. Netherl., 2, 165, 1924). Photographic light-curves were also published by E. v.d. Hoven van Genderen (Bull. Astron. Inst. Netherl., 9, No. 339, 1939) and S. Gaposchkin (Ann. Harv. Coll. Obs., 113, 69, 1953). No solution appears to have been made nor has a photoelectric light-curve been published. The secondary is of slightly later spectral type than the primary. The star is a member of the open cluster Collinder 228. System630Orbit1End System631Orbit1Begin These orbital elements are described as `approximate' by Walborn himself and should certainly be confirmed. The star is a member (possibly a blue straggler, see O.J. Eggen, Astrophys. J., 173, 63, 1972) of the cluster I.C. 2602. Walborn suggests its spectroscopic peculiarities may be related to its binary nature. System631Orbit1End System632Orbit1Begin The new observations by Swensen and McNamara agree with other recent observations by M. Grewing and T. Herczeg (Z. Astrophys., 64, 256, 1966) and older ones by W.A. Hiltner (Astrophys. J., 101, 108, 1945) in ruling out the large eccentricity found by J.A. Pearce (Publ. Astron. Soc. Pacific, 52, 287, 1940). The smaller eccentricity is in accord with the photometric evidence, although coincidentally Pearce found a period of apsidal motion not in conflict with the variations in times of minima. The observations show a large scatter, and some systematic departures from a Keplerian velocity curve. These facts may explain the large values found for the eccentricity by Pearce and they prevent a definitive determination of the orbital elements by any of the investigators cited. There is also an appreciable rotation effect. Pearce also measured features that he identified as the secondary spectrum and derived a mass-ratio of about 0.3. D.M. Popper (Publ. Astron. Soc. Pacific, 74, 129, 1962) believes that the D lines and H-alpha are double. The secondary spectrum is visible during primary eclipse. There is some possibility of variation in V0. The epoch is the time of primary minimum. Lucy & Sweeney adopt a circular orbit. R.H. Koch (Astron. J., 66, 230, 1961) described the difficulties he encountered in solving his precise BV light-curves, and several other investigators have since attempted to improve his solutions (e.g. B. Cester et al., Astron. Astrophys., 61, 469, 1977, who derived spectral types of B5 V and F9 III, V.A. Caracatsanis, Astrophys. Space Sci., 47, 375, 1977 and E.F. Guinan, Contr. Villanova Univ. Obs., No. 1, 1975). A completely new light-curve (in b and y) has been published by K. Oh and K. Chen (Astron. J., 89, 126, 1984). All investigators agree on an orbital inclination around 81 deg or 82 deg, but estimates of the fractional luminosity (in V) of the primary component range from 0.8 to 0.96. System632Orbit1End System633Orbit1Begin Epoch is T0. System633Orbit1End System634Orbit1Begin The star is a member of the cluster Trumpler 16 in the Carina nebula. The orbital elements of the primary component are reasonably well determined, but those of the secondary are relatively uncertain. The system is certainly massive but since eclipses appear to be unlikely it is hard to know exactly how massive the components are. A 9.2m companion at 18.7" is listed in I.D.S. System634Orbit1End System635Orbit1Begin The orbit is assumed circular, in accordance with the light-curve, and the epoch is the time of primary minimum. The system contains two single-lined spectroscopic binaries which are believed to revolve about their common centre of mass in about 25 years. Probably all members of the system are early-type stars and Leung et al. estimate the total mass of the system to be 90 MSol. Approximate orbital elements for the second close binary were derived by N.D. Morrison and P.S. Conti as follows: P=21.72d, T (inferior conjunction of brighter star)=J.D. 2,443,532.72, omega=126 deg, e=0.34, K1=48 km/s and V0=8 km/s. The observations by Leung et al. appear to confirm these elements. For the eclipsing pair, Leung et al. find an orbital inclination of 86 deg, and that the primary of that pair gives about three times as much light as the secondary. The whole multiple system is believed to belong to the cluster Collinder 228. System635Orbit1End System636Orbit1Begin This star is in the H II region associated with eta Car. Although the scatter of the observations is fairly large, the coverage of the velocity curve of the primary is good. On the other hand, the secondary spectrum is seen on only a few plates and both its spectral type and the value of K2 are relatively uncertain. There may be some interference from gaseous streams, but it is not considered to be serious by Thackeray and Emerson. Eclipses are unlikely. System636Orbit1End System637Orbit1Begin The two stars in this system are closely similar and apparently evolved. The epoch is the time of primary minimum. H.E. Jorgensen and K. Gyldenkerne (Astron. Astrophys., 44, 343, 1975) published uvby observations of the light-curve, but had difficulty deciding which minimum was produced by an occultation. G. Giuricin et al. (Astron. Astrophys., 85, 259, 1980) find that primary minimum is an occultation, which leads them to adopt an orbital inclination close to 83 deg and a fractional luminosity (in y) for the brighter star of 0.65. System637Orbit1End System638Orbit1Begin The Durchmusterung number is from the C.P.D. No precise spectral classification is given for this star, but its spectrum is said to resemble that of upsilon Sgr and, like the latter, it is a hydrogen-deficient star. The elements, including the period, are all provisional. The orbit is assumed circular and the epoch is the time of inferior conjunction of the primary star. Variations in light of the order of 0.1m in V, believed to be caused by radial pulsation, are discussed by P.W. Hill et al. (I.A.U. Colloq. No. 87, p. 245, 1986). Although the orbital period is uncertain, any value permitted by the observations gives this system the shortest known period for a hydrogen-deficient system. System638Orbit1End System639Orbit1Begin Rather surprisingly, no elements were published for this bright Am binary until preliminary elements were determined by T.F. Worek, W.R. Beardsley and M.W. King (Astron. J., 74, 375, 1969). Later H.A. Abt and S.G. Levy (Astrophys. J. Supp., 59, 229, 1985) published elements having apparently overlooked the earlier work, which they did not cite. They give spectral types of A2, A8 and F0 from the K line hydrogen lines and metallic lines respectively. There are few grounds for choosing between the elements given by Abt and Levy and the revised Allegheny values given in the Catalogue. The close agreement between the two sets merits the b classification. Worek et al. are probably correct in assuming a circular orbit (the epoch is T0). They estimate that the invisible secondary component is a K5 star. The star is the brightest component of A.D.S. 7942: companions are 11.5m at 27.3" and another faint star at 233". System639Orbit1End System640Orbit1Begin The magnitude given is on the v scale and is taken from L.F. Smith (Mon. Not. Roy. Astron. Soc., 138, 109, 1968). The orbit is assumed circular and the epoch is the time of superior conjunction of the O-type star. Elements of the W-R component (upper line) are derived from measures of the C IV lambda 4441 emission line. From the minimum mass of the O-type star, it is estimated that the orbital inclination is not less than 65 deg. The star is the first well-established example of a binary containing a WC star and an observable secondary component. System640Orbit1End System641Orbit1Begin Results of an earlier investigation were published by T.H. Parker (J. Roy. Astron. Soc. Can., 5, 377, 1911). W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 226, 1935) improved Parker's value for the period. Parker's observations were remeasured and new elements computed, and elements were computed from two series of Victoria observations. No changes were apparent, and the elements given in the catalogue are based on both the Victoria series. Any apsidal motion is too slow to be detected in the interval covered by the observations. System641Orbit1End System642Orbit1Begin The star is the brighter component of A.D.S. 7967: B is 8.73m at 35.2" and of spectral type G0 V. The two stars share a common proper motion; a few measurements of the radial-velocity of B give a mean value within 1.4 km/s of the systemic velocity of A. The physical association of the two stars appears very likely but is not proven. System642Orbit1End System643Orbit1Begin This RS CVn system displays emission at H-alpha and is the optical counterpart of the X-ray source 2A 1052 + 606. The orbit is assumed circular and the epoch is T0. System643Orbit1End System644Orbit1Begin The orbit is assumed circular, in accordance with the most recent light-curve, and the epoch is the time of primary minimum. Coverage of the velocity-curve is incomplete and the observations show a large scatter. Although D.J.K. O'Connell (Ric. Astron. Spec. Vatican, 7, 399, 1968) found evidence for apsidal motion from his photographic light-curve, photoelectric UBV light-curves obtained by S. Soderhjelm (Astron. Astrophys. Supp., 22, 263, 1975) indicate that the orbit is circular. Soderhjelm found an orbital inclination close to 81 deg and that the hotter (but smaller) star gives 0.31 of the total light in V. O'Connell identifies three companions of HH Car, of which the brightest is C.P.D. 58 deg 2840 (HH Car is C.P.D. 58 deg 2839) at 13" separation. Mandrini et al. find that this companion has a radial velocity close to the systemic velocity of the eclipsing pair. They hesitate, however, to suggest a physical association since the spectrum of C.P.D. 58 deg 2840 is that of an F-type giant, suggesting that the star is less massive and more evolved than the components of the close pair. System644Orbit1End System645Orbit1Begin These elements supersede the preliminary ones published by some of the same authors in I.A.U. Symp. No. 88, p. 177, 1980. The magnitude is on a narrow-band photoelectric scale (L.F. Smith, Mon. Not. Roy. Astron. Soc., 138, 109, 1968). The upper row gives elements derived from measures of the N V emission lines in the W-R spectrum, the lower row gives elements of the component displaying an absorption spectrum. The orbit is assumed circular and the epoch is the time of inferior conjunction of the O-type star. The orbital inclination is expected to be low (about 46 deg). The O-type star is probably of luminosity class V. System645Orbit1End System646Orbit1Begin This system is of interest since it is the central star of the planetary nebula DS 1 and the spectra of both components are visible. The light of the star varies by about half a magnitude in the same period as the radial velocity, and the variations can be represented by the reflection effect. The magnitude given is an approximate mean (see Drilling, Astrophys. J., 270, L13, 1983). No spectral types are given, but velocities of the less massive component are derived from measures of C III emission lines and those of the more massive are derived from He II absorption lines. The zero of phase is the time of maximum light, which is superior conjunction of the C III emission source. Although the mean velocity curves look fairly well defined, there are indications that the observations depart from them systematically at certain stages. The light-curve requires an orbital inclination certainly greater than 53 deg and probably around 72 deg. System646Orbit1End System647Orbit1Begin This star has been considered to be physically associated with alpha UMa (W.P. Bidelman, Publ. Astron. Soc. Pacific, 70, 168, 1958). Petrie considered that the systemic velocities and trigonometric parallaxes of the two systems did not support this view. Their angular separation is 6'. The systemic velocity of alpha UMa is still uncertain however. System647Orbit1End System648Orbit1Begin This system is A.D.S. 8035 with Delta m close to 3m. Underhill adopted the orbital elements by H.S. Jones and H.H. Furner (Mon. Not. Roy. Astron. Soc., 98, 92, 1937) with P=44.0y, T=1865.9. She also assumed their values of e and omega and derived K and V0 only. The orbital inclination is 161. deg. The visual orbit by W.D. Heintz (Munchen Veroff., 5, 247, 1963) is now considered superior to that by Jones and Furner although the predictions of the two orbits about radial velocities during the interval of observation are similar. C.D. Scarfe (Astrophys. Space Sci., 11, 112, 1971) has shown that the observed velocities do not agree well with either of these orbits, or even with that derived by P. Couteau (J. Observateurs, 42, 31, 1959). Visual observers are hampered by the very close approach of the two stars at periastron. This is just the time when the radial velocities will be able to give most information, but the next approach, according to Heintz' values of the elements will be about the year 2000. All elements should be considered uncertain until then. System648Orbit1End System649Orbit1Begin See note for HD 61936. System649Orbit1End System650Orbit1Begin This system belongs to the class of AM Her binaries. The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The values given for K1 and V0 are approximate means from the bases of the emission lines (hydrogen and ionized helium); the peaks give a somewhat lower value for K1. Spectroscopic observations have also been published by N.F. Voikhanskaya, (Astron. Zh., 63, 516, 1986). System650Orbit1End System651Orbit1Begin This is also an AM Her binary. Mukai and Charles have detected the sodium D-lines and (in emission) the infrared Ca II triplet, which features they ascribe to the secondary star, classified as dM5-6. The orbit is assumed circular and the epoch is defined as the time of the linear polarization pulse. The time of inferior conjunction of the secondary star is 0.98m (about 0.078d) later. System651Orbit1End System652Orbit1Begin See note for HD 61936. The star is the brighter component of A.D.S. 8055; companion is 11.5m at 3.1". System652Orbit1End System653Orbit1Begin Andersen's observations superseded those of H. Mauder (Astron. Astrophys., 4, 437, 1970) which were obtained at much lower dispersion. The secondary star is appreciably fainter than the primary, and only the lines lambda 3933 of Ca II, and lambda 4481 of Mg II were measured in the secondary spectrum. Great care was taken in the selection of lines for measurement to avoid lines in which the two component spectra were likely to be badly blended. The orbit was assumed circular and the epoch is the time of primary minimum. D.M. Popper (Publ. Astron. Soc. Pacific, 95, 757, 1983) has published results obtained from Lick observations. They are very similar to those given in the Catalogue and this justifies upgrading those to a quality. Photoelectric observations were obtained by H. Mauder and U. Kohler (Astron. Astrophys., 1, 147, 1969) and rediscussed by Mauder (loc. cit.). They show a range of variation of about 0.3m in B. The inclination is about 76 deg. Andersen finds Delta MV=1.37; the effective temperatures of the two stars are similar. System653Orbit1End System654Orbit1Begin System654Orbit1End System655Orbit1Begin This is a nova-like variable and the elements given in the Catalogue are derived from measures of the emission lines of He II. The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The period is only approximately known. The orbital inclination is likely to be in excess of 30 deg. System655Orbit1End System656Orbit1Begin System656Orbit1End System657Orbit1Begin Lucy & Sweeney adopt a circular orbit and find V0=3.4 km/s. This latter finding confirms the statement in the Sixth Catalogue that the value +2.9 km/s given in Heard's paper was a misprint. The spectrum is classified as A2 from the K line and A7 from the metallic lines. System657Orbit1End System658Orbit1Begin See note for HD 61936. System658Orbit1End System659Orbit1Begin See note for HD 61936. System659Orbit1End System660Orbit1Begin Griffin suggests that the invisible companion has a mass of the order of 0.1 MSol. System660Orbit1End System661Orbit1Begin The magnitude is a narrow-band photoelectric magnitude from L.F. Smith (Mon. Not. Roy. Astron. Soc., 138, 109, 1968). The orbit is assumed circular for the absorption-spectrum component, but a small (and presumably spurious) eccentricity fits the emission-line velocities better. The epoch is the time of inferior conjunction for the W-R star, but there are small phase displacements from one line to the next. The upper row gives elements derived from the C III and C IV emission lines, the lower those derived from hydrogen and helium absorption lines. The emission lines in the W-R spectrum give very different values for V0. If the O-type component has a mass normal for its spectral type, the orbital inclination is about 36 deg. System661Orbit1End System662Orbit1Begin The epoch is the time of primary minimum. The elements given are derived from measures of the helium lines and the small eccentricity probably should be neglected, especially since no value is given for omega. Measures of the hydrogen lines lead to the derivation of a more eccentric orbit and lower semi-amplitudes. No photoelectric light-curve is available; the system was shown to be eclipsing from photographic observations (S. Gaposchkin, Ann. Harv. Coll. Obs., 113, No. 2, 1953). System662Orbit1End System663Orbit1Begin The elements derived by Sahade and Cesco have been preferred although the solution was a graphical one and Lucy & Sweeney question the reality of the orbital eccentricity. R.F. Sanford (Astrophys. J., 86, 153, 1937) found a smaller value of K1. D.M. Popper, as quoted by A.G. Kulkarni and K.D. Abhyankar (J. Astrophys. Astron., 2, 119, 1981), has found preliminary values of K1=35 km/s and K2=130 km/s. Undoubtedly, Popper's study -- when it is published -- will supersede the others. The first observations of the D-line of the secondary spectrum were reported by E.W. Miller and D.H. McNamara, (Publ. Astron. Soc. Pacific, 75, 346, 1963) who also noted the presence of H-alpha in emission. Several emission-lines of non-stellar origin, in the ultraviolet, have been reported by M.J. Plavec (Bull. Am. Astron. Soc., 19, 708, 1987). These will probably turn out to be related to distortions in the velocity-curve found by Sahade and Cesco. Photoelectric UBV light-curves have been obtained and analyzed by Kulkarni and Abhyankar (op. cit.) and re-analyzed by J. Koul and K.D. Abhyankar (J. Astrophys. Astron., 3, 93, 1982) and P.B. Etzel (Bull. Am. Astron. Soc., 18, 976, 1986). Agreement between the various analyses is not fully satisfactory. The orbital inclination is well over 80 deg, the magnitude difference (Delta V) between components is between 1.0m and 1.5m. Spectral types are A0 V or A1 V and K1 III or G8 III. System663Orbit1End System664Orbit1Begin The paper cited gives only a table of the elements of this and other dwarf-novae systems and little is known about the observations on which the results are based. No epoch is given. Reference: W.Wargau \& N.Vogt, Mitt. A.G., 55, 77, 1982 System664Orbit1End System665Orbit1Begin This is another binary of the AM Her type and, at the time of discovery, had the shortest period of the known cataclysmic binaries. It is also the first AM Her binary known to eclipse. The epoch is the time of primary minimum and the orbit is assumed circular. The value given for K2 is a lower limit, derived from measures of the peaks of H-beta and H-gamma emission. This emission is believed to be associated with the secondary star (believed to be a late M-type dwarf) rather than with the white dwarf. The orbital inclination is estimated to be 76 deg. Results of IUE observations of this and other AM Her systems have been published by P. Szkody, J. Liebert and R.J. Panek (Astrophys. J., 293, 321, 1985). System665Orbit1End System666Orbit1Begin Wolff's discussion, the most recent, complements the earlier studies by H.A. Abt (Publ. Astron. Soc. Pacific, 65, 274, 1953) and H.A. Abt et al. (Astrophys. J., 153, 177, 1968). All these studies are in good agreement except for a possible slow change in the value of omega which, according to Wolff, is consistent with a period of apsidal rotation of about 700 years. Abt et al. were the only ones to derive K2 from relatively few plates. The value given is theirs, as is also the classification of the secondary spectrum. Eclipses have been looked for and not found, so the maximum inclination is about 81 deg. The visual magnitude difference is about 0.5m. The primary star is well known as an Ap star with strong lines of strontium in its spectrum, and as a magnetic variable with the same period as the orbital period. The star is the brightest member of A.D.S. 8115: B is 11.5m at 1.0", C is 9.8m at 57.2" and does not share the proper motion of A. System666Orbit1End System667Orbit1Begin These two stars are the components of the multiple star A.D.S. 8119. The element V0 is, in each case, the velocity of the centre of mass of the whole system as deduced from the motion of each component. The epoch given for HD 98230 is an arbitrary one. Visual orbits for the pair AB, and for the system HD 98231 have been computed by W.D. Heintz (Astron. Nachr., 289, 269, 1967). He finds i=86.3 deg for the latter pair. Berman computed the mass-ratio (0.77) and the total mass (2.63 MSol) of the pair AB (P=59.84y) from the spectroscopic observations available to him. The spectral types given are from a recent revision by B.W. Bopp (Publ. Astron. Soc. Pacific, 99, 38, 1987) who also resolves the puzzle of the lithium line (lambda 6708) being visible only in the spectrum of component A. System667Orbit1End System668Orbit1Begin These two stars are the components of the multiple star A.D.S. 8119. The element V0 is, in each case, the velocity of the centre of mass of the whole system as deduced from the motion of each component. The epoch given for HD 98230 is an arbitrary one. Visual orbits for the pair AB, and for the system HD 98231 have been computed by W.D. Heintz (Astron. Nachr., 289, 269, 1967). He finds i=86.3 deg for the latter pair. Berman computed the mass-ratio (0.77) and the total mass (2.63 MSol) of the pair AB (P=59.84y) from the spectroscopic observations available to him. The spectral types given are from a recent revision by B.W. Bopp (Publ. Astron. Soc. Pacific, 99, 38, 1987) who also resolves the puzzle of the lithium line (lambda 6708) being visible only in the spectrum of component A. Reference: W.H.v.d.Bos, Mem.Acad.R.Sc.Let.; Denmark; 8th Ser., 12, 295, 1928 System668Orbit1End System669Orbit1Begin Lloyd's discussion supersedes the only previous one by F. Henroteau (Pop. Astron., 27, 29, 1919). The two spectra are never completely resolved, but Lloyd was able to confirm that the period deduced by Henroteau is close to the correct value. Although a reliable value of K2 could not be derived, a mass-ratio of about 0.9 is indicated. The spectral type given in the Catalogue is from the Bright Star Catalogue; however Lloyd suggests both components have types in the range A5 to A9. The system is unusual in having an orbit of such high eccentricity with so short a period. Lloyd could find no evidence for apsidal motion. System669Orbit1End System670Orbit1Begin This system is one of those in which an extremely accurate (X-ray) pulsar orbit is matched with a highly uncertain orbit for the optical component. Even the spectral type is only approximate. The very small orbital eccentricity indicated by the X-ray observations (G. Fabbiano and E.J. Schreier Astrophys. J., 214, 235, 1977) is negligible as far as the optical observations are concerned. Thus the orbit is assumed circular and the epoch is the time of mid-eclipse. The upper row gives the value of K1 derived from the observed a sin i (determined from the pulse period) the lower row gives elements derived from the He II lines (considered the most reliable by Hutchings et al.). The quality rating refers to the X-ray orbit. The orbit of the optical component is also discussed by M. Mouchet, S.A. Ilovaisky and C. Chevalier (Astron. Astrophys., 90, 113, 1980) and a model of the system is discussed by T.S. Kruzina and A.M. Cherepashchuk (Astron. Zh., 63, 494, 1986). S.S. Holt et al. (Astrophys. J., 227, 563, 1979) give an account of Ariel observations. System670Orbit1End System671Orbit1Begin This is a visual binary (A.D.S. 8148) with a period of 192 y, in which the companion is 2.7m fainter than the primary. The visual orbit has been derived by P. Baize (J. Observateurs, 35, 73, 1952) and his values of P, T, e, and omega were assumed. The quality classification refers only to the elements K and V0. Although the velocity variation is consistent with that expected, the scatter of individual observations is approximately equal to the derived value of K, and some caution in accepting the elements appears desirable. System671Orbit1End System672Orbit1Begin Another cataclysmic variable for which only an incomplete statement of the orbital elements has been published, without sudegcient description of the observations to enable an assessment to be made. No epoch is specified; a circular orbit appears to have been assumed. The value of K is a lower limit, and no value is given for V0. Reference: W.Wargau \& N.Vogt, Mitt. A.G., 55, 77, 1982 System672Orbit1End System673Orbit1Begin Except for some preliminary measurements by B. Paczynski (Astron. J., 69, 124, 1964) these are the first radial-velocity measurements of this W UMa system, and the only ones to show the secondary spectrum. The orbit is assumed circular. The epoch is the time of primary minimum as deduced from McLean's table of observations. R.E. Wilson and E.J. Devinney (Astrophys. J., 182, 539, 1973) find an orbital inclination of 79 deg and that the brighter component gives 0.92 of the total (blue) light. A 9.0m companion at 67" is listed in I.D.S. System673Orbit1End System674Orbit1Begin Lucy & Sweeney adopt a circular orbit. System674Orbit1End System675Orbit1Begin This spectroscopic triple system contains the visual pair A.D.S. 8189 which is not resolved on the spectrograph slit at Victoria. The original orbit by Petrie and Laidler is preferred to the later one by R.M. Petrie and A.H. Batten (Publ. Dom. Astrophys. Obs., 13, 383, 1969) because the latter study is based on observations over several years during which the observed velocities were effected by the variations arising from the visual orbit. Petrie and Batten found somewhat lower and less accurate values of K1 and K2 than did Petrie and Laidler. Unfortunately the variation found for the velocities of the components of the visual orbit are not in good agreement with the predictions made from that orbit. The maximum velocity difference for the visual pair is about 6 km/s.the expected difference was closer to 12 km/s. They found, for the visual components, that Delta m=0.48. System675Orbit1End System676Orbit1Begin Double lines were first discovered in this spectrum by D.M. Popper (Astron. J., 71, 175, 1966). Observations of this system are rather few, concentrated at the nodes, and show a fairly large scatter as would be expected from the spectral type. The secondary spectrum is described as somewhat later than the primary. The orbit was assumed circular and the epoch is the time of primary minimum. Note the different values found for V0 of each component. Andersen and Gronbech also published photometric observations: the eclipse is about 0.55m deep in the Stromgren b colour, and the value of b-y hardly changes through the orbital cycle. They find i=76 deg and the primary star gives 0.64 of the total light. A new analysis, by R.E. Wilson and J.B. Rafert (Astrophys. Space Sci., 76, 23, 1981), did not substantially change these results. System676Orbit1End System677Orbit1Begin This is the brighter component of A.D.S. 8242. Component B is 0.2m fainter than A, of similar spectral type, and separated from it by about 2". The stars probably are physically connected. The spectrum of A shows emission at H and K and in the Balmer lines. The emission at H-alpha is variable, and on account of this and of the general similarity of the system to YY Gem and CC Eri, Bopp and Fekel predict that the primary component will be subject to flares. They estimate i<=56 deg. System677Orbit1End System678Orbit1Begin This appears to have been amongst the first of the barium stars discovered to be a spectroscopic binary. System678Orbit1End System679Orbit1Begin The elements given are derived from measurements of the broad wings of the emission lines. The narrow peaks give a similar velocity-curve about 230 deg out of phase. The orbit is assumed circular and the epoch is the time of superior conjunction of the (broad) emission-line source. The spectrum of the secondary has not been detected. Shafter and Szkody place upper limits of 0.19 MSol and 0.4 MSol on the masses of the red and the white dwarfs, respectively. System679Orbit1End System680Orbit1Begin Fainter member A.D.S. 8250: A is 6.4m at 9.7" and is H.D. 101177. Several other more distant components are listed in I.D.S. System680Orbit1End System681Orbit1Begin Lucy & Sweeney adopt a circular orbit. System681Orbit1End System682Orbit1Begin Epoch is T0 : orbit assumed circular. Emission lines of Ca II are associated with the star in front at primary minimum. From measures of these lines K2=72 km/s. H. Shapley (Princeton Obs. Contr., No. 3, 1915) found from the light-curve i=81 deg and the light ratio to be about 0.6. System682Orbit1End System683Orbit1Begin This is an infrared source and Humphreys proposes that it consists of an A-type star surrounded by a shell (in which the dominant supergiant F-type spectrum arises) which is fed by a proposed M-type star that has filled its Roche lobe. The Ca II lines (H and K) give velocities that vary with the same period as those derived from the other lines but in a different phase (not 180 deg out of phase). These are supposed to arise from the stream from the M-type star to the A-type one. The epoch is an arbitrary zero. The observed velocities are still only few in number and the binary nature of this object is still conjectural. System683Orbit1End System684Orbit1Begin The magnitudes given for this W UMa system are approximate V magnitudes estimated from the data given by Sistero and Castore de Sistero in another paper (Astrophys. J., 78, 413, 1973). The orbit was assumed circular and the epoch is the time of primary minimum. Orbital elements and the values given in the Catalogue are a mean for all lines. Note the different values of V0 for each component. The orbital inclination is found to be close to 79 deg and the primary star contributes 0.81 of the total light in V. System684Orbit1End System685Orbit1Begin The secondary star appears to be similar in type to the primary, but much fainter. A few isolated measurements have been made of the secondary spectrum, but no reliable value of K2 could be deduced. The spectroscopic and photometric values of e do not agree; thus it is difficult to know whether or not the spectroscopic orbit confirms the apsidal motion indicated by photometry. The only photometric study so far is by D.J.K. O'Connell (Publ. Riverview College Obs., 2, 5, 1939). A photoelectric light-curve and spectrographic observations at higher dispersion would be very useful. System685Orbit1End System686Orbit1Begin This star is in the field of I.C. 2944 and Gieseking studied it by his objective-prism method (See note for HD 61936). He assumed a circular orbit and the epoch is T0. The value of V0 is only relative to standards in the field. System686Orbit1End System687Orbit1Begin Epoch is T0. R.S. Dugan (Princeton Obs. Contr., No. 2, 1912) found from the light-curve that i=85.7 deg. This was confirmed by H.N. Russell and H. Shapley (Astrophys. J., 39, 405, 1914) who also found the light-ratio to be about 0.13. System687Orbit1End System688Orbit1Begin See the note for H.D. 102010. All the same comments apply, except there is a possibility that the real orbit of this star is eccentric. System688Orbit1End System689Orbit1Begin This is the orbit of the visible component of a system that contains an X-ray pulsar (pulse period 297 sec.). The magnitude and spectral type are taken from R.H. Densham and P.A. Charles (Mon. Not. Roy. Astron. Soc., 201, 171, 1982). The period found by Hutchings et al. is within the limits set by Densham and Charles, but is still uncertain. A period of 12.081d is possible but would require an appreciable eccentricity (0.45) considered physically implausible. At periods near 10.75d, both circular and elliptical orbits are possible, and either fits the observations equally well. In the solution given in the Catalogue, a circular orbit was assumed and the epoch is T0. Derivation of an orbit for the X-ray source from accurate timing of pulses is made difficult by the (presumably fortuitous) presence of another pulsing X-ray source, with a very similar period, nearby in the sky. System689Orbit1End System690Orbit1Begin The new observations supersede the only previous orbit determination by J.B. Cannon (J. Roy. Astron. Soc. Can., 4, 455, 1910). The spectral types are as given in the Bright Star Catalogue; Batten et al. suggest A6 V + G8 III IV and H.A. Abt (private communication) puts the secondary as early as F8. Preliminary solutions showed the orbital eccentricity to be negligibly small and the orbit was assumed circular. The epoch is T0. There may be small systematic errors in V0, because of the nature of the composite spectrum. S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) published six velocity measurements that agree well with the new orbital elements, except for a small systematic difference in velocity. His value of 71.6918d for the period is also in good agreement with that of Batten et al. The velocities of the A-type component were obtained by subtracting a standard G-type spectrum from the observed composite and cross-correlating the residual with spectra of Vega. A systematic difference in V0 was found for the two components. The B magnitude difference is estimated as 0.36m, the A-star being the brighter. Recently, K.G. Strassmeier, S. Weichinger and A. Hanslmeier (Inf. Bull. Var. Stars, No. 2937, 1986) estimate Delta V=0.43m, the G-star being the brighter. The system is an X-ray source; probably the G-star is the origin of this radiation (F.M. Walter, Publ. Astron. Soc. Pacific, 97, 643, 1985). A small light variation observed by D.S. Hall et al. (Inf. Bull. Var. Stars, No. 1798, 1980) is not caused by eclipses. If the A-type star lies on the main-sequence, an orbital inclination of 50 deg --55 deg is indicated. The system is sometimes grouped with the RS CVn stars, partly because of the light- variation reported by Hall et al. and partly because of H and K emission reported by A. Young and A. Koniges (Astrophys. J., 211, 836, 1977). Batten et al. have questioned the reality of the emission and the combination of an evolved star with an A-type main-sequence object is rather different from what is usually found in RS CVn systems. A 9 m companion at 74.3" is listed in I.D.S. A limited number of radial-velocity measures of this companion does not rule out the possibility of a physical association with the spectroscopic pair. System690Orbit1End System691Orbit1Begin Lucy & Sweeney adopt a circular orbit. Curchod and Hauck give the spectral type as A2, A7 and F3 from the K line, hydrogen lines and metallic lines respectively. System691Orbit1End System692Orbit1Begin Other elements were published by G.A. Shajn (Izv. Krym. Astrofiz. Obs., 4, 148, 1949). His values agree quite well with Harper's except for the eccentricity for which he finds about twice Harper's value. Lucy & Sweeney, using Harper's observations, obtain e=0.089, which they accept as a real eccentricity. System692Orbit1End System693Orbit1Begin The spectral type given is assigned by P.C. Keenan (Bull. Inf. Centre Don. St., 24, 19, 1983) who actually gave K0 III CN-0.5. Other authorities give a luminosity class IV. The elements given are derived only from observations made at Haute Provence. Three earlier Mount Wilson observations, if there is no systematic difference between them and the others, require a period of 490.6 days, without much change in the other elements. Ginestet et al. believe that part of the discrepancy between the Mount Wilson and Haute Provence observations may be that they require a different V0, because of motion of the close pair about a third body. H.A. McAlister et al. (Astrophys. J. Supp., 51, 309, 1983) report a companion resolved by speckle interferometry (at rho=0.17") and also note that an occultation companion has been observed. Ginestet et al. argue that this companion cannot be the secondary star and is, therefore, a third body. System693Orbit1End System694Orbit1Begin The two shallow eclipses of this binary are nearly equal in depth and the two spectra are closely similar. The designation of a `primary' minimum is thus somewhat arbitrary; the epoch given corresponds to the middle of the eclipse of the somewhat less massive star. A circular orbit was assumed, even though the light-curve indicates a small non-zero value of e cos omega. Neglect of this will not affect the semi-amplitudes of the velocity-curve, but may be partly responsible for the difference found between the values of V0 for each component. Analysis of the B light-curve (J.M. Garcia and A. Gimenez, Astrophys. Space Sci., 125, 181, 1986) is made difficult by the close visual companions. The eclipsing system belongs to A.D.S. 8347; companions are B (8.5m at 0.3"), C (8.3m at 3.7") and D (6.5m at 63.1"). Only the last of these is photometrically innocuous. Popper has shown that the eclipsing binary must be A, since he could prevent the light of C from entering the spectrograph slit, and if B were the close pair, the spectral lines would be at least triple. The total effect of B and C on the light-curve is, however, very uncertain, since the magnitude estimate of B, at least, is also uncertain. The orbital inclination probably lies between 74 deg and 85 deg. System694Orbit1End System695Orbit1Begin Struve and Morgan did not give an explicit value for K2, but they did give values for the mass-ratio, and for (m_1+m_2)sin^3i which lead to msin^3i=1.05 MSol and m2sin^3i=0.75 MSol. Petrie(II) attempted to measure Delta m, and could not confirm the existence of the secondary spectrum. The system should probably be regarded as a single-spectrum system. A companion is listed in I.D.S. at 90" separation. All other stars in the field have much greater separations than this. System695Orbit1End System696Orbit1Begin The orbit is assumed circular and the epoch is the time of primary minimum. The system has both resemblances to and differences from cataclysmic variables and there has been much debate about its nature. Opinion seems to be settling that it contains a white dwarf and an M-type dwarf. Other important papers about the system are: D.H. Ferguson et al. (Astrophys. J., 251, 205, 1981 -- discovery of its nature), H. Ando, A. Okazaki and S. Nishimura (Publ. Astron. Soc. Japan, 34, 141, 1982 -- photometry) J.B. Hutchings and A.P. Cowley (Publ. Astron. Soc. Pacific, 97, 328, 1985 -- UV spectroscopy) and D.H. Ferguson et al. (Astrophys. J., 316, 399, 1987 -- most recent general discussion). System696Orbit1End System697Orbit1Begin Epoch is T0. System697Orbit1End System698Orbit1Begin An earlier investigation by J.B. Cannon (Publ. Dom. Obs., 4, 125, 1917) was based on an incorrect value for the period. Petrie(II) found Delta m=1.24. System698Orbit1End System699Orbit1Begin The observations by Hill and Barnes supersede those by R.F. Sanford (Astrophys. J., 79, 89, 1934) with which the former are in quite good accord. Rotational broadening makes spectral classification difficult and the secondary cannot be seen at all, even during primary minimum. Maximum and minimum magnitudes given are only approximate. The distortion and variability of the light-curve make it difficult to analyze. Observations have been published by L. Binnendijk (Astron. J., 74, 1024, 1969), C. Blanco and F. Catalano (Mem. Soc. Astron. Ital., 41, 343, 1970) and P.G. Niarchos (Astron. Astrophys. Supp., 61, 313, 1985). Re-analyses of some of these have been published by S.R. Jabbar and Z. Kopal (Astrophys. Space Sci., 92, 99, 1981) and J. Ka lu _ zny (Acta Astron., 36, 121, 1986). There is a considerable range in the results, but the orbital inclination is probably close to 80 deg and the fractional luminosity of the brighter component (in V) about 0.85. System699Orbit1End System700Orbit1Begin The epoch is T0. A circular orbit was assumed after solutions for an elliptical one had shown the eccentricity to be very small (about 0.02). Slightly different values of T0 are found for each component. The one given is for the primary. Bolton et al. make a rough estimate of Delta B=0.5m for the magnitude difference. System700Orbit1End System701Orbit1Begin These elements agree well with those found by J. Lunt (Cape Annals, 10, pt. 7, 14G, 1924). Lunt did not measure the secondary spectrum. A 13.8m companion at 4.5" is listed in I.D.S. System701Orbit1End System702Orbit1Begin Epoch is T0.orbit assumed circular. System702Orbit1End System703Orbit1Begin The orbit is assumed circular and the epoch is the time of primary minimum. The elements derived depend on rather few observations at a dispersion of 30 A/mm -- hence the d classification. The values of K1 and K2 are unlikely to be much changed, however, by subsequent work. In the same paper, ubvy photometric observations are presented and analyzed. The orbital inclination is found to be close to 80 deg and the magnitude difference between the components is Delta V=0.93m. The system is probably a member of the cluster N.G.C. 4103. Identification is from the Cape Photographic Durchmusterung. System703Orbit1End System704Orbit1Begin Griffin believes that the spectral type is later than the one he quotes (given by Upgren). The small eccentricity is barely significant. Griffin estimates that the probability that the true orbit is circular is less than ten percent. System704Orbit1End System705Orbit1Begin Harper later revised P to 462.8d and T to J.D. 2,424,665.79 (Publ. Dom. Astrophys. Obs., 6, 227, 1935). System705Orbit1End System706Orbit1Begin No M-K type is available but Griffin concludes from unpublished photometry that the star is a giant. System706Orbit1End System707Orbit1Begin Epoch is T0. Different lines yield velocities which may lead to different elements. The hydrogen-line velocities are made nugatory by the emission features. D.J.K. O'Connell (Riverview Publ., 1, 33, 1935) found from the light-curve that i is between 75 deg and 80 deg. He also found a light-ratio of about 0.8, but Woolf reports the spectrum of only one stellar component. A brief report on the UV spectrum of this star has been published by W. Strupat (Mitt. Astron. Gesells., 62, 275, 1984). System707Orbit1End System708Orbit1Begin The epoch is the time of primary minimum which, together with the period, was taken from the light-curve published by S. Rucinski (Publ. Astron. Soc. Pacific, 88, 777, 1976). From these UBV observations, Rucinski deduced an orbital inclination of 90 deg. The primary minimum is deeper by 0.1m in V. The light-curve shows the orbit to be circular. The same observations were also discussed by P.G. Niarchos (Astrophys. Space Sci., 58, 311, 1978). The star may be a member of the Coma cluster (Mel 111). System708Orbit1End System709Orbit1Begin The magnitude of this star is variable, since the star is a Cepheid; the orbital motion has had to be separated from the pulsational variations in velocity. The orbit should probably be assumed to be circular. System709Orbit1End System710Orbit1Begin Epoch is T0. Orbital elements have also been published by E.V. Woitkevitch-Okulitch (Pulkovo Bull., No. 94, 1924) and by Luyten. H.A. Abt (Astrophys. J. Supp., 6, 37, 1961) has published observations which lead to the following revisions: P=1.2709934d, K1=69.8 km/s, V0=2.2 km/s. The discrepancy in the values of K1 should be investigated. Abt classifies the spectrum as A5, F2, F5 IV according to K line, hydrogen lines and metallic lines, respectively. System710Orbit1End System711Orbit1Begin This is a dwarf nova for which only very approximate elements are given. (Both K1 and K2 lie in the range 60 km/s to 120 km/s). No epoch has been given. Reference: W.Wargau & N.Vogt, Mitt. A.G., 55, 77, 1982 System711Orbit1End System712Orbit1Begin This spectroscopic binary is A.D.S. 8470B. The component A is H.D. 106365 (6.9m, K2 III) and, separated by 26.7", has a common proper motion with B. The systemic velocity of B is close to the mean velocity of A. Griffin argues that the difference of 1.1 km/s may be partly caused by differential gravitational red-shifts and does not signify a real difference of radial velocities. Reports by G.A. Bakos (Astron. J., 79, 866, 1974) that the velocity of A is also variable are as yet unconfirmed. There is also a component C, 14.0m and 2.7" from B, which probably shares the proper motion and radial velocity of the whole system. According to O.J. Eggen (Astron. J., 68, 483, 1968) the system may belong to the `61 Cyg group'. This conclusion is questioned by Griffin since the spectroscopic evidence suggests a distance of about 100 pc for the system. System712Orbit1End System713Orbit1Begin The epoch is T0. The magnitudes given are estimates of the visual magnitude, but this system is well-known for the variability of its light-curve. K. Kalchaev (Trudy Astrophys. Inst. Kazakstan, 17, 18, 1971) and G.A. Bakos (Veroff. Remeis-Sternw. Bamberg, 9, No. 100, 293, 1971) attempt to explain the variability in terms of gas streams. Several photometric investigations have been published since the Seventh Catalogue (P.G. Niarchos, Astrophys. Space Sci., 58, 301, 1978, Astron. Astrophys. Supp., 53, 13, 1983; R.W. Hilditch, Mon. Not. Roy. Astron. Soc., 196, 305, 1981; S.B. Jabbar and Z. Kopal, Astrophys. Space Sci., 92, 99, 1983; L. Binnendijk, Publ. Astron. Soc. Pacific, 96, 646, 1984 and J. Kaluzny, Acta Astron., 34, 217, 1984). Agreement between the many solutions is not good, but probably the orbital inclination is around 80 deg and the fractional luminosity of the larger star is around 0.8. Several photometric investigators draw attention to the need for a modern velocity-curve. The star is an obvious candidate for observation and measurement by cross-correlation techniques. The star is the brighter member of A.D.S. 8472; companion is 13.1m at 1.3". System713Orbit1End System714Orbit1Begin This was listed without any other designation as No. 352 in the Sixth Catalogue. The orbit given there was derived by S. Gaposchkin (Astron. J., 67, 360, 1962) from spectroscopic observations by J.L. Greenstein. Gaposchkin's interpretation of the system as a normal B-type binary led to a large distance for the star both from the Sun and from the plane of the Galaxy. J. Smak (Acta Astron., 19, 165, 1969) was the first to suggest that a period less than one day might fit the observations better than Gaposchkin's value for the period did, and remove some of the difficulties of interpretation. New photometric observations by Young et al. and further spectroscopic observations by Greenstein that they discussed, have confirmed Smak's suggestion. The epoch is a time close to, but not coincident with, the deeper minimum of light. The primary star appears to be a very old Population I subdwarf, or even possibly a member of the halo Population II. The epoch is the time of the deeper minimum. The spectral type is not well defined. The magnitude at maximum is well determined on the V scale, that at minimum is roughly estimated from data given by Young et al. The coverage of the velocity-curve is now fairly good, but there are still some large residuals. New photometric and spectrophotometric observations have been published by A. Young and S.T. Wentworth (Publ. Astron. Soc. Pacific, 94, 815, 1982) who find that the invisible companion is a white dwarf and that no mass is being transferred in the system at present. System714Orbit1End System715Orbit1Begin The spectral type is an estimate based on the photometric colours and some other considerations; it is not obtained by normal M-K methods of classification. System715Orbit1End System716Orbit1Begin The new orbital elements supersede those obtained by W.H. Christie (Astrophys. J., 83, 433, 1936) with which they are in reasonable agreement. System716Orbit1End System717Orbit1Begin The magnitude given is on the VE scale (O.J. Eggen and J.L. Greenstein, Astrophys. J., 141, 83, 1965). The spectral type of the red-dwarf secondary is only approximate. The orbital elements are derived from measures of the H-alpha emission line in the M-type spectrum. The epoch is the time of inferior conjunction of the M-type star: the orbit was found to be circular. Eclipses have been looked for, but not found. The spectrum not measured is that of a white dwarf. If the red dwarf is assumed to have a mass of 0.39 MSol and a radius of 0.5 RSol, the upper limit to the orbital inclination is 72 deg and the lower limit to the white-dwarf mass is 0.43 MSol. Although the star is optically coincident with the Ursa Major cluster, its proper motion and radial velocity proclaim that it is not a member. System717Orbit1End System718Orbit1Begin The elements given in the Catalogue supersede those derived from Harper's earlier study (Astrophys. J., 27, 160, 1908) and those found by N. Ichinohe (Astrophys. J., 26, 282, 1907). A peculiar velocity-curve derived by Ichinohe for the secondary component was not confirmed by Harper. Harper suggests the period should be revised to 71.8d. Petrie(II) found Delta m=0.36. System718Orbit1End System719Orbit1Begin The short-period velocity variation found by Fehrenbach (Ann. Astrophys., 11, 35, 1948) seems to be spurious. In a later investigation by G.H. Herbig and B.A. Turner (Astrophys. J., 118, 477, 1953) the secondary spectrum was detected. The mass-ratio was found to be about 0.5, and the spectral types were given as G0 III-IV and A3 V. Star is the brightest component of A.D.S. 8530: companions are 11.8m at 35" and 8.3m at 65.2". System719Orbit1End System720Orbit1Begin The eccentricity, although small, is significant. The star's spectroscopic parallax and systemic velocity show it not to be a member of the Coma cluster, although it is in the same direction. System720Orbit1End System721Orbit1Begin The elements given in the Catalogue agree well with those found by R.F. Sanford (Astrophys. J., 56, 452, 1922). The value of K2 is only an estimate, but since Sanford found K2=74 km/s, it cannot be far wrong. Emission is observed in the Ca II lines of both components. The light of the system is slightly variable. Greenstein, Hack and Struve find Delta m=0.9 from their spectrophotometry. There are indications that the metal abundance in this system is lower than in the Sun. System721Orbit1End System722Orbit1Begin System722Orbit1End System723Orbit1Begin The values of K1 and K2 are lower limits; no value is given for V0 or for the epoch. The star is a dwarf nova and the elements can serve at best as a rough indication of the properties of the system. Reference: W.Wargau \& N.Vogt, Mitt. A.G., 55, 77, 1982 System723Orbit1End System724Orbit1Begin This is another binary X-ray pulsar. The measured quantity is a sin i, K1 being deduced from that, while V0 is unknown. Since the X-ray pulses can be accurately timed, the orbit of the X-ray source is well determined, despite a fairly large gap in the `velocity-curve'. The spectral type and magnitude given are those of the optical counterpart (Wray 977). An earlier X-ray orbit, based on nearly the same period, was published by N.E. White and J.H. Swank (Astrophys. J., 287, 856, 1984). It agrees closely with that given in the Catalogue. Earlier work, cited in the papers mentioned there, was based on incorrect values for the period. Attempts to determine the orbital elements of the optical component have been less successful, since the spectrum shows many of the phenomena associated with mass loss and accurate measurement is difficult. J.B. Hutchings et al. (Publ. Astron. Soc. Pacific, 94, 541, 1982) completed their paper before the 41.5d period was found, although they discussed this possible period in an addendum. They found that lines of silicon, oxygen and nitrogen yielded velocities opposite in phase to the motion of the X-ray source, with K2 in the range 14 km/s to 18 km/s. Observations of the visible spectrum were also published by H. Mauder, M. Ammann and E. Schulz (Mitt. Astron. Gesells., 43, 227, 1978). They, too, were hampered by ignorance of the correct period and found a value of K2 around 20 km/s. System724Orbit1End System725Orbit1Begin The first to recognize this star as a spectroscopic binary was F.J. Neubauer (Lick Obs. Bull., 15, 190, 1932), who suggested a period of 0.98d. A.D. Thackeray and G. Hill (Mon. Not. Roy. Astron. Soc., 168, 55, 1974) showed that the true period is much longer. The new observations, near velocity maximum, have permitted improvements to P, K1 and V0 and reductions in the uncertainties of these elements. Thackeray and Wegner believe their velocity measurements are unaffected by contamination with the light of alpha 2 Cru, 4.4" away and magnitude 2.09. The two stars have a common proper motion but different radial velocities. Neubauer believed that alpha 2 Cru was also a spectroscopic binary. Thackeray and Hill believed that it had a constant velocity. Thackeray and Wegner, however, inclined again to the belief that alpha 2 Cru may be a spectroscopic binary since otherwise the velocity discrepancy is hard to explain for a presumably physical pair. The new value of V0 strengthens the case for regarding alpha_1 Cru as a member of the Sco{Cen association. System725Orbit1End System726Orbit1Begin Harper (Publ. Dom. Astrophys. Obs., 6, 230, 1935) later revised the period to 11.788d. Objective-prism results derived by Ch. Fehrenbach (Ann. Astrophys., 11, 35, 1948) agree well with those given here. Both sets of observations have been discussed by R. Pretre (Ann. Obs. Toulouse, 29, 27, 1963). Lucy & Sweeney adopt a circular orbit. System726Orbit1End System727Orbit1Begin The spectral class is A5 from the K line and F2 from the metal lines. A magnetic field was found by H.W. Babcock (Astrophys. J. Supp., 3, 141, 1958) but not subsequently confirmed. The star forms a common-proper-motion pair (A.D.S. 8658) with the bright Ap star (V=5.29) H.D. 108662, from which it is separated by 145". Aitken also lists a faint component C separated by 1.7" from B. System727Orbit1End System728Orbit1Begin This is the first set of spectroscopic orbital elements determined for this W UMa system. The velocities were determined by cross-correlation and one node of the velocity-curve is well covered. Only a few observations define the other node, however. The period and epoch (time of primary minimum) appear to be those given in the third edition of the G.C.V.S. A circular orbit was assumed. E.F. Milone et al. (Astrophys. J. Supp., 43, 339, 1980) have published UBV observations, along with a detailed summary of earlier work. Their full analysis of the asymmetric light-curves is, however, dependent on the velocity-curves and is still awaited. System728Orbit1End System729Orbit1Begin Despite the rather limited coverage of the velocity-curve, the observations and results of McLean and Hilditch are probably to be preferred to those of O. Struve and L. Gratton (Astrophys. J., 108, 497, 1948). The period and epoch (time of primary minimum) are taken from the fourth edition of the G.C.V.S. The orbit is assumed circular. Synthetic light-curve solutions for this system have been published by L. Binnendijk (Vistas in Astron., 21, 359, 1977) who finds an orbital inclination of about 86 deg and a fractional luminosity (in yellow light) for the larger star of about 0.7. The light-curve is variable; earlier solutions were published by P. Broglia (Contr. Oss. Astron. Milano-Merate, No. 165, 1960) and R.E. Wilson and E.J. Devinney (Astrophys. J., 182, 539, 1973) who obtained results similar to Binnendijk's. System729Orbit1End System730Orbit1Begin Star is fainter component of A.D.S. 8600: A is 5.7m at 20.2". Petrie(II) found Delta m=0.55. Curchod and Hauck give the spectral type as A5, A7 and F2 from the K line, hydrogen lines and metallic lines, respectively. The spectral types given in the Seventh Catalogue appear to have been erroneous. System730Orbit1End System731Orbit1Begin The epoch is the time of primary minimum and the orbit is assumed circular in accordance with the light-curve. The new orbit by McFarlane et al. supersedes that determined by O. Struve and L. Gratton (Astrophys. J., 108, 497, 1948) because of both the quality of the new observations and the detection, with their aid, of the secondary spectrum. The paper by McFarlane et al. also contains UVBRI photometric observations, which probably likewise supersede the only other photoelectric observations published by K.D. Abhyankar et al. (Astron. Astrophys. Supp., 13, 101, 1973). McFarlane et al. find that the system is not quite in contact and derive an orbital inclination close to 86 deg. The luminosity ratio depends on whether the primary component is in radiative or convective equilibrium and is at least 6.1 in V. System731Orbit1End System732Orbit1Begin System732Orbit1End System733Orbit1Begin There are discrepancies in published values for both the V magnitude and the spectral type. The choice of V magnitude is somewhat arbitrary (the other value is 0.1m brighter) but the evidence seems to favour the G8 spectral type given, rather than the alternative G3. One observation suggests the possibility of a variable V0. System733Orbit1End System734Orbit1Begin Two components of A.D.S. 8627: separation 5.4". A third component at 59" from A has magnitude 10.5m. System734Orbit1End System735Orbit1Begin System735Orbit1End System736Orbit1Begin Probably a member of the Coma cluster. Lucy & Sweeney confirm the reality of the small eccentricity. The spectrum is A3, A8 and F0 from the K line, the hydrogen lines and the metallic lines, respectively. Reference: G.A.Shajn, Pulkovo Circ.,, No. 21; 35, 1937 System736Orbit1End System737Orbit1Begin Petrie(I) found Delta m=0.11. System737Orbit1End System738Orbit1Begin The orbital elements determined for this Wolf-Rayet binary (also known as MR 42) are described by the authors themselves as preliminary. Another brief account of the system is given by V.S. Niemela (I.A.U. Symp. No. 88, p. 177, 1980). The epoch is the time of inferior conjunction of the star with the absorption-line spectrum. The orbit is assumed circular. The elements given for the orbit of the Wolf-Rayet (upper row) star are derived from measures of the N V line at lambda 4603, which give a smaller semi-amplitude and a lower scatter than those of any other emission line in the spectrum. The minimum mass of this system is high, but eclipses have not yet been reported. System738Orbit1End System739Orbit1Begin Garcia regards this as a symbiotic star, there being also an early-type component in the spectrum. J.W. Fried (Astron. Astrophys., 88, 141, 1980) believed that the binary period was 70.8d and found K1=9.8km/s (late-type component). Garcia finds that his observations cannot be harmonized with this period, although he cannot rule out a period of 205 d. Neither orbit is very convincing. No epoch is given by Garcia; that in the Catalogue is the time of the lowest observed velocity. Neither does Garcia specify V0, although his diagram of the velocity-curve suggests that it is close to zero. The binary nature of this object cannot be regarded as established beyond all doubt. System739Orbit1End System740Orbit1Begin Richardson and McKellar found Delta m=0.03, using Petrie's method. System740Orbit1End System741Orbit1Begin Epoch is T0. Orbital elements were determined by J.B. Cannon (Publ. Dom. Obs., 2, 269, 1915). His value of K1 (40.99 km/s) was appreciably lower than that found by Bertiau. W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 230, 1935) revised Cannon's value of the period, and questioned the reality of the secondary spectrum measured by Cannon. He did not change the other elements. Bertiau could not detect the secondary spectrum, but suspected some effect of its continuum. H.A. Abt (Astrophys. J. Supp., 6, 37, 1961) confirms Bertiau's elements, except for a small change in V0. He gives P=38.3240c. He gives the spectral type as A6, F2, F6 IV according to the K line, the hydrogen lines and the metallic lines, respectively. Petrie(II) was able to measure the lines of the secondary component, and found Delta m=0.43. Lucy & Sweeney accept the eccentricity as real. System741Orbit1End System742Orbit1Begin No epoch is specified. The orbital elements are derived from measurements of the wings of the Balmer emission lines in the spectrum of this dwarf nova. The value of K1 has been slightly increased to compensate for the effects of exposure time. The orbital inclination is estimated at around 70 deg. System742Orbit1End System743Orbit1Begin Epoch was fixed in order to determine the orbital elements. The masses, however, should be fairly well determined. Petrie(II) found Delta m=0.49. Star is fainter component of A.D.S. 8682: A is 5.3m at 21.6". System743Orbit1End System744Orbit1Begin Griffin claims that this system has the smallest known value of K1 determined spectroscopically (but see notes for Nos. 30, 785 and 1379). System744Orbit1End System745Orbit1Begin The new elements supersede those published by R. Margoni, M. Perinotto and E. Nasi (Mem. Soc. Astron. Ital., 40, 301, 1969) with which, nevertheless they are in quite good agreement, provided the identification of primary and secondary in the earlier paper is switched (the components are nearly equal). The H.D. number given by Worek et al. is a misprint. The spectrum is A2 from the K line and F0 from the metal lines. The epoch is T0 and the orbit was assumed circular after the small eccentricity of the preliminary solution was shown to be not significant. The difference in V0 between the new elements and the old is probably the effect of systematic differences between observatories. The star is the brightest member of A.D.S. 8710; companions 7.9m at 3.7" and 10.4m at 124.1". Both are probably optical, but Worek et al. argue that a physical association between A and B cannot be entirely ruled out. Their relative motion could be orbital and they find the spectrum of B to be F5-7 V-IV, so that the expected Delta m falls within the range of observational uncertainty. Unfortunately, radial-velocity measurements of B are affected by scattered light from A. System745Orbit1End System746Orbit1Begin The elements are designated `provisional' by Christie. System746Orbit1End System747Orbit1Begin Epoch is time of primary minimum. Period is variable. Light-curve and partial solution are given by S. Gaposchkin (Ann. Harv. Coll. Obs., 113, 69, 1953). System747Orbit1End System748Orbit1Begin This is the first star of a group of seven spectroscopic binaries near the north galactic pole that have been studied by Latham et al. All the orbits have appreciable eccentricities, but the time of periastron passage (113.) is given as days elapsed from an epoch which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. The data published for three of the systems are not sudegcient to permit an assessment of the quality of the orbits, although to judge from the velocity-curves that are published, all the orbits are reliable. The values of V0 appear to have been referred to the I.A.U. system of standard velocities and are not just relative to the velocity of the standard used in cross-correlation. Two of the binaries show both spectra, but explicit values of K2 have not been published. The serial numbers are from the catalogue by D. Weistrop, which she first described in Astron. J., 77, 366, 1972. System748Orbit1End System749Orbit1Begin See note on Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (-4.5) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. System749Orbit1End System750Orbit1Begin A 9.5m companion at 25.1" is listed in I.D.S. System750Orbit1End System751Orbit1Begin This is the second brightest Wolf-Rayet star in the sky. An absorption component (classified as 09.5/B0 Iab by N. Houk and A.P. Cowley, Univ. Michigan Catalogue of Two Dimensional Spectral Types for the H.D. Stars, Vol. 1, 1975) has been recognized in the spectrum for some time, but this is the first determination of the orbit of the system. The orbital elements given for the W-R component (upper line) are based on measures of the emission line C IV lambda 5801/12. A still higher amplitude (and different phase) is obtained from the C III line at lambda 5696, which is probably more susceptible to perturbations in the upper atmosphere of the W-R component. The zero of phase is the time at which the W-R star is in front (the velocity derived from the C IV line is equal to the systemic velocity and increasing). The systemic velocity has not been directly determined and is arbitrarily assumed to be zero. The value of K2 (absorption lines) is an upper limit. Narrow-band photometry at lambda 4860 (near emission lines at lambda lambda 4650 and 4686) shows a small light-variation at the wavelengths of the emission lines consistent with an eclipse of the outer regions of the W-R atmosphere. The very large mass-ratio (K abs =KWR > 29) is exceptional for W-R systems and leads, with a reasonable assumption of 50 MSol for the mass of the O-type star, to i=36 deg and mWR<1.7 MSol. Moffat and Seggewiss discuss the evolutionary implications of these values, and suggest as an alternative that the actual spectroscopic-binary companion of the Wolf-Rayet star is invisible, and that the O-type spectrum arises from a relatively distant but unresolved third component. At present the only evidence for this interpretation is the unusually low mass found for the Wolf-Rayet star on the more obvious interpretation. The whole system does have a 7.5m visual companion at 5.3" separation. This companion possibly shares a common proper motion with the Wolf-Rayet binary. System751Orbit1End System752Orbit1Begin Epoch is T0 and a circular orbit was assumed. Orbital elements were also published by A.H. Joy (Astrophys. J., 72, 41, 1930) whose values of V0 and K1 agree well with Popper's but whose value of K2 is appreciably larger (99 km/s). Popper's result is based on the well resolved D lines and is certainly more reliable. The system is the prototype of a group containing late-type stars showing H and K emission in their spectra and often displaying variable light-curves, the characteristics of which are now commonly accepted as the results of spots on at least the cooler star of the pair. Most of the brighter (nearer) members of the group are also recognized as soft X-ray sources and intermittent radio sources. The best set of photoelectric light-curves remain those published by S. Catalano and M. Rodono (Mem. Soc. Astron. Ital., 38, 395, 1967) which show clearly the precessing wave typical of these systems. Those authors found an orbital inclination of 84 deg and fractional luminosity (at lambda 5150) of 0.27 for the star of earlier type. More recent analyses (J.A. Eaton and D.S. Hall, Astrophys. J., 227, 907, 1979 -- who discuss the starspot hypothesis at length -- and I.B. Pustylnik and L. Einasto, Astrophys. Space Sci., 105, 259, 1984) agree about the inclination but give somewhat different values for the fractional luminosities. The depth of eclipse varies: the minimum magnitude in the Catalogue is an estimate based on the work of Catalano and Rodono and the out-of-eclipse magnitude given by R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 79, 101, 1975). Although no new orbit has been published since the Seventh Catalogue, a number of spectrophotometric studies have been made. C.G. Rhombs and J.D. Fix (Acta Astron., 26, 301, 1976) studied the continuum flux distribution at phases affected by the wave in the light-curve and found that it resembled that of the cooler star. The same authors also found the ultraviolet excess to be associated with the cooler star (Astrophys. J., 216, 503, 1977). S.A. Naftilan and S.A. Drake (Publ. Astron. Soc. Pacific, 92, 675, 1980) failed to find, from limited data, any correlation between emission-line strengths and phase, except that H-alpha appears stronger during primary eclipse. Emission-line variations were also studied by E.J. Weiler (Mon. Not. Roy. Astron. Soc., 182, 77, 1978). System752Orbit1End System753Orbit1Begin See note for Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (1.4) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. System753Orbit1End System754Orbit1Begin See note for Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (-28.0) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. System754Orbit1End System755Orbit1Begin Lucy & Sweeney adopt a circular orbit. System755Orbit1End System756Orbit1Begin See note for Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (-1.1) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. This is one of the two-spectra systems. Latham et al. say that the two semi-amplitudes are approximately equal. System756Orbit1End System757Orbit1Begin See note for Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (0.4) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. This is the other two-spectra system. The value of K2 is approximately 30 percent larger than that of K1. System757Orbit1End System758Orbit1Begin See note for Weistrop 33436 [SB9 system 748]. The time of periastron passage is given as days elapsed from an epoch (65.0) which does not seem to match the first observation and the Julian Date cannot be recovered from the published information. System758Orbit1End System759Orbit1Begin The original observations were by O. Struve (Astrophys. J., 106, 92, 1947) but the computation by Lucy & Sweeney is preferred to Struve's graphical solution. The epoch is T0. The magnitudes and spectral type are taken from the fourth edition of the G.C.V.S. M.B. Shapley analyzed a photographic light-curve (Harvard Obs. Bull., No. 848, 32, 1927) and found i=86 deg and the light-ratio to be about 0.03. System759Orbit1End System760Orbit1Begin Griffin discusses the uncertainty surrounding the spectral type and concludes that the dG6 classification by Joy is the best available. He also draws attention to the large proper motion. System760Orbit1End System761Orbit1Begin The star has a fainter companion, distant about 35" from the spectroscopic pair. Both proper motion and radial velocity indicate that this companion is optical. System761Orbit1End System762Orbit1Begin The peculiarity of this spectrum is a strong enhancement of the lines of Co II. Because the observations show a somewhat larger-than-expected scatter, Dworetsky suggests that the star may be pulsating in a short period. System762Orbit1End System763Orbit1Begin The relatively large mass-function leads Griffin to suggest that the invisible secondary is itself a close pair of G-type dwarfs, otherwise, its spectrum should be visible. System763Orbit1End System764Orbit1Begin In addition to those given in the Catalogue, orbital elements have been published by: H.C. Vogel (Astrophys. J., 13, 328, 1901); H. Ludendorff (Astron. Nachr., 180, 276, 1909); L. Hadley (Publ. Michigan Obs., 2, 76, 1915); A. Hnatek (Astron. Nachr., 209, 48, 1919); C.U. Cesco (Astrophys. J., 104, 287, 1946) and G. de Strobel (Asiago Contr. No. 20, 1950). There are also discussions by A. Krancj (Publ. Bologna Univ. Obs., 7, No. 11, 1959), and H.N. Russell (quoted by F.G. Pease in Publ. Astron. Soc. Pacific, 39, 313, 1927). Russell combined spectroscopic and interferometric data and found i=60 deg. These several determinations are in good agreement with each other, especially those by Hadley, Cesco, de Strobel, and Fehrenbach and Prevot. There is some evidence for a variation in V0, but it would be necessary to check the wavelengths used before investigating this. Petrie(I) found Delta m=0.03. Spectral type is taken from Bright Star Catalogue. Star is brighter component of A.D.S. 8891: companion is 3.95m at about 14". (see HD 116657 B). System764Orbit1End System765Orbit1Begin Although the star has been known to be variable in velocity for some time, orbital elements were not published for it until H.A. Abt published his investigation of Am binary stars (Astrophys. J. Supp., 6, 37, 1961). His value of the period, however, was twice the correct one. Gutmann found no evidence for any change in V0, such as was suspected by W.R. Beardsley (Astron. J., 69, 532, 1964). The spectral types given by Abt were A2, A8 and A7 from the K line, the hydrogen lines and the metallic lines, respectively. The star is A.D.S. 8891 B. System765Orbit1End System766Orbit1Begin Very thorough studies of the spectroscopic orbit, interferometric orbit and light variations by the same group have greatly improved our knowledge of this system (see R.R. Shobbrook et al., Mon. Not. Roy. Astron. Soc., 145, 131, 1969 and D. Herbison-Evans et al., ibid., 151, 161, 1971). Apsidal motion is found with a period of about 130 years (the value of omega for 1969 is given in the Catalogue). Light variations of about 0.14m, once thought to indicate shallow eclipses, seem, rather, to be a combination of ellipticity effects and pulsations of the beta CMa type. There is a 4-hour periodicity in both the light-curve and the velocity-curve as well as the 4-day one. Short-term changes in the line profiles have recently been studied by G.A.H. Walker et al. (Publ. Astron. Soc. Pacific, 94, 143, 1982). These variations may help to account for some of the differences between values found for K1, K2 and V0 in this investigation and in earlier ones (R.H. Baker, Publ. Allegheny Obs., 1, 65, 1909; O. Struve and E.G. Ebbighausen, Astrophys. J., 80, 365, 1934; O. Struve Astrophys. J., 128, 310, 1958). Estimates of the magnitude difference between the components range from 1.49m (Petrie(II)) to about 2m (Herbison-Evans et al.) if an old determination of 2.4m by Struve is discounted. Herbison-Evans et al. also find an orbital inclination of about 66 deg and a distance of 84 parsecs (+/-4 parsecs). I. Fejes (Astron. J., 79, 25, 1974) finds evidence for a deficiency of neutral hydrogen in the direction of Spica (from 21-cm observations) and other evidence for anomalous interstellar abundances in that direction is provided by D.G. York and B.F. Kinahan (Astrophys. J., 228, 127, 1979), who studied ultraviolet interstellar lines. R.J. Reynolds (Astron. J., 90, 92, 1985) has discovered an extended H II region around the star. The UV spectrum of Spica itself has been studied by W.H. Bruce, G.H. Mount and P.D. Feldman (Astrophys. J., 227, 884, 1979), T.J. Herczeg, Y. Kondo and K.A. van der Hucht (Astrophys. Space Sci., 46, 379, 1977) and J.B. Hutchings and G. Hill (Astron. Astrophys. Supp., 42, 135, 1980). System766Orbit1End System767Orbit1Begin Struve, Cesco, and Sahade doubt the significance of the spectroscopic value of e. They comment on the low masses that seem to be implied by these elements. C. Payne-Gaposchkin (Astrophys. J., 100, 186, 1944) has analyzed the light-curve and finds i=77 deg. She also estimates Delta m=1.3. The spectrum may be Am, but is not listed by Curchod and Hauck. System767Orbit1End System768Orbit1Begin The epoch is the time of primary minimum and the orbit is assumed circular. This eclipsing binary was once thought to be a member of the globular cluster omega Cen, but determination of the binary's orbit has clearly shown the system to be a foreground object. Two solutions of the light-curve give rather different results. R.F. Sistero (Inf. Bull. Var. Stars, No. 316, 1968) finds an inclination of 72 deg and a fractional luminosity (photographic) for the brighter component of 0.77. A.I. Kaskambas (Astrophys. Space Sci., 64, 427, 1979) finds 77 deg and 0.6 respectively. This latter solution might suggest that both spectra should be visible, whereas only one is observed. System768Orbit1End System769Orbit1Begin The spectral type given is from the H.D. Catalogue. On the basis of unpublished photometry and the small proper motion, Griffin suggests that the type should be G8 III. System769Orbit1End System770Orbit1Begin The eclipsing nature of this variable was first discovered by F.H. Schmidt and J.D. Fernie (Inf. Bull. Var. Stars, No. 2527, 1984) who also published a diagram of the velocity-curve. The magnitude given is on the Stromgren y scale; the minimum magnitude is approximate. The epoch is the time of primary minimum. The velocity-curve is fairly well defined, but not Keplerian. Distortion of the primary star and asymmetric light-distribution over it ensure that the measured velocity is not that of the centre of mass. The semi-amplitude has been corrected (observed value 31 km/s) to allow for this fact. The stars are not in contact but Mochnacki et al. suggest that the system will become an A-type W UMa system. The orbital inclination is about 72 deg, the masses are estimated to be 1.9 MSol (visible star) and 0.3 MSol. According to I.D.S., there is a visual companion 13.1m at 22.8". System770Orbit1End System771Orbit1Begin The magnitudes for this dwarf nova cover the range of mean values given by N. Vogt and J. Breysacher (Astrophys. J., 235, 945, 1980) who also published a preliminary velocity curve. The epoch is T0 for the absorption-line component. A circular orbit was assumed. The velocity-curve of the absorption-line component is reasonably well determined; the value of K given for the white dwarf (lower line) is the mean of measures of the emission lines of H-gamma and H-delta. The orbital inclination is estimated at around 62 deg; at most the system displays grazing eclipses. System771Orbit1End System772Orbit1Begin The epoch is the approximate date of the first observation, which happens to be about the time of inferior conjunction of the M-type giant. No value is given for V0 -- it probably lies between 35 km/s and 40 km/s. From IUE observations, M. Kafatos, A.G. Michalitsianos and R.W. Hobbs (Astrophys. J., 240, 114, 1980) deduce that the hot companion is the central star of a planetary nebula. System772Orbit1End System773Orbit1Begin These elements supersede those published earlier by Harper (Publ. Dom. Obs., 4, 232, 1918). Luyten had pointed out that Harper's earlier work was based on an incorrect value for the period. Elements have also been published by P. Bourgeois (Bull. Astron. Roy. Obs. Uccle, 2, 222, 1938). He found a slightly larger value of e and a smaller value of K1 than did Harper. Lucy & Sweeney adopt a circular orbit. P.S. Conti (Astrophys. J., 149, 629, 1967) refined Harper's value of the period and measured K2, from the calcium emission lines, as 34.2 km/s +/-5.0 km/s. This would give a mass ratio of 0.28 and very small minimum masses. From these data and from infrared colours published by H.L. Johnson et al. (Comm. Lunar & Planetary Lab., 4, 99, 1966) Conti deduces that the system is an Algol-type system seen at very low inclination. System773Orbit1End System774Orbit1Begin Two different techniques of spectroscopy with high time-resolution have been applied to this system and the results of either one would clearly supersede the work of O. Struve (Astrophys. J., 108, 153, 1948). The other investigation is by A.W. Shafter (Astron. J., 89, 1555, 1984). Unfortunately, the increase in precision has shown that the `elements' (K1 and V0) are variable: Schlegel et al. found different values in the years 1981 and 1982. They also find line-to-line differences that Shafter suggests arise from the unreliability of some of the weaker lines. The 1981 value of K1 is preferred because it is closer to Shafter's. The very large difference in V0 found by the two sets of investigators is presumably partly a consequence of different techniques of measurement. The epoch is the time of primary minimum (O. Mandel, Peremm. Zvezdy, 15, 474, 1965). Shafter gives a time of superior conjunction of the secondary of J.D. 2,445,376.973. Spectroscopic observations with the 6-m telescope are reported by N.F. Voikhanskaya (Pis. Astron. Zh., 11, 617, 1985). The high-speed photometry by B. Warner and R.E. Nather (Mon. Not. Roy. Astron. Soc., 159, 427, 1972) and R.E. Nather and E.L. Robinson (Astrophys. J., 190, 637, 1974) demonstrated flickering with a period of approximately 29 seconds. Optical and infrared light-curves have been obtained by J. Frank et al. (Mon. Not. Roy. Astron. Soc., 195, 505, 1981) who find an orbital inclination of 65 deg and estimate an M2 V spectral type for the fainter star. The V magnitudes given in the Catalogue are approximations derived from their plot of the light-curve. System774Orbit1End System775Orbit1Begin System775Orbit1End System776Orbit1Begin Later spectrograms measured by A.J. Deutsch (Astrophys. J., 101, 377, 1945) tend to confirm these elements. Deutsch detected traces of a secondary spectrum of type about K5. M.B. Shapley (Harvard Obs. Bull., No. 797, 1924) found from the photographic light-curve that i=79.1 deg and the light-ratio is about 0.94. Lucy & Sweeney adopt a circular orbit. System776Orbit1End System777Orbit1Begin The scatter is larger than the semi-amplitude. System777Orbit1End System778Orbit1Begin Lucy & Sweeney also adopt an elliptical orbit. System778Orbit1End System779Orbit1Begin Reference: G.A.Shajn, Pulkovo Circ.,, No. 25; 26, 1939 System779Orbit1End System780Orbit1Begin Petrie(II) found Delta m=0.60. System780Orbit1End System781Orbit1Begin The original observations were by O. Struve and L. Gratton (Astrophys. J., 108, 498, 1948) but an incorrect photometric period misled these investigators into believing that the spectroscopically brighter component was eclipsed at secondary minimum. Kwee derived the correct period, removed the anomaly and improved the fit of the radial-velocity observations. The epoch is the time of primary minimum. Two discussions of photoelectric light-curves have now appeared (G. Russo and C. Sollazzo. Astrophys. Space Sci., 78, 141, 1981; A.D. Mallama and A.N. Witt, Acta Astron., 26, 253, 1976). The orbital inclination is at least 85 deg and the hotter component gives about 0.97 of the total light in B and V. Assuming the primary spectral type is A2 V, Mallama and Witt estimate the secondary to be about G3. System781Orbit1End System782Orbit1Begin New observations and analyses (B.N. Ashoka, R. Surendiranath and N. Kameswara Rao, Acta Astron., 35, 395, 1985; H. Levato et al., Astrophys. J. Supp., 64, 487, 1987) do not seem to yield results preferable to those of the analysis by Lucy & Sweeney of observations by R.E. Wilson (Lick Obs. Bull., 8, 130, 1914). The epoch is T0. System782Orbit1End System783Orbit1Begin Preliminary elements for this system containing two nearly equally evolved giants were published by D.M. Popper (Astrophys. J., 169, 549, 1971). Since the publication of the Seventh Catalogue, a full photometric study of the system has appeared (B. Gronbech, K. Gyldenkerne and H.E. Jorgensen, Astron. Astrophys., 55, 401, 1977). The larger star in the pair is brighter, but cooler, and was designated `component 2' by Andersen. The two spectra are similar, but component 2 has the stronger spectrum. The epoch is the time of primary minimum. The orbital inclination is close to 88 deg and the difference in magnitude is Delta V=0.38m. The relative positions of the two stars in the H-R diagram are not consistent with evolutionary-model calculations. See also M. Kitamura and Y. Nakamura (Ann. Tokyo Obs., 21, 311, 1987) for a discussion of gravity-darkening coedegcients in this system. System783Orbit1End System784Orbit1Begin The epoch is the time of primary minimum and, together with the period, is taken from the photometric study by L. Winkler (Astron. J., 82, 648, 1977). There is evidence that the period is increasing (N.S. Awadalla and A. Yamasaki, Astrophys. Space Sci., 107, 347, 1984). The light-curve shows the orbit to be circular, but the few observations are concentrated at the nodes and show a rather large scatter. Awadalla and Yamasaki have studied all available photoelectric light-curves (including new ones of their own) and find, by assuming the spectroscopic mass-ratio, an orbital inclination close to 70 deg and a fractional luminosity of about 0.2 (in V) for the fainter component. Somewhat different results are given by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978). System784Orbit1End System785Orbit1Begin The photoelectric radial-velocity observations are of high precision and the period is probably established. The low amplitude, however, makes it difficult to be sure that the other elements are well determined. System785Orbit1End System786Orbit1Begin The fainter component of 3 Cen (A is 4.56m at about 8") but, apart from common membership in the Sco{Cen group the two stars are probably not related. Levato et al. could not see the phosphorous lines previously reported in the spectrum. System786Orbit1End System787Orbit1Begin This binary has only recently been studied and the paper on spectroscopic work is complemented by one on photometric observations (M.A. Cerruti and R.F. Sistero, Publ. Astron. Soc. Pacific, 94, 189, 1982). The magnitudes, although on the V scale, are approximate. The orbit is circular. The epoch is the time of primary minimum (there is a difference between the two papers in this respect; we have assumed the value given in the spectroscopic study is correct). The spectroscopic elements are described by the authors themselves as `preliminary'. There are signs of systematic deviations from the velocity- curve. The orbital inclination is found to be close to 65 deg and the fractional luminosity (in V) of the larger component is 0.55. System787Orbit1End System788Orbit1Begin System788Orbit1End System789Orbit1Begin This is a triple system containing a short-period eclipsing binary. The spectrum of the secondary of the eclipsing pair is not seen. The A-type star is apparently a main-sequence object and is the primary of the eclipsing pair. The epoch given for the short-period orbit is T0. The orbit was assumed to be circular. Fekel's unpublished elements for the long-period orbit represent a considerable improvement on those published by Schoffel and Popper. E. Schoffel (Astron. Astrophys., 61, 107, 1977) has published UBV light-curves. He finds i is close to 84 deg and the G8 star contributes about 0.66 and the A star about 0.3 of the total light in V. System789Orbit1End System790Orbit1Begin This is a triple system containing a short-period eclipsing binary. The spectrum of the secondary of the eclipsing pair is not seen. The A-type star is apparently a main-sequence object and is the primary of the eclipsing pair. The epoch given for the short-period orbit is T0. The orbit was assumed to be circular. Fekel's unpublished elements for the long-period orbit represent a considerable improvement on those published by Schoffel and Popper. E. Schoffel (Astron. Astrophys., 61, 107, 1977) has published UBV light-curves. He finds i is close to 84 deg and the G8 star contributes about 0.66 and the A star about 0.3 of the total light in V. Reference: F.C.Fekel,,,, (Unpublished) System790Orbit1End System791Orbit1Begin Companion to 4 Cen. Elements described as `very marginal' by Levato et al., who also supply the magnitude and spectral classification. System791Orbit1End System792Orbit1Begin Levato et al. improved the orbital period originally derived, with the other elements, by G.F. Paddock (Lick Obs. Bull., 9, 42, 1916). The star belongs to the Sco{Cen group and has a visual companion at 14.9" (see HD 121263). Identification is from the Cordoba Durchmusterung. System792Orbit1End System793Orbit1Begin Orbital elements were published by A.C. Maury (Pop. Astron., 29, 636, 1921) and her values of P, e and omega were assumed by Popper. He estimated Delta m=0.5, from spectrophotometric measures. System793Orbit1End System794Orbit1Begin Earlier spectroscopic studies were published by W.E. Harper (J. Roy. Astron. Soc. Can., 4, 191, 1910 and Publ. Dom. Astrophys. Obs., 6, 232, 1935) and E. Bianchi (Mem. Soc. Astron. Ital., 1, (N.S.) 31, 1920). New observations by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976) confirm Bertiau's results. An astrometric orbit by Z. Daniel and K. Burns (Publ. Am. Astron. Soc., 9, 146, 1938) gives i=73 deg. A faint distant companion is listed in I.D.S., but its motion suggests that there is no physical connection between it and eta Boo. System794Orbit1End System795Orbit1Begin The combined photometric and spectroscopic study by Popper supersedes earlier work by G.A. Shajn (Izv. Krym. Astrofiz. Obs., 5, 105, 1950) and by E.D. Miner and D.H. McNamara (Publ. Astron. Soc. Pacific, 75, 343, 1963) as well as a rediscussion of data by B. Cester et al. (Astron. Astrophys. Supp., 32, 347, 1978). The light-curve shows the orbit to be circular and the epoch is the time of primary minimum. The two components are indistinguishable photometrically (Delta m=0) although one is about 3 percent more massive. The orbital inclination is 88.4 deg. The magnitude at maximum is taken from R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 79, 101, 1975) and the eclipse depth from the fourth edition of the G.C.V.S. System795Orbit1End System796Orbit1Begin System796Orbit1End System797Orbit1Begin According to R.H. Koch (Astron. J., 72, 411, 1967) the photometric colours suggest a slightly earlier spectral type (F8) for the primary star. The epoch is the time of primary minimum and the orbit was assumed circular. The spectrograms on which the orbit is based are of very low dispersion and a modern study of the system is desirable. Differences between photometric observations by M. Kitamura, T. Nakamura and C. Takahashi (Publ. Astron. Soc. Japan, 9, 191, 1957) and by Koch (loc. cit.) have led to several reanalyses (G. Giuricin, F. Mardirossian and M. Mezzetti, Astron. Astrophys. Supp., 39, 255, 1980; R.E. Wilson and J.B. Rafert, ibid., 42, 195, 1980). R.A. Botsula, Peremm. Zvezdy, 20, 577, 1978 and M. Hoffman (Astron. Astrophys. Supp., 47, 561, 1982) have found that the light-curve is variable, the latter suggesting that the system is related to the RS CVn group. G. Giuricin et al. (Mon. Not. Roy. Astron. Soc., 206, 305, 1984) reconsidered their earlier work and find an orbital inclination close to 88 deg and a fractional luminosity (at lambda 5125) of 0.68 for the hotter star. System797Orbit1End System798Orbit1Begin New observations do not confirm the period of 1025 d proposed by W.H. Christie (Astrophys. J., 83, 433, 1936). These new elements still require confirmation. System798Orbit1End System799Orbit1Begin This is an astrometric binary (major semi-axis of photocentric orbit approx 0.1") that is also a single-spectrum spectroscopic binary. The elements given are those derived from radial velocities alone, although Kamper also offers a combined solution from radial-velocity and astrometric measures. The period is 9.907y and the time of periastron passage 1952.03. The orbital inclination (from the combined measures) is 93.5 deg. The parallax is about 0.06". System799Orbit1End System800Orbit1Begin Earlier investigations were published by W.E. Harper (J. Roy. Astron. Soc. Can., 1, 237, 1907 and Publ. Dom. Astrophys. Obs., 6, 232, 1935) by J.S. Plaskett (Report of Chief Astronomer, Canada, p. 103, 1907) and by J.A. Pearce (Publ. Dom. Astrophys. Obs., 10, 331, 1956). Elst and Nelles call attention to inconsistencies between the various sets of observations used by Pearce. In particular, the Ottawa observations lead to a different V0 (Ottawa radial-velocity measures are known to be subject to systematic errors) and a smaller K1. The Yerkes and Lick observations were combined with the new material to give K1, e and omega, while V0 and T are derived from the new observations alone. The results are an undoubted improvement on Pearce's solution, but we still hesitate to give an a classification. System800Orbit1End System801Orbit1Begin Epoch is primary minimum and the orbit is assumed circular. Although no new spectroscopic work has been published, two good photometric studies have appeared since the Seventh Catalogue. They are by R.L. Walker and C.R. Chambliss (Astron. J., 88, 535, 1983) and J. Andersen, J.V. Clausen and B. Nordstrom (Astron. Astrophys., 137, 281, 1984). They lead to similar pictures of the system, the chief differences being that Walker and Chambliss give the spectral types as F6-7 IV-V and make one component slightly brighter than the other, while Andersen et al. treat the components as virtually indistinguishable. The magnitudes given are from the paper by Chambliss and Walker. The orbital inclination is very close to 90 deg. The masses are now very well-known; Andersen et al. suggest that the components are near the end of their main-sequence life. System801Orbit1End System802Orbit1Begin The epoch is the time of minimum light and the orbit is assumed circular. The object is a cataclysmic variable of the AM Her class. The observations on which this study is based were made with the Anglo-Australian telescope and at the South African Astronomical Observatory. The elements given are those derived from measurements of the narrow emission components as observed with the Anglo-Australian telescope. The emission lines show complex profiles and different components give quite different elements. In general, the values of K1 determined at each observatory are similar for each component, but the values of V0 tend to differ. Although velocity-curves derived from individual components are better covered than for many cataclysmic variables, doubt remains about their interpretation. System802Orbit1End System803Orbit1Begin A 9.2m companion at about 62" is listed in I.D.S. System803Orbit1End System804Orbit1Begin The new observations confirm the results of W.E. Harper (Publ. Dom. Obs., 1, 303, 1916) and are an undoubted improvement on them. The only significant difference between the two sets of elements is in the value of K2. Harper found 72 km/s, but indicated that the true value was probably lower. Petrie(I) found Delta m=0.51. System804Orbit1End System805Orbit1Begin Epoch is T0. System805Orbit1End System806Orbit1Begin The new observations supersede the earlier ones of R.K. Young (Publ. Dom. Astrophys. Obs., 4, 27, 1927) and show that the period is about 30 days longer than his value. Nevertheless, the other elements are not greatly altered. System806Orbit1End System807Orbit1Begin These elements are described as preliminary by Bakos himself. Although the semi-amplitude is relatively small, it is more than twenty times its mean error. The star is the fainter component of A.D.S. 9173: the brighter is 4.54m at 13.3" whose proper motion is similar but not identical. System807Orbit1End System808Orbit1Begin This is the first spectroscopic orbit for this W UMa system and demonstrates the power of the cross-correlation method of radial-velocity measurement. Coverage of the primary curve is good, but there are some systematic departures from it which may be partly due to the distortion of the component. The orbit is assumed circular and the epoch is the time of primary minimum. Several photometric observers have been attracted to the system and several analyses of the available light- curves have been published. Among the most recent are S.J. Lafta and J.F. Grainger, Astrophys. Space Sci., 127, 153, 1986, P.G. Niarchos, ibid., 58, 301, 1978 and S.W. Mochnacki and N.A. Doughty, Mon. Not. Roy. Astron. Soc., 156, 243, 1972. The orbital inclination is about 79 deg. The photometric and spectroscopic estimates of mass-ratio agree. System808Orbit1End System809Orbit1Begin The period in the binary orbit is 4.4 years, however the star is, also a magnetic variable with a period of 9.2954d, and some velocity variation with this period may be contributing to the scatter of the observations. The peculiarities of the spectrum consist in the variable strength of the lines of Eu II and Cr II which vary with the period of the magnetic field. System809Orbit1End System810Orbit1Begin Harper later revised the period to 7.3683d (Publ. Dom. Astrophys. Obs., 6, 233, 1935). The spectrum is classified as A2 from the K line and F2 III from the metal lines. System810Orbit1End System811Orbit1Begin An earlier investigation by A. Colacevich (Oss. e Mem. Arcetri, 59, 15, 1941) was based on a period of 206.9d. Abt has shown this to be incorrect, but his own elements are preliminary. He regards even the period as approximate. Epoch is T0. The light of the system has been suspected to be variable. Petrie(II) found Delta m=0.14. According to Abt, the spectral types derived from the K line, the hydrogen lines, and the metallic lines are A2, A8 and A7 respectively. System811Orbit1End System812Orbit1Begin New observations largely confirm the orbital elements found by R.K. Young (Publ. Dom. Obs., 3, 95, 1915). They lead to a slight improvement in the period, and a very considerable improvement in the precision with which the elements are known. System812Orbit1End System813Orbit1Begin The formal errors are very small, but only eleven observations are available. The system is of interest in that its period is short and it contains two closely similar early A-type stars that rotate slowly and yet are apparently not Am stars. A 12.0m companion at 22" is listed in I.D.S. System813Orbit1End System814Orbit1Begin New observations with IUE supplement those previously published by G. Wallerstein and S.C. Wolff (Publ. Astron. Soc. Pacific, 78, 390, 1966) and greatly strengthen the determination of the orbital elements of the subdwarf component. The amplitude of the G-type component is still poorly known because of the large scatter in the measured velocities (the spectral lines are much broadened by rotation). Howarth estimates the mass-ratio (O-type star.G-type star) to be 0.59+/-0.24, compared with 1.0+/-0.1 by Wallerstein and Wolff. This would make the subdwarf less massive than the 4.3 MSol proposed by the latter authors. Although both Howard and Wallerstein and Wolff suggest that the system may display eclipses, the only photometric search so far has not revealed any (J.D. Fernie, J. Roy. Astron. Soc. Can., 60, 260, 1966). J. Gruschinska et al. (Astron. Astrophys., 121, 85, 1983) published an analysis of the atmospheric structure of the subdwarf. System814Orbit1End System815Orbit1Begin The magnitudes given refer to alpha 1 and alpha 2 Cen individually. The period of 81.18y or 29,652 d, together with the values of T, e and omega, are based on a visual orbit by A.W. Roberts (Astron. Nachr., 139, 10, 1896). We have retained them, instead of adopting a more modern orbit, since they are the values Lunt used in deriving K1 and V0 (he estimated K1=K2). The orbit quality refers to these spectroscopic elements. The visual orbit is by now well-known and modern solutions differ primarily from this one in giving a shorter period (see W.D. Heintz, Observatory, 102, 42, 1982, who gives P=79.92y and discusses the relative value of astrometric and spectroscopic determinations of the mass-ratio. It is to be regretted that there is not a systematic high-precision study of the radial velocities of the two bright components of this system. Of the values given for omega, that of 232 deg refers to the orbit of the fainter relative to the brighter. Other spectroscopic observations were made by W.H. Wright (Lick Obs. Bull., 3, 3, 1904 and Publ. Lick Obs., 9, 238, 1907), H. Jones (determination of mean velocity only -- Cape Annals, 10, pt. 8, 116, 1928) and A.J. Wesselink (Mon. Not. Roy. Astron. Soc., 113, 505, 1953). Wesselink found V0=22.7 km/s, m2/m1=0.4 (compared with 0.82 from meridian observations, but see Heintz, loc. cit.) and pi=0.776". Two recent spectrophotometric studies of these bright stars have been published by D.R. Soderblom (Astron. Astrophys., 158, 273, 1986) and G. Smith, B. Edvardsson and U. Frisk (ibid., 165, 126, 1986). System815Orbit1End System816Orbit1Begin A periodic variation of about 0.25m in V is thought to be caused by eclipses (G. Jackisch, Inf. Bull. Var. Stars, No. 314, 1968 and A.J. Harris, ibid., No. 365, 1969). The times of these possible eclipses are apparently consistent with the spectroscopic observations. System816Orbit1End System817Orbit1Begin The value of V0 for HD 129132 AB is, of course variable. Only one and a half long-period cycles have been covered and the elements for HD 129132 ABC are correspondingly uncertain. System817Orbit1End System818Orbit1Begin The value of V0 for HD 129132 AB is, of course variable. Only one and a half long-period cycles have been covered and the elements for HD 129132 ABC are correspondingly uncertain. System818Orbit1End System819Orbit1Begin Harper later revised the period to 12.8244d (Publ. Dom. Astrophys. Obs., 6, 234, 1935). Petrie(II) found Delta m=0.28. Star is fainter (6.8m) component of common-proper-motion pair A.D.S. 9406: A is 6.1m at 3.0". Magnitude in Catalogue refers to combined light of system. System819Orbit1End System820Orbit1Begin Two independent investigations have been made recently of this newly recognized binary; the other is by K.W. Kamper and R.W. Lyons (J. Roy. Astron. Soc. Can., 75, 56, 1981). The study by Beavers and Salzer is preferred, but it is the fairly good agreement between the two that leads us to classify these elements as b rather than c. System820Orbit1End System821Orbit1Begin Epoch is T0. Fekel (private communication) has detected the secondary spectrum in the red. System821Orbit1End System822Orbit1Begin The magnitudes represent the observed range which is probably not quite the full range of variation. The spectral type is inferred from the results of the cross-correlation with standard spectra. The epoch is time of primary minimum: the light-curve shows the orbit to be circular. The primary velocity-curve is well covered and shows a distinct rotation effect during primary minimum. The secondary spectrum is visible despite an estimated Delta m of over 3 m (the cross-correlation brings it out) but measures of it hardly define a Keplerian curve. The orbital inclination (determined from photometric observations published in the same paper) is very close to 90 deg. The secondary spectral type is early or middle K. The stars are nearly in contact, despite this temperature difference. System822Orbit1End System823Orbit1Begin Tomkin's success in detecting the infrared Ca II triplet in the secondary spectrum (with a Reticon) ensures that his values for the orbital elements supersede the several earlier investigations (J. Sahade and C.A. Hernandez, Astrophys. J., 137, 845, 1963; D.B. McLaughlin, Publ. Michigan Obs., 6, 28, 1934 and F. Schlesinger, Publ. Allegheny Obs., 1, 123, 1909 -- recomputed by Luyten). The small eccentricity found by Tomkin is perhaps questionable, however. The light-curve does not require any eccentricity and the value proposed is less than twice its mean error. Earlier work suggested that V0 might be variable, and R.H. Koch (Astron. J., 67, 130, 1962) found some evidence for third light in the UBV light-curves. Sahade and Hernandez questioned the variability of V0, however, and Tomkin does so even more strongly. The strongest evidence for variation comes from the oldest observations and may well be the consequence of the wavelengths adopted for radial-velocity measurement. The best light- curve remains that obtained by Koch (loc. cit.) and his magnitudes are given in the Catalogue. Recently, Guiricin et al. (Astron. Astrophys. Supp., 37, 513, 1979) re-analyzed Koch's observations. They adopted a transit at primary minimum instead of an occultation, and did not require third light. They found an orbital inclination of about 81 deg and a fractional luminosity in V for the primary component of 0.94. There is some disagreement whether the primary spectral type is B9.5V or A0 V. The secondary must be early G. A brief spectrophotometric study has been published by N.I. Krivasheeva and V.V. Lenshin (Astron. Tsirk., No. 1420, 3, 1986). System823Orbit1End System824Orbit1Begin After decades of neglect, this star was observed simultaneously by two independent groups (the other was R.-J. Dettmar and F. Gieseking, Astron. Astrophys. Supp., 54, 541, 1983). Our choice of the elements to include in the Catalogue may not be entirely impartial, but the elements chosen are characterized by the lowest mean error of an individual observation and are based on the spectrograms of the highest dispersion. The two new sets of elements agree within their uncertainties and either would supersede the original determination by R.K. Young (Publ. Dom. Astrophys. Obs., 4, 32, 1927). Both the modern sets of observations have larger than usual residuals for the spectral type and dispersion used, which both groups of investigators suggested might be related to the semi-regular variability of the primary star. (This is one of the few semi-regular variables in a binary with a known orbit). The V magnitude varies by about 0.3m (O.J. Eggen, Astrophys. J. Supp., 14, 307, 1967). Although a period of about 40d has been suggested, it has not been substantiated. The eccentricity is probably genuine, but Dettmar and Gieseking found a smaller value. System824Orbit1End System825Orbit1Begin System825Orbit1End System826Orbit1Begin The epoch is T0 and the orbit is assumed circular in accordance with the light-curve. A definitive value of V0 was not obtained by Popper; it must be slightly variable. Other spectroscopic elements (based on fewer spectrograms of lower dispersion) were determined by L. Binnendijk (Publ. Dom. Astrophys. Obs., 13, 27, 1967). He used spectrograms obtained by W.E. Harper and found K1=127 km/s and K2=202 km/s. The spectroscopic (and eclipsing) binary is the fainter component of a visual binary (A.D.S. 9494). Since the major semi-axis of the visual orbit is less than 4" (minimum separation less than 1") and the other component is 0.5m to 1.0m brighter, the latter's light is always a problem in the interpretation of photometric observations and often one in that of spectroscopic observations. The latest visual orbit is that determined by W.D. Heintz (Astrophys. J. Supp., 37, 71, 1978). The close pair, a W UMa system, has attracted many photometric observers. Two recent discussions are by H.W. Duerbeck (Astron. Astrophys. Supp., 32, 361, 1978) who finds the light-curve to be variable, even within a few weeks, and C. Maceroni et al. (ibid., 45, 187, 1981) who derive an orbital inclination of 71 deg and a fractional luminosity in V for the hotter star of 0.61. A new study of both the short-period and long-period orbits of this system was completed by G. Hill while the Catalogue was in press. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System826Orbit1End System827Orbit1Begin Both components are subgiants. System827Orbit1End System828Orbit1Begin The epoch (time of primary minimum) and period are taken from M. Hoffman (Astron. Astrophys. Supp., 33, 63, 1978). The spectral type is as given by McLean and Hilditch: the fourth edition of the G.C.V.S. gives G2 V. The light-curve shows the orbit to be circular. Radial-velocity measurements have also been published by Y.C. Chang (Astrophys. J., 107, 96, 1948) and Hoffmann (loc. cit.). Chang could not resolve the component spectra, even at quadratures, and wisely refrained from trying to deduce anything but V0 from them. Hoffmann has suggested that Chang's observations provide evidence of a third body with an orbital period of about 34.7 times that of the close pair. Despite evidence for variations in the period and light-curve of the system, however, confirmation from modern observations is essential, if the existence of the third body is to be accepted. Hoffmann discussed the light-curves in some detail, but did not solve for the elements. G. Wolfschmidt, J. Rahe and E. Schoffel (Mitt. Astron. Gesells., 45, 49, 1978) give an orbital inclination of about 77 deg and a fractional luminosity for the larger component of 0.85. System828Orbit1End System829Orbit1Begin Epoch is T0 : orbit assumed circular. Star is brighter component of A.D.S. 9520: companion, 10.8m at 17.9", is probably optical. System829Orbit1End System830Orbit1Begin Epoch is T0. The value for the eccentricity is an upper limit, no value is given for omega. System830Orbit1End System831Orbit1Begin This is the brightest component of A.D.S. 9532: B is 9.4m at 57.8" and C is 1.9" from B and still fainter. The visual orbit has been determined for Aa by Heintz. The period is 22.35y. The elements P, T, e, and omega are well determined from the visual orbit. Heintz has determined K1 and V0 from Lick and Yerkes spectrograms. The magnitude difference between the stars in the spectroscopic pair is about 0.5m. The value of K1 must therefore be very uncertain and Heintz finds that it is difficult to reconcile it with the visual elements. The spectrum is that of a `silicon star'. Heintz gives i=161 deg and the total mass as 8.5 MSol. A homogeneous series of high-dispersion spectrograms would be of value in the study of this system. Reference: W.D.Heintz, Veroff. Munchen, 7, 22, 1966 System831Orbit1End System832Orbit1Begin The individual observations show a large scatter, but the coverage of the velocity curve is good. The star's light varies by about 0.1m and the system may be eclipsing. Thackeray and Emerson suggest that the visual triple H.D. 135160 shares a common-space-motion with this system. A 13.5m companion to H.D. 135240 itself is probably unrelated physically. System832Orbit1End System833Orbit1Begin There are two published orbits for this system that do not agree very well. The other is by O. Struve (Astrophys. J., 102, 74, 1945) who assumes (probably correctly) a circular orbit and finds V0 = 43 km/s, K1 = 47 km/s, D.M. Popper (Ann. Rev. Astron. Astrophys., 18, 115, 1980) gives m1=m2=1.00 MSol, which implies a value of K1 + K2 midway between the two published values. Emission is observed in the H and K lines of Ca II; this together with the subgiant classification puts the system in the RS CVn group. The emission apparently comes from the component in front at primary minimum. There is no modern light-curve: B.W. Sitterly (Pop. Astron., 30, 231, 1922) found i>81 deg. System833Orbit1End System834Orbit1Begin These stars form A.D.S. 9537, the only known visual binary of which each component is a W UMa system. The separation of the two eclipsing pairs is 16.1" and both proper motions and radial velocities (despite a discrepancy of unknown origin within each pair) indicate that these two systems are travelling together in space. Older observations of each star led to provisional elements, and those of BV Dra appeared to be reliable enough to be published (with e quality) in earlier Catalogues. In fact, the superior cross-correlation measurements have shown those elements to have been worthless for any purpose beyond establishing the variability. The epochs given are times of primary minima and the light- curves show the orbits to be circular. Spectral types given for the more massive (brighter) components of each system are probably fairly reliable; those for the fainter components are necessarily uncertain. The spectrophotometric values of Delta m (blue light) are 0.63m and 0.45m for BV and BW Dra respectively. The discrepancy between the values of V0 derived from each component, in each system is not fully understood. It is not removed by taking into account the distortion and asymmetrical distribution of surface brightness of each component. Probably the values given for the primary components are the more reliable. Since the proper motions are also appreciable, the total space velocity is quite large. The intrinsic interest of these two systems has attracted several photometric observers. A detailed discussion of the light-curves and of the nature of the systems has been published by J.K. Ka lu _ zny and S.M. Rucinski (Astron. J., 92, 666, 1986). They find that the two systems are intrinsically different in the sense that neither can evolve into the other. They find orbital inclinations of 76 deg (BV) and 74 deg (BW) and fractional luminosities for the larger components of 0.67 (BV) and 0.73 (BW). Because they consider the effects of light distribution over the surfaces, they derive slightly different values of K1, K2 and V0 (in each system) from those given in the Catalogue. They discuss the evolutionary status of the entire system and conclude that it belongs to the intermediate-to-old disk population. The system is probably close enough for a trigonometrical parallax to be determined (A.R. Upgren, W.D. Heintz private communications). System834Orbit1End System835Orbit1Begin These stars form A.D.S. 9537, the only known visual binary of which each component is a W UMa system. The separation of the two eclipsing pairs is 16.1" and both proper motions and radial velocities (despite a discrepancy of unknown origin within each pair) indicate that these two systems are travelling together in space. Older observations of each star led to provisional elements, and those of BV Dra appeared to be reliable enough to be published (with e quality) in earlier Catalogues. In fact, the superior cross-correlation measurements have shown those elements to have been worthless for any purpose beyond establishing the variability. The epochs given are times of primary minima and the light- curves show the orbits to be circular. Spectral types given for the more massive (brighter) components of each system are probably fairly reliable; those for the fainter components are necessarily uncertain. The spectrophotometric values of Delta m (blue light) are 0.63m and 0.45m for BV and BW Dra respectively. The discrepancy between the values of V0 derived from each component, in each system is not fully understood. It is not removed by taking into account the distortion and asymmetrical distribution of surface brightness of each component. Probably the values given for the primary components are the more reliable. Since the proper motions are also appreciable, the total space velocity is quite large. The intrinsic interest of these two systems has attracted several photometric observers. A detailed discussion of the light-curves and of the nature of the systems has been published by J.K. Ka lu _ zny and S.M. Rucinski (Astron. J., 92, 666, 1986). They find that the two systems are intrinsically different in the sense that neither can evolve into the other. They find orbital inclinations of 76 deg (BV) and 74 deg (BW) and fractional luminosities for the larger components of 0.67 (BV) and 0.73 (BW). Because they consider the effects of light distribution over the surfaces, they derive slightly different values of K1, K2 and V0 (in each system) from those given in the Catalogue. They discuss the evolutionary status of the entire system and conclude that it belongs to the intermediate-to-old disk population. The system is probably close enough for a trigonometrical parallax to be determined (A.R. Upgren, W.D. Heintz private communications). System835Orbit1End System836Orbit1Begin The spectral type of the secondary is computed from the depth of eclipse. Bartolini et al. also published a light-curve based on V observations. It has been re-analysed by G. Giuricin, F. Mardirossian and S. Ferluga (Astron. Nachr., 302, 187, 1981) who find the two stars to be in contact. The orbital inclination is about 74 deg and the fractional luminosity of the brighter component is 0.99. System836Orbit1End System837Orbit1Begin The new observations supersede previous work (J.A. Pearce, Publ. Am. Astron. Soc., 8, 219, 1935; J.S. Plaskett, Publ. Dom. Astrophys. Obs., 1, 187, 1920; J. Sahade and O. Struve, Astrophys. J., 102, 480, 1945) because, for the first time, reliable measures of the secondary spectrum have been made (in the infrared) and omission of velocities derived from the hydrogen and helium lines from the plate means for the primary component clearly demonstrate that the true orbit is circular, in accordance with the light-curve. All the Victoria observations (stretching over about sixty years) can be harmonized by one fairly well determined value of K1, although there is some evidence that V0 may be variable, which could indicate the presence of a third body. The epoch is the time of primary minimum. Direct evidence for circumstellar matter in the system is provided by the observations of O. Struve, J. Sahade and S.-S. Huang (Publ. Astron. Soc. Pacific, 69, 342, 1957). Photometric observations and analysis have been published by D.B. Wood (Astrophys. J., 127, 351, 1958; 128, 595, 1958) and by S. Catalano, S. Cristaldi and G. Lacona (Mem. Soc. Astron. Ital., 37, No. 2, 1966). A re-analysis of the former by B. Cester et al. (Astron. Astrophys., 61, 469, 1977) gives an orbital inclination close to 80 deg and fractional luminosity in V for the brighter component of 0.96. Cester et al., however, believed the spectral type of the secondary component to be somewhat later than subsequently found by Batten and Tomkin. A discussion combining the spectroscopic and photometric data that are now available for this star would be useful. System837Orbit1End System838Orbit1Begin The new observations supersede those of W.H. Christie (Publ. Dom. Astrophys. Obs., 4, 55, 1927) since resolution of the secondary spectrum has led to a revision of all the elements, including the period. The primary star is an Am star (A3, A7, and F0 from the K line, hydrogen lines, and metal lines respectively). The secondary component is not an Am star, although it too rotates slowly. System838Orbit1End System839Orbit1Begin Two companions are listed in I.D.S. The closer of these (separation 1") shows evidence of orbital motion about the spectroscopic pair. Its light is included in the magnitude given in the Catalogue, but the difference in magnitude is 1.5m. Thackeray suggests that this triple system belongs to the Sco-Cen association. The 9m companion at 26.5" has neither the spectral type nor the radial velocity that would be expected if it were physically associated with the other three stars. System839Orbit1End System840Orbit1Begin The magnitude varies by about 0.1m and the object appears to be a non-eclipsing RS CVn system and ellipsoidal variable. Although W.P. Bidelman and D.J. MacConnell (Astron. J., 78, 687, 1973) classified the spectrum as K1 III and F, lines of only the K-type spectrum are seen by Fekel et al., who suggest that the other component is G or K. Light and velocity variations were first discovered by E.W. Burke et al. (Inf. Bull. Var. Stars, No. 2111, 1982) and B.W. Bopp et al. (Astrophys. J., 275, 691, 1983). Only with the observations of Fekel et al., however, has it become possible to remove an ambiguity of a factor of two in the period. The orbit was assumed circular when an elliptical solution gave a negligibly small eccentricity. The epoch is T0. System840Orbit1End System841Orbit1Begin New observations by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976) confirm the earlier elements. System841Orbit1End System842Orbit1Begin Chang assumed P=41.56y, T=1933.829, together with the values of e and omega, from a visual orbit by O. Lohse (Publ. Astrophys. Obs. Potsdam, 20, 119, 1909). More modern orbits by E. Silbernagel (Astron. Nachr., 234, 441, 1929) and A. Danjon (Bull. Astron. Paris, 11, 191, 1938) are very similar. The system is A.D.S. 9617. Two faint distant companions listed in I.D.S. are probably optical. The quality designation refers only to the spectroscopically determined elements. The magnitude is the combined light of the visual pair. System842Orbit1End System843Orbit1Begin The epoch is T0 and the orbit was assumed circular after a preliminary solution showed the eccentricity not to be significant. The spectral type given is not a direct classification but an estimate based on the colour index, small proper motion and the appearance of the radial-velocity traces. System843Orbit1End System844Orbit1Begin Member of the Sco-Cen group with two visual companions 14m and 12.5m at about 20" and 30" respectively. System844Orbit1End System845Orbit1Begin The importance of this system is that it belongs to Population II. System845Orbit1End System846Orbit1Begin P=10.496y. These elements supersede those derived by J.B. Cannon (Publ. Dom. Obs., 1, 375, 1912). Neubauer found some evidence for a shorter-period velocity-variation with the following elements: P=320.13d, T=J.D. 2,426,475, omega=102 deg, e=0.7, K=1.4 km/s, V0 (variable), and f(m)=0.000034 MSol. There is one visual observation listed in I.D.S. of the secondary in the 10.5y orbit. The spectrum shows Sr, Cr, and Eu peculiarities. System846Orbit1End System847Orbit1Begin The computation by Lucy & Sweeney of the elements from observations by W.H. Christie (Astrophys. J., 83, 433, 1936) is preferred to Christie's own provisional analysis. The epoch is T0. An earlier orbit by Christie (Publ. Dom. Astrophys. Obs., 3, 310, 1926) was based on an erroneous value for the period. The spectrum is Am, and is classified as A3, A0 and F0 by the K line, hydrogen lines and metallic lines respectively (Curchod and Hauck). System847Orbit1End System848Orbit1Begin Various spectral types and luminosity classes are given in the literature; this one is based on the continuum flux-distribution in the infrared (B.W. Bopp, R.D. Gehrz and J.A. Hackwell, Publ. Astron. Soc. Pacific, 86, 989, 1974). Since the star is considered to be an FK Com variable, the giant classification seems the most plausible. The authors themselves describe the orbital elements as preliminary. The small eccentricity is not significant. There is a possibility that V0 is variable. System848Orbit1End System849Orbit1Begin The star probably belongs to the Sco-Cen group and displays evidence of an expanding circumstellar shell. It is one of the two approximately equal components for which a visual orbit of P=147y and a=0.6" has been computed by W.D. Heintz (Astron. Nachr., 283, 145, 1956). System849Orbit1End System850Orbit1Begin As far as the primary component is concerned, the elements given by Tomkin and Popper are obtained from a new analysis of the observations made and discussed by E.G. Ebbighausen (Publ. Astron. Soc. Pacific, 14, 411, 1976). Tomkin and Popper also succeeded in detecting the much fainter secondary spectrum by means of Reticon observations in the infrared. Their work thus supersedes not only Ebbighausen's but also the earlier investigations by F.C. Jordan (Publ. Allegheny Obs., 1, 85, 1909), J.B. Cannon (J. Roy. Astron. Soc. Can., 3, 419, 1909) and D.B. McLaughlin (Publ. Michigan Obs., 5, 91, 1933). There is fairly good agreement between these investigators on the value of K1 but Cannon's value for e differed from the others. The values adopted for e and omega by Tomkin and Popper are partly influenced by the photometric values of e cos omega and e sin omega. Photometric observations in the red were published and discussed by G.E. Kron and K.C. Gordon (Astrophys. J., 110, 63, 1949) and discussed also by E. Budding (Astrophys. Space Sci., 26, 371, 1974). Tomkin and Popper also analyzed these observations. They deduced an orbital inclination close to 88 deg and found that the secondary gives only 0.02 of the total red light. Observations of the UV spectrum have been briefly discussed by T.J. Herczeg, Y. Kondo and K.A. van der Hucht (Astrophys. Space Sci., 46, 379, 1977). System850Orbit1End System851Orbit1Begin Although the velocity-curve published by Levato et al. does not look convincing, A.D. Thackeray (Mem. Roy. Astron. Soc., 70, 33, 1966) measured double lines on two plates. The star probably belongs to the Sco-Cen group. System851Orbit1End System852Orbit1Begin Other investigations have been published by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 137, 1919 -- recomputed by Luyten) and B. Smith (Astrophys. J., 110, 63, 1949). All agree reasonably well on the value of K1 and in finding a small eccentricity -- Smith was probably correct in adopting a circular orbit -- but a modern spectroscopic study of this fairly bright system would be useful. The elements given in the Catalogue differ slightly from either of the solutions actually published by Pearce, being based on all the Victoria observations available to him. Pearce also drew attention to the variability of the period and estimated a mass-ratio of 0.28 from spectrograms obtained during primary eclipse. Photometric observations have been published by R.L. Baglow (Publ. David Dunlap Obs., 2, 1, 1952) and K. Walter (Astron. Astrophys. Supp., 32, 57, 1978). The latter's observations were analyzed by G. Giuricin, F. Mardirossian and F. Predolin (Astrophys. Space Sci., 73, 389, 1980) who find an orbital inclination of 85 deg and a fractional luminosity for the brighter star (in yellow) of 0.64. The star is the brighter member of A.D.S. 9706: companion is 9.5m at 3.4". System852Orbit1End System853Orbit1Begin Another member of the Sco{Cen group. The primary velocity-curve is poorly defined. System853Orbit1End System854Orbit1Begin This is another X-ray pulsar, although the orbital elements are not so well determined as for some of the others, partly because of incomplete coverage of the velocity-curve and partly because of an intrinsic variability of the pulsar period. Similar results were obtained by P.J.N. Davison, M.G. Watson and J.P. Pye (Mon. Not. Roy. Astron. Soc., 181, 73P, 1977). The epoch is the time of superior conjunction of the X-ray source. The directly measured quantity is a 1 sin i, from which K1 is derived. The values of V0 and K2 and the spectral classification are taken from the work of D. Crampton, J.B. Hutchings and A.P. Cowley (Astrophys. J., 225, L63, 1978). They also derive a value of K1 from the emission line of He II lambda 4686, which is in close accord with the value derived from X-ray observations. They estimate an orbital inclination of about 70 deg. The B magnitudes are taken from the fourth edition of the G.C.V.S. System854Orbit1End System855Orbit1Begin The maximum magnitude is from R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 72, 101, 1975) and the minimum is estimated from L. Binnendijk's BV light-curves (Astron. J., 77, 239, 1972). Analysis of these light-curves by F. Mardirossian et al. (Astron. Astrophys. Supp., 40, 57, 1980) and R.E. Wilson and J.B. Rafert (ibid., 42, 195, 1980) indicate that the orbital inclination is near 80 deg and the primary component contributes at least 0.95 of the total light in V. The light-curve shows no evidence for orbital eccentricity, and Lucy & Sweeney adopt a circular orbit. System855Orbit1End System856Orbit1Begin Orbital elements have also been published by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 3, 179, 1925 -- recomputed by Luyten). The new elements serve only to underline the difficulties of interpreting the system. The elements V0, K1, and K2 all differ from Plaskett's values (26.6 km/s, 134.8 km/s and 137.7 km/s, respectively -- note the apparent reversal in the mass-ratio and the considerable reduction of the total mass). It is clear that the velocity-curve of the secondary component, at least, has changed appreciably, and the question arises, `How far can the secondary spectrum be attributed to the secondary star?' A long series of two-prism spectrograms had been obtained by R.M. Petrie, who was also puzzled by many features of the system. Earlier, Petrie(II) found Delta m=0.12, consistent in sense with Abhyankar's and Sarma's value for the mass-ratio. Star is the brighter component of A.D.S. 9737: fainter component (zeta1 CrB) is 6.0m at 6.3". System856Orbit1End System857Orbit1Begin Epoch is T0. The two spectra are very similar in type and intensity. System857Orbit1End System858Orbit1Begin At the time of writing only an abstract is available for judging these two orbits. The quality rating is based on the published values of the mean errors of a single observation. The star is a close visual binary and each component is a spectroscopic pair. Only one spectrum of the fainter (visual) component can be seen. All three visible spectra are closely similar. System858Orbit1End System859Orbit1Begin At the time of writing only an abstract is available for judging these two orbits. The quality rating is based on the published values of the mean errors of a single observation. The star is a close visual binary and each component is a spectroscopic pair. Only one spectrum of the fainter (visual) component can be seen. All three visible spectra are closely similar. System859Orbit1End System860Orbit1Begin Elements have also been published by F.C. Jordan (Publ. Allegheny Obs., 3, 153, 1914). Agreement between the two sets is good. Petrie(II) found Delta m=1.39. The few measures made of the secondary spectrum indicate a mass-ratio of about 0.6. System860Orbit1End System861Orbit1Begin Epoch is T0. Lucy & Sweeney adopt a circular orbit. Apparently no analysis of the light-curve has been published. System861Orbit1End System862Orbit1Begin According to C. Blanco and F.A. Catalano (Astron. J., 76, 630, 1971), the light of this star is variable. A slightly different value for T is found from the observations of the secondary component. System862Orbit1End System863Orbit1Begin Lucy & Sweeney confirm the eccentricity. System863Orbit1End System864Orbit1Begin The systemic velocity appears to be variable, the value given refers to observations obtained in 1961-65 and was obtained by Wilson's method together with a value of 1.42 for the mass-ratio. The value given for K1 is in fact the sum of K1+K2. The epoch is T0 and the orbit was found to be circular (e<0.003), although a value was derived for omega. The primary component is a `mercury star'; the secondary resembles an early Am star. Dworetsky finds Delta m=1.14 at lambda 4481. System864Orbit1End System865Orbit1Begin Member of the Sco-Cen group and an occultation double. (Levato et al. believe the occultation and spectroscopic pair to be the same.) Double lines suspected on one plate (W.W. Campbell and J.H. Moore, Publ. Lick Obs., 16, 231, 1928) System865Orbit1End System866Orbit1Begin Member of the Sco-Cen group. System866Orbit1End System867Orbit1Begin This is another cataclysmic variable of the AM Her type. The magnitude given is a mean and is subject to fluctuations of the order of 1m. The spectrum is characterized by emission lines of hydrogen, helium and ionized carbon, nitrogen and oxygen. The epoch is the time of linear polarization peaks. The values given for K1 and V0 are the means for all lines. K. Mukai and P.A. Charles (Mon. Not. Roy. Astron. Soc., 222, 1P, 1986) have detected the secondary spectrum and it is their spectral type that is given in the Catalogue. System867Orbit1End System868Orbit1Begin The spectral type is variously given as G0 IV or G2 V. According to Beavers and Salzer, G0 IV is in better agreement with the trigonometrical parallax of 0.041". The I.D.S. lists an 11.8m companion at nearly 100" separation, but the relative motion would suggest that the pair is optical. System868Orbit1End System869Orbit1Begin Member of the Sco-Cen group. Elements described as `very marginal' by Levato et al. System869Orbit1End System870Orbit1Begin Member of the Sco-Cen group. Brighter component of A.D.S. 9846; companion 12.8m at 38.3". System870Orbit1End System871Orbit1Begin Member of Sco-Cen group. System871Orbit1End System872Orbit1Begin The velocities show a large scatter about the mean curve, perhaps partly because they are derived from spectrograms obtained at three different observatories, but partly because of the nature of the spectrum and the possible influence on it of gas streams. This is a Be star for which the binary nature now seems fairly certain. The orbital elements are not well determined, however, and a later paper (P. Harmanec et al., Bull. Astron. Inst. Csl, 27, 47, 1976) has shown differences in the elements obtained from different lines of the Balmer series. System872Orbit1End System873Orbit1Begin Elements have also been published by O. Struve and C.T. Elvey (Astrophys. J., 66, 217, 1927-- recomputed by Luyten). H. Levato et al. (Astrophys. J. Supp., 64, 487, 1987) have also recomputed elements from all available observations. S.J. Inglis (Publ. Astron. Soc. Pacific, 68, 259, 1956) also published observations and found Delta m=1.2. The orbit of the primary component seems to be well determined but there is a disturbing difference in the values found for K2 (Struve and Elvey found 180 km/s). Thus, again, the masses of the components are quite uncertain. The light of the star has been suspected of variability. Epoch is an arbitrary zero that corresponds roughly to T0. Star is brighter component of A.D.S. 9862: companion is 12.2m at 50.4". System873Orbit1End System874Orbit1Begin This is an X-ray pulsar for which no optical counterpart was known at the time the paper by Kelley, Rappaport and Ayasli was published. Coordinates are approximate and no magnitude or spectral type can be given. Kelley et al. speculate that the companion object may be a Be star. The directly measured quantity is either the delay in the pulse arrival time, or the change in the pulse period. The value of K has therefore been derived from that of a sin i. Although individual observations are very precise, the coverage of the orbit is patchy. An elliptical orbit cannot be ruled out, but a circular one was assumed and the epoch is the time of superior conjunction of the X-ray source. System874Orbit1End System875Orbit1Begin The epoch is T0. The orbit was assumed circular after a solution for an elliptical orbit gave a negligibly small eccentricity. Two observations give very large residuals and raise the possibility that the primary star sometimes shows radial-velocity variations that are not of orbital origin. From three observations of the secondary spectrum, Griffin deduces a mass-ratio of 0.82 and suggests that the system might display eclipses. System875Orbit1End System876Orbit1Begin The magnitude is variable by about 0.03m in V. The light variations are correlated with the orbital period and the epoch is the time of maximum light in V. The orbit is assumed circular and the value of K1 is a mean for all emission lines. The value of V0 is indeterminate, but Isserstedt et al. suggest that this is a runaway object and that the secondary is a neutron star. System876Orbit1End System877Orbit1Begin This is a recurrent nova and the maximum magnitude refers to its brightest outburst; at minimum the magnitude is variable. These new observations confirm earlier estimates of K1 (R.F. Sanford, Astrophys. J., 109, 81, 1949; R.P. Kraft, Astrophys. J., 127, 625, 1958 and B. Paczynski, Acta Astron., 15, 197, 1965 -- based on Kraft's observations). Kraft measured the H-beta emission line, which he ascribed to the nova component, and his value of K2 is given in the Catalogue. Kenyon and Garcia did not rely on this emission line and preferred to estimate the mass-ratio by indirect methods -- one of which leads to a result very similar to Kraft's while the other would imply much lower masses. One doubtful observation of a visual companion at 0.2" is recorded in I.D.S. System877Orbit1End System878Orbit1Begin The variable radial velocity of this chemically peculiar star was first pointed out by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976) and his velocities fit the period derived by Dworetsky. Aikman could not completely resolve the two spectra, however, and did not derive the period. Dworetsky describes his own elements as provisional and estimates the mass-ratio (primary.secondary) as 1.5. System878Orbit1End System879Orbit1Begin P=44.70y, T=1905.39. These elements together with e and omega are taken from a visual orbit by R.G. Aitken (Publ. Lick Obs., 16, 31, 1928) who also found i=29.1 deg. A more modern visual orbit has been published by P. Baize (l'Astronomie, 56, 157, 1942). The quality is assigned only to the spectroscopically determined elements. The system is A.D.S. 9909: there is a 7.2m third component at 7.6" from A. System879Orbit1End System880Orbit1Begin Petrie found Delta m=1.17. The wide difference in the spectral types, however, makes the determination of Delta m difficult. The A0 (fainter) component appears to be distinctly subluminous and under-massive. The determination of K2 is much less certain than that of K1. The epoch is T0. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. System880Orbit1End System881Orbit1Begin The new observations and discussion by Peterson et al. supersede the earlier work of Z. Daniel and F. Schlesinger (Publ. Allegheny Obs., 2, 127, 1912), J.C. Duncan (Lowell Bull., 2, 21, 1912), W.J. Luyten, O. Struve and W.W. Morgan (Publ. Yerkes Obs., 7, 251, 1939) and K.D. Abhyankar (Astrophys. J. Supp., 4, 157, 1959, see also Bull. Astron. Soc. India, 7, 123, 1979). The elements of the primary orbit are well determined. Apsidal motion is now established, with a period of the order of 730 years. The value given for omega is appropriate to the epoch, T, given in the Catalogue. An apparently variable systemic velocity may be partly accounted for by systematic errors between observatories, but may also reflect real orbital motion of the close pair about the visual companion. The value given for V0 in the Catalogue is derived from the observations of Peterson et al. alone; other elements are derived from all available observations. Peterson et al. derive V0=+3.8 km/s from observations of the secondary, but do not find the large difference between the two components that was found by Abhyankar. The star is the brightest component of A.D.S. 9913. Observations of an occultation of the system by the Moon enabled D.S. Evans, J.L. Elliott and D.M. Peterson (Astron. J., 83, 438, 1978) to derive Delta m for the pair AB as 3.31m at a separation 0.46", and, for the pair AC, Delta m=2.41 at a separation of 13.5". An occultation of the system by Jupiter has also been observed (J.L. Elliot, K. Rages and J. Veverka, Astrophys. J., 197, L123, 1975 and 207, 994, 1976; J.L. Elliot and J. Veverka, Icarus, 27, 359, 1976). From this, an orbital inclination of about 65 deg is derived and an angular separation of the spectroscopic component of 0.0015". Angular diameters of the component stars of the close pair have also been determined. A parallax of about 0.005 is estimated from the system's membership of the Sco-Cen association. System881Orbit1End System882Orbit1Begin The elements are in good agreement with an earlier set obtained by H.D. Curtis (Lick Obs. Bull., 4, 156, 1907) revised by Luyten, except that Abt and Levy find a slightly larger value of K1. Both Luyten and Lucy & Sweeney adopted a circular orbit, and it is clear from these new elements that this is probably the correct procedure (e=0.01+/-0.01). The epoch is presumably T0, but this is not clear from the paper by Abt and Levy. System882Orbit1End System883Orbit1Begin The spectrum is classified as A3 from the K line and F0 from the metallic lines. System883Orbit1End System884Orbit1Begin Another symbiotic star whose orbital elements are rated as `preliminary' by Garcia himself. The elements depend on only seven observations, but a photometric periodicity of about 550 d appears to be present in the U band (L. Meininger, Inf. Bull. Var. Stars, No. 1611, 1979) and in the variable line profiles (S.E. Smith and B.W. Bopp, Mon. Not. Roy. Astron. Soc., 195, 733, 1981). The epoch is the day of the first observation (close to superior conjunction of the K-type star) and the value of V0 is not given by Garcia, but is estimated from his plot of the velocity-curve. The system is known to be a source of soft X-rays (M. Anderson, J.P. Cassinelli and W.T. Sanders, Astrophys. J., 247, L127, 1981). Other descriptions of the spectrum (including the UV spectrum) are given by R. Falomo (Astrophys. Space Sci., 91, 63, 1983) and M.H. Slovak et al. (Bull. Am. Astron. Soc., 15, 665, 1983). System884Orbit1End System885Orbit1Begin Lucy & Sweeney accept the eccentricity. System885Orbit1End System886Orbit1Begin Earlier observations from Lick and Cape observatories fit the velocity-curve fairly well, but observations from Mount Wilson show an appreciable scatter. System886Orbit1End System887Orbit1Begin A mercury-manganese star whose binary nature was also discovered at the Hale Observatories (H.W. Babcock, Carnegie Institution Year Book, 70, 404, 1971). System887Orbit1End System888Orbit1Begin Member of Sco{Cen group. T.S. van Albada and D. Sher (Bull. Astron. Inst. Netherl., 20, 204, 1969) measured double lines on one plate. System888Orbit1End System889Orbit1Begin The first elements were published by A. van Hoof (Astrophys. J., 137, 824, 1963) and were recomputed by Lucy & Sweeney, who preferred a circular orbit. Levato et al. have used all available radial-velocity observations and obtained a value of K1 close to that found by Lucy & Sweeney, but once again reintroduce an orbital eccentricity. The star belongs to the Sco-Cen group and is the brighter member of A.D.S. 9951; the companion is 6.5m at 41.1". Each component is itself double and H.D. 145501 at 41" is A.D.S. 9951C. System889Orbit1End System890Orbit1Begin Member of Sco-Cen group: elements called `very marginal' by Levato et al. System890Orbit1End System891Orbit1Begin Griffin suggests that this star may be a subgiant and the system may be of the RS CVn type. He reports that Bopp finds H-alpha to be too strong for the H.D. type of K0. The epoch is T0. System891Orbit1End System892Orbit1Begin These elements supersede those derived by Christie in Publ. Astron. Soc. Pacific, 46, 238, 1934. According to I.D.S. the star has twice been reported double, with a separation of 0.1". It is not clear whether or not the visual companion, if real, is identical with the spectroscopic secondary component. System892Orbit1End System893Orbit1Begin Both the nature of the radial-velocity traces and unpublished photometry suggest that this star is a giant. System893Orbit1End System894Orbit1Begin The first orbit published by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 231, 1925 and 6, 234, 1935) and recomputed by Luyten was shown by R.W. Tanner (Publ. David Dunlap Obs., 1, 473, 1949) to be based on an incorrect value for the period. Bakos has used these same observations and added new ones, obtained at higher dispersion. He has slightly revised Tanner's value for the period, and the mean errors for a single plate suggest that Bakos' solution is a slight improvement on the older one -- with which it is in reasonable agreement. Probably the small orbital eccentricity should have been ignored, but the epoch given is the time of periastron passage. The magnitude of the system is slightly variable (by about 0.05m). Two periodicities have been claimed -- the orbital period and a slightly longer one. Bakos gives and discusses photometric observations as well as spectroscopic ones. The system has been described as a deg Sct variable, but this is far from certain. More probably, the variations are, at least partly, those to be expected in an RS CVn system: variable H and K emission is seen in the spectrum. The UV spectrum (as observed with IUE) has been discussed by R.A. Stern (Bull. Am. Astron. Soc., 15, 665, 1983) and S.P. Tarafdar and P.C. Agrawal (Mon. Not. Roy. Astron. Soc., 207, 809, 1984). Observations of H-alpha are reported by S.C. Barden (Bull. Am. Astron. Soc., 16, 473, 1984). The star is the brightest member of A.D.S. 9949: B is sigma 1 CrB (m V=6.66) physically related to A with an orbital period of the order of 1,000 years. Of the other companions, C (13.3m at 8.7" in I.D.S.) is probably, and D (10.8m at 71.0" in I.D.S.) is certainly optical. System894Orbit1End System895Orbit1Begin A new orbital study has been published by J. LaSala and J.R. Thorstensen (Astron. J., 90, 2077, 1985). It confirms the orbital period and leads to slightly different elements (K1 = 48 km/s and V0 = 125 km/s). The uncertainties are such that the differences between this and the values of Cowley and Crampton are not significant, and there is no obvious reason to prefer one set of values over the other. Both sets of elements are derived from measures of the base of the emission line of He II lambda 4686. LaSala and Thorstensen show that other lines, in particular H-beta, differ in phase by a variable amount from the He II line. This may account for some reports of phase changes in the system. Even measures of the He II line may be affected by radiation from a hot spot or a gaseous stream. A circular orbit was assumed and the epoch is T0. The magnitudes are estimated from light-curves published by D.E. Mook (Astrophys. J., 150, 125, 1967). D. Crampton et al. (Astrophys. J., 207, 907, 1976) have estimated i=30 deg and individual masses of approximately 1.3 MSol (for the X-ray component) and 1 MSol. System895Orbit1End System896Orbit1Begin The star is a beta CMa variable, with a light amplitude of about 0.8m. Disentangling of the velocity variations due to pulsation (P=0.25d) and those due to orbital motion is rather difficult. The orbital period could be either 34.23d or 34.13d, with a slight preference for the former value. Earlier investigations have been made by F.C. Henroteau (Lick Obs. Bull., 9, 173, 1918, Publ. Dom. Obs., 5, 303, 1921, and 8, 45, 1922); R.D. Levee, (Astrophys. J., 115, 402, 1952); and O. Struve, D.H. McNamara and V. Zebergs (Astrophys. J., 122, 122, 1955). Earlier work by T. Selga is not available at Victoria. Star is brighter member of A.D.S. 10009: companion is 8.7m at 20". System896Orbit1End System897Orbit1Begin System897Orbit1End System898Orbit1Begin Lucy & Sweeney adopt a circular orbit. System898Orbit1End System899Orbit1Begin The magnitudes given are visual magnitudes derived from uvby photometry. The two spectral types are closely similar. The epoch is the time of primary minimum (the two minima are almost equal in depth), although note that there is fairly rapid apsidal motion with a period of about 40y. The small eccentricity is thus real and confirmed by the photometric observations. Despite fairly large uncertainties for individual observations, values of K1 and K2 are known to within one percent. The orbital inclination is close to 82 deg and the stars differ by 0.36m in visual magnitude. System899Orbit1End System900Orbit1Begin According to I.D.S. there is a 10.3m companion at about 20". System900Orbit1End System901Orbit1Begin Harper reconsidered the system and suggested P might be revised to 5.0193d (Publ. Dom. Astrophys. Obs., 6, 235, 1935). System901Orbit1End System902Orbit1Begin A 7.5m companion at 22" is listed in I.D.S. Thackeray classifies it as B9 V and regards it as a physical companion of the spectroscopic pair. System902Orbit1End System903Orbit1Begin These elements are described as `marginal' by Abt and Levy themselves. System903Orbit1End System904Orbit1Begin Binary nature of the star was discovered by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961) who gave orbital elements based on approximately half the true period. Abt was aware of the possibility that the true period is in the neighbourhood of 27 d. Abt and Gutmann differ in the values they find for the mass-ratio and the relative intensities of the component spectra. Gutmann's observations seem to be correct in these respects. H.A. Abt and S.G. Levy (Astrophys. J. Supp., 59, 229, 1985) saw no need to revise these elements in their recent new study of Am binaries. Gutmann found both stars to be of the same spectral type, and classified them as A7. Abt finds the spectral class to be A2, A7 and A7 from the K line, the hydrogen lines and the metallic lines, respectively. Gutmann found Delta m=0.54, using Petrie's method. If the stars obey the mass-luminosity relation the orbital inclination is 30.5 deg. A 7.8m companion at 1.0" is listed in I.D.S. System904Orbit1End System905Orbit1Begin Griffin believes this star to be a giant and draws attention to the short period, suggesting that the system might prove to belong to the RS CVn group. SB9 correction: The epoch given in the original paper is NOT for the periastron passage. System905Orbit1End System906Orbit1Begin A few isolated observations of the secondary spectrum lead to a mass-ratio of 1.61 and minimum masses of 0.29 MSol and 0.18 MSol. System906Orbit1End System907Orbit1Begin Based on observations and calculations by H.M. Reese. A 10.1m `companion' at 256" is listed in I.D.S., but there seems to be no reason to suppose that there is any physical connection. System907Orbit1End System908Orbit1Begin The spectrum shows emission cores in the H and K lines of Ca II and also emission in the h and k lines of Mg II and at H-alpha. The system is a known X-ray source. Primarily on photometric grounds, Johnson and Mayor suggest that the invisible secondary is itself a binary -- probably consisting of a red dwarf and a white dwarf. System908Orbit1End System909Orbit1Begin Slightly different elements, based on Griffin's observations, have been published by A. Abad and A. Elipe (Astrophys. J., 302, 764, 1986). Griffin believed the secondary spectrum to be just visible and drew resemblances between this system and that of Capella. Later, he confirmed the presence of the secondary spectrum (R.F. Griffin, Mon. Not. Roy. Astron. Soc., 210, 745, 1984 -- note at end of the paper) but the measured velocity poses problems of interpretation. It seems unlikely that the orbital elements of the primary star are seriously in error, but more observations are needed to elucidate this system. System909Orbit1End System910Orbit1Begin Lucy & Sweeney accept this orbital eccentricity. The star is the brighter member A.D.S. 10116: companion is 13.9m at 3.8". System910Orbit1End System911Orbit1Begin Petrie(II) found Delta m=0.70. A 7.3m companion is listed in I.D.S. at 157". It has an appreciably larger proper motion than does the spectroscopic pair. System911Orbit1End System912Orbit1Begin This is a very interesting dwarf system resembling YY Gem, but even smaller. The epoch is the time of primary minimum, and the orbits were assumed circular, after preliminary solutions showed the eccentricities to be negligibly small. The radii of the two stars are each of the order of one quarter that of the Sun. Lacy's thorough photometric and spectroscopic study of the system leads him to the conclusion that it is the smallest, faintest, and least massive main-sequence eclipsing binary known. The system is known to be a flare star, but is much less active than Population I flare stars of similar luminosity. Kinematically, the system appears to be a Population II object (space velocity 163 km/s). Low-dispersion spectrograms obtained by S.M. Rucinski (Acta Astron., 28, 167, 1978) show that the strength of molecular features in the spectrum support classification of the star as a subdwarf; the spectrum is very similar to that of Barnard's star. The light-curve shows variations that can be ascribed to star spots. Lacy finds that the orbital inclination is 89.8 deg, and that the larger component gives 0.53 of the total light at 8200A. The binary system has a 15.0m common-proper-motion companion at 25.7" separation. The parallax is 0.069". System912Orbit1End System913Orbit1Begin Elements derived earlier by A.H. Joy and O.L. Dustheimer (Astrophys. J., 81, 479, 1935) do not agree well with Sahade's values. Joy and Dustheimer found K1=105.5 km/s. The light-curve shows the eccentricity to be spurious, and Lucy & Sweeney adopt a circular orbit. C.-C. Wu et al. (Bull. Am. Astron. Soc., 5, 345, 1973), from satellite observations at lambda 2460, find evidence for an absorbing cloud between the components. The independent photometric analyses of UBV light-curves by E.J. Devinney et al. (Publ. Astron. Soc. Pacific, 82, 10, 1970) indicate that i is close to 84 deg and the primary star gives 0.95 of the light in V. These results were substantially confirmed by F. Mardirossian et al. (Astron. Astrophys. Supp., 40, 57, 1980). The spectral type of the secondary is derived from the photometric colours, and the magnitudes are estimated from data in the paper by Devinney et al. System913Orbit1End System914Orbit1Begin The new observations are probably an improvement on those obtained by O. Struve and L. Gratton (Astrophys. J., 108, 497, 1948) and by O. Struve and V. Zebergs (ibid., 130, 789, 1959) although the agreement between the different sets of observations is relatively good for a W UMa system. This fact justifies the c category, despite the rather strong concentration of the new observations at one node of the orbit. The maximum magnitude is taken from Wilson's paper (see below) and the minimum is estimated from his data. The spectral types are as given by Struve and Gratton. The period is variable; the epoch is the time of primary minimum as given by W.C. Maddox and B.B. Bookmyer (Inf. Bull. Var. Stars, No. 1569, 1979) but the nodes are shifted with respect to this ephemeris. The orbit is assumed circular despite a suggestion by C. Maceroni, L. Milano and G. Russo (Astron. Astrophys. Supp., 49, 123, 1982) that the asymmetry of the light-curve simulates that to be expected in an eccentric orbit. Maceroni et al. analyzed the BV observations published by R.E. Wilson (Astron. J., 72, 1028, 1967) and found an orbital inclination of 71 deg and a fractional luminosity (in V) for the cooler component of 0.66. Somewhat different results were obtained by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978). The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System914Orbit1End System915Orbit1Begin The new observations cover the most interesting part of the velocity-curve of this visual system. Combined with earlier observations discussed by L. Berman (Publ. Astron. Soc. Pacific, 53, 22, 1941) and A.B. Underhill (Publ. Dom. Astrophys. Obs., 12, 159, 1963), they are sudegcient to cover the entire orbital period. Analysis (by Scarfe et al.) of the spectroscopic and visual observations separately produces results that do not entirely agree. Presented in the Catalogue is their combined solution (P=34.487y -- fixed, T=1967.828) which they do not find entirely satisfactory and present as preliminary. From time to time a third body has been suggested for this system. Scarfe et al. consider this an unlikely explanation for the systematic departures they find from the predicted velocity-curve. The orbital inclination is 133 deg and the ascending node is at 236 deg. Since there are no velocity observations of the secondary, and the visual orbit is a relative one, the masses cannot be estimated without making some assumption about the parallax or the mass-ratio. A total mass of between 2 MSol and 3 MSol seems to be indicated. The visual companion is 2.63m fainter (in V). The major semi-axis of the orbit is about 1.3". System915Orbit1End System916Orbit1Begin Epoch is T0. Results of an earlier investigation by R.F. Sanford (Astrophys. J., 64, 172, 1926) agree well with the present results. There is a slight difference in the values found for K1 (Sanford gives 97.4 km/s) but it is probably not greater than the uncertainty of the element. Abrami's results have been further discussed by A. Krancj (Publ. Bologna Univ. Obs., 7, 11, 1959). Petrie(II) found Delta m=0.40. He also assigned the spectral types given in the Catalogue. Reference: A.Abrami, Trieste Contr., No. 285,, 1959 System916Orbit1End System917Orbit1Begin Epoch is T0.orbit is assumed circular. This is another RS CVn system with H and K emission visible in the spectrum and showing Doppler shifts in phase with those of the secondary spectrum but of smaller amplitude. D.M. Popper (Publ. Astron. Soc. Pacific, 74, 129, 1962) emphasizes that all the lines in the photographic region of the spectrum are blended and that the mass-ratio should be determined from measures of the D-line. He has since published values of 1.4 MSol for the mass of each component (Adv. Astron. Astrophys., 5, 85, 1967) which imply a considerably smaller value of K2 than found by Joy. A photographic light curve was obtained by L. Plaut (Bull. Astron. Inst. Netherl., 9, 121, 1940) and rediscussed by S. Kriz (Bull. Astron. Inst. Csl, 16, 306, 1965) who found i=81.4 deg and the fractional luminosity of the primary star to be 0.76. The star is the brighter component of A.D.S. 10152: companion is 8.8m at 8.2". The velocity of B as measured by Joy and the positional measurements indicate that these stars share a common motion. System917Orbit1End System918Orbit1Begin This is a cataclysmic variable containing a white dwarf (elements on upper line) and a red dwarf. The magnitudes give the approximate range of variation in V. The orbit is assumed circular and the epoch is the approximate time of superior conjunction of the white dwarf. The spectrum of the secondary is described as `early-to-middle K'. The white-dwarf velocities are derived from measures of the wings of the emission lines, specifically H-alpha and H-beta. Absorption lines, one of which is presumably a blend of Fe I and Ca I lead to the value derived for K2. Both absorption and emission lines give different values for V0 in different years. The value derived from the absorption lines is especially uncertain. System918Orbit1End System919Orbit1Begin This system was studied in a survey of members of the cluster N.G.C. 6231 and the related association Sco OB1. The observations are few and show a fairly large scatter. The epoch is T0. System919Orbit1End System920Orbit1Begin System920Orbit1End System921Orbit1Begin The epoch is the time of primary minimum and the orbit was assumed to be circular on the basis of photometric measurements. The scatter of observations is fairly large, and coverage of the velocity-curve is incomplete. Photoelectric light-curves in yellow and blue light have been published by K.C. Leung (Astron. J., 79, 852, 1974). He found i=81.7 deg and a fractional luminosity of 0.95 for the larger star in yellow light. Somewhat different results were obtained by K.C. Leung and R.E. Wilson (Astrophys. J., 211, 853, 1977) where further discussion of the system will be found. Observations of the spectrum with IUE are reported by J.S. Shaw and E.F. Guinan (Bull. Am. Astron. Soc., 15, 926, 1983). System921Orbit1End System922Orbit1Begin Epoch is T0. Approximate elements have also been published by A.C. Maury (Pop. Astron., 29, 22, 1921) while J. Sahade and L. Garcia de Ferrer (Bol. Assoc. Arg. Astron., 26, 69, 1981) report new observations that lead to a different velocity-curve from that found by Struve, but give no details. W.J. Luyten (Publ. Minnesota Obs., 2, 38, 1935) discussed Maury's observations from the point of view of apsidal motion, but Struve found no detectable eccentricity. Photoelectric observations have been published by P. Rudnick and C.T. Elvey (Astrophys. J., 87, 353, 1938) and D.W.N. Stibbs (Mon. Not. Roy. Astron. Soc., 108, 398, 1948). The latter have been twice re-analyzed recently (B. Cester et al. Astron. Astrophys., 61, 469, 1977 and D.P. Schneider, J.J. Darland and K.-C. Leung, Astron. J., 84, 236, 1979). Both groups find an orbital inclination somewhat over 60 deg and a fractional luminosity (in B) for the hotter star between 0.6 and 0.7. The two spectral types are similar, according to Struve, but there are discordant remarks in the literature. Reference: O.Struve, Festschrift fur Ellis Stromgren,, 258, 1940 System922Orbit1End System923Orbit1Begin These orbital elements have been determined from objective-prism spectra and the value of V0 is relative. The absolute value is believed to be close to 30 km/s and the system is probably a member of the Sco OB 1 association and possibly of the cluster N.G.C. 6231. The epoch is T0 and the orbit is assumed circular. The next nine entries in the Catalogue are actual or possible members of N.G.C. 6231. System923Orbit1End System924Orbit1Begin The identification number is from the C.P.D. System924Orbit1End System925Orbit1Begin Velocity-curves defined only by points near the nodes that show a large scatter. System925Orbit1End System926Orbit1Begin The velocity curve is not well covered. System926Orbit1End System927Orbit1Begin The new observations supersede those by O. Struve (Astrophys. J., 100, 189, 1944) who apparently derived an incorrect period (3.10d). The observations still show a large scatter. The epoch is T0. The light of the system is slightly variable. System927Orbit1End System928Orbit1Begin The identification number is from the C.P.D. Half the velocity-curve is well covered, as is the other node, but the scatter is large. System928Orbit1End System929Orbit1Begin The first study of the orbit of this system was by O. Struve who could not rule out a period of about 1.5d. G. Hill et al. (Astrophys. J., 79, 1271, 1974) confirmed the long period and drew attention to a possible light variation but gave no new elements. Seggewiss has refined the period found by Struve and thereby improved the velocity-curve. The orbit was assumed circular and the epoch is the average date of maximum radial velocity for the emission-line curves. Different lines give different elements and the values given in the Catalogue are means of the emission (WR) components on the upper line and of the H and He II absorption (O-type) component on the lower. W. Neutsch, H. Schmidt and W. Seggewiss (Mitt. Astron. Gesells., 43, 148, 1977) have published a short note on the shell surrounding the Wolf-Rayet component. System929Orbit1End System930Orbit1Begin See note for HD 151910. System930Orbit1End System931Orbit1Begin See note for HD 151910. Since this orbit has an appreciable eccentricity, the epoch is the time of periastron passage. System931Orbit1End System932Orbit1Begin These elements supersede those derived by G. Hill et al. (Astron. J., 79, 1271, 1971) and E.N. Walker (Mon. Not. Roy. Astron. Soc., 152, 333, 1970). The agreement with the last-named is fair, but there are differences in the velocity-curves derived from measures of different lines and the value of V0 is affected by the stellar wind from the primary. The reality of the eccentricity is questionable, but the epoch is the nominal time of periastron passage. Photometric observations (UBV) have been published by A.W.J. Cousins and H.C. Lagerwey (Mon. Notes Astron. Soc. South Africa, 28, 120, 1969). The light-curve is dominated by the ellipticity effect and the eclipses, if any, are very shallow. Analyses have been published by I.D. Howarth and R. Wilson (I.A.U. Colloq. No. 59, p. 481, 1981) and by I.D. Howarth (Mon. Not. Roy. Astron. Soc., 203, 1021, 1981). The orbital inclination is close to 75 deg and well over 90 percent of the total light comes from the component whose spectrum is visible. Howarth estimates that the invisible secondary is a B2 V star. Earlier, detection of an X-ray burst in the field of this star (R.S. Polidan et al., Astrophys. J., 233, L7, 1979) had led to speculation that the secondary might be a black hole. Howarth (Mon. Not. Roy. Astron. Soc., 206, 625, 1983) has also described the IUE spectrum, while P. Massey et al. (Astrophys. J., 231, 171, 1979) have discussed the variable H-alpha emission. This is the last of the group of stars belonging to N.G.C. 6231. System932Orbit1End System933Orbit1Begin Epoch is T0, derived from the time of minimum given in Finding List. Photoelectric light-curves have been obtained by A.R. Hogg and G.E. Kron (Astrophys. J., 60, 100, 1955) and A.M. van Genderen (Bull. Astron. Inst. Netherl., 16, 151, 1962). Both were difficult to solve. K.K. Kwee and A.M. van Genderen (Astron. Astrophys., 126, 94, 1983) have obtained new observations and analyzed them by the method of Wilson and Devinney. They find a system of two highly distorted stars and need to introduce third light. The orbital inclination is about 78 deg and the brighter component produces nearly all the light. J.K. Kaluzny (Acta Astron., 35, 327, 1985) obtains similar results. System933Orbit1End System934Orbit1Begin These elements supersede those previously published by Harper (Publ. Astron. Soc. Pacific, 44, 260, 1932). Elements have also been derived by G.A. Shajn and O.A. Melnikov (Pulkovo Obs. Circ., 19, 11, 1936). They agree closely with Harper's values, but this is partly because the Victoria observations were used together with the Crimea observations. The combination revealed a small systematic difference between velocities determined at the two observatories. The elements determined from the Victoria observations alone have been preferred, since they are based on the more homogeneous set. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. System934Orbit1End System935Orbit1Begin This is a poorly observed system both photometrically and spectroscopically. The epoch is T0 (as computed from the light elements quoted by Struve from S. Gaposchkin, Veroff. Berlin-Babelsberg, 9, part 5, 1932). Struve believed, however, that the eclipse was late, since he did not observe the full range of 2.4m. The velocity-curve is distorted by the rotation effect. Gaposchkin's photographic light-curve leads to an estimated orbital inclination of 84 deg and light-ratio of about 0.08. A. Akazaki (Publ. Astron. Soc. Japan, 32, 445, 1980) obtained spectrograms and measured the surface gravity of the primary star. He concludes that the system is a normal Algol-type system and not of the `R CMa type'. System935Orbit1End System936Orbit1Begin The new observations by Duerbeck and Teuber agree well with E.G. Ebbighausen's earlier work (Astron. J., 72, 392, 1967), but not with results derived from observations by Wellmann and published by H. Mauder (Z. Astrophys., 55, 59, 1962). The epoch is the time of primary minimum (the period appears to have been constant since 1941). The orbit was assumed circular since an elliptical solution showed the eccentricity not to be significant statistically. A photoelectric light-curve was published by B. Cester (Mem. Soc. Astron. Ital., 30, 287, 1959) who found an orbital inclination of about 79 deg and a fractional luminosity for the primary star of 0.9. Mauder's (loc. cit.) results are similar and he computed the secondary's spectral type, as given in the Catalogue. E.C. Olson and E.W. Weis (Astrophys. J., 79, 642, 1974), who found some evidence of gas streams in the system, gave the secondary spectral type as F7 V. Duerbeck and Teuber adopt F9 IV. The V magnitude, at or near maximum, is taken from R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 79, 101, 1975). The magnitude at minimum is estimated from Cester's value for the depth of eclipse. System936Orbit1End System937Orbit1Begin The new discussion of the orbital elements of the X-ray component, by J.E. Deeter, P.E. Boynton and S.H. Pravdo, supersedes that used in the Seventh Catalogue (i.e. H. Tananbaum et al., Astrophys. J., 174, L143, 1981) as well as other investigations such as those by P.J.N. Davison and A.C. Fabian (Mon. Not. Roy. Astron. Soc., 178, 1P, 1977) and P.C. Joss et al. (Astrophys. J., 235, 592, 1980). The orbital elements are derived from the variations of the X-ray pulsation period and thus a sin i, the quantity determined, is known very accurately and K1 is once again the derived quantity. The orbit is assumed circular since the eccentricity can be shown to be very much less than 0.01 (by some orders of magnitude). The epoch, which is expressed in ephemeris time for the barycentre of the solar system, is the time of mean longitude 90 deg, and is approximately the time of X-ray eclipse. No value of V0 can be determined. The optical component can also be observed, but measures of its spectrum are very uncertain. The latest are by J.B. Hutchings et al. (Astrophys. J., 292, 670, 1985) which supersede earlier studies by D. Crampton and J.B. Hutchings (Astrophys. J., 191, 483, 1974) and D. Crampton (ibid., 187, 345,, 1974). The `orbital elements' derived from hydrogen and helium lines vary with the 35-day `on-off' cycle of the X-ray source. In this respect, the lines of ionized calcium appear more stable and lead to K2 approx 85 km/s, V0 approx 60 km/s, but elements of the optical component remain very uncertain. The optical spectrum varies from B1 V to F0 V, which is ascribed to the heating effect of the X-ray component. This effect is also demonstrated by the optical pulsations (J. Middleditch and J. Nelson, Astron. J., 208, 567, 1976 and J. Middleditch, ibid., 275, 278, 1983). From these, Middleditch and Nelson derive an orbital inclination of 87 deg and masses of 1.3 MSol (X-ray component) and 2.2 MSol. Observations of HZ Her with IUE are discussed by A.K. Dupree et al. (Nature, 275, 400, 1978) and I.D. Howarth and B. Wilson (Mon. Not. Roy. Astron. Soc., 204, 1091, 1983). Other studies include J.B. Hutchings and D. Crampton (Astron. Astrophys., 52, 441, 1977 -- the emission line at He lambda 4686 and the precessing disk model), B. Margon and J.G. Cohen (Astrophys. J., 222, L33, 1978 -- study of line profiles) and C.-C. Wu et al. (Publ. Astron. Soc. Pacific, 94, 149, 1982 -- the ultraviolet light-curve). System937Orbit1End System938Orbit1Begin The new observations give elements that agree well with those obtained earlier by W.E. Harper (Publ. Dom. Obs., 4, 243, 1918) and revised by him (Publ. Dom. Astrophys. Obs., 6, 236, 1935). The system can now be considered well known. System938Orbit1End System939Orbit1Begin Heard and Hurkens report that there is no difficulty in distinguishing the components at a dispersion of 12 A/mm although the difference in line strengths is not great and they found no obvious difference in the spectral types. System939Orbit1End System940Orbit1Begin Shallow eclipses (0.04m and 0.02m) are observed. Emission H and K lines are found in the spectrum. Elements were also derived by J.S. Plaskett (J. Roy. Astron. Soc. Can., 4, 460, 1910). The two sets of elements are in good agreement. Lucy & Sweeney adopt a circular orbit. F. Hinderer, from photoelectric observations, finds i=82.4 deg, Delta m=3.44 (Astron. Nachr., 284, 1, 1958). He also gives for the masses 2.8 MSol and 1.3 MSol, and for the spectral types gG1 and dA8 to dF0. D.F. Gray (Astrophys. J., 251, 155, 1981 and 262, 682, 1982) discusses the rotation of the primary and turbulence in its atmosphere. Star is brighter component of A.D.S. 10242: B is 11.2m at 76.2". System940Orbit1End System941Orbit1Begin Elements derived by W.E. Harper (J. Roy. Astron. Soc. Can., 3, 477, 1909; 4, 302, 1910; Publ. Dom. Astrophys. Obs., 6, 237, 1935) are vitiated by his failure to recognize the effects of blending of the secondary component. Harper found K=52 km/s. Luyten's elements are based on observations by R.H. Baker (Publ. Allegheny Obs., 2, 21, 1910). Baker fixed the value of T to obtain the orbital elements. Luyten avoided this by giving the epoch T0. Petrie(I) found Delta m=1.50, and that spectral types are A0, A2. System941Orbit1End System942Orbit1Begin The authors describe the two spectra as differing `only slightly in character and intensity'. System942Orbit1End System943Orbit1Begin This is the optical counterpart of the X-ray source 3U 1700 37. The new determination of orbital elements supersedes that by J.B. Hutchings (Astrophys. J., 192, 677, 1974) as well as earlier ones, including E.N. Walker (Mon. Not. Roy. Astron. Soc., 162, 151, 1973), G. Hensberge et al. (Astron. Astrophys., 29, 69, 1973), J.B. Hutchings et al. (Mon. Not. Roy. Astron. Soc., 163, 13P, 1973) and S.C. Wolff and and N.D. Morrison (Astrophys. J., 187, 69, 1974). The epoch is the time of the middle of X-ray eclipse. Different lines give different orbital elements, but the mean from all lines is not very different from the values from the He II absorption lines given in the Catalogue. While the actual value of the eccentricity is uncertain, J.B. Hutchings (Astrophys. J., 226, 264, 1978) found that the light-curve definitely indicates an elliptical orbit; he also estimated i=87 deg. Hammerschlag-Hensberge gives no value for V0. The one in the Catalogue is estimated from her graphical representation of the velocity-curve. The epoch is the time of mid-eclipse of the X-ray source. Reports of coronal emission lines in the spectrum (A.K. Dupree, S.L. Baliunas and J.B. Lester, Astrophys. J., 218, L71, 1977) were not confirmed by later investigations (D.L. Lambert and J. Tomkin, Astrophys. J., 228, L37, 1979 and J.B. Lester, ibid., 231, 164, 1979). Spectrophotometric observations are reported by J. Dachs (Astron. Astrophys., 47, 19, 1976) and G.G. Fahlman and G.A.H. Walker (Astrophys. J., 240, 169, 1980) who find evidence for gas streams in the system. Ultraviolet light-curves have been published by G. Hammerschlag-Hensberge and C.-C. Wu (Astron. Astrophys., 56, 433, 1977). Observations with IUE have been published by A.K. Dupree et al. (Nature, 275, 400, 1978) and a brief report on observations with Voyager has appeared (T.E. Carone and R.S. Polidan, Bull. Am. Astron. Soc., 18, 946, 1986). System943Orbit1End System944Orbit1Begin Elements for the primary component alone were also published by R.F. Sanford (Astrophys. J., 86, 153, 1937). Popper also made photoelectric observations and found i=89.4 deg and the light-ratio to be 0.96. The star whose spectrum shows slightly stronger lines is in front at minima given by J.D. 2,435,648.775 + 4.183511E. This is the less massive star, but the two stars are so nearly equal, that no contradiction of the mass-luminosity relation can be regarded as established. B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978) re-analyzed Popper's photometric observations, finding almost the same value for the inclination but reversing the light-ratio. The epoch is T0 for the star with the stronger spectrum. System944Orbit1End System945Orbit1Begin Christie wrote, `Other widely different velocity-curves also represent the observational data, but the one here published seems the most probable'. The star has been suspected of variation in its light. System945Orbit1End System946Orbit1Begin This is an eclipsing dwarf nova that usually shows an emission-line spectrum, although on one occasion an absorption spectrum of approximately solar type was reported. During quiescent phases, the out-of-eclipse V magnitude is within a few tenths of 15.0m (N. Vogt, Astrophys. J. Supp., 53, 21, 1983, A. Bruch, Inf. Bull. Var. Stars, No. 2287, 1983). Eclipses are about two magnitudes deep in V, The epoch is the time of mid-eclipse as given by K. Beuermann and M.W. Pakull (Astron. Astrophys., 136, 250, 1984). The orbit was assumed circular and the value given for K1 is the mean obtained from measures of H-beta and H-gamma. Values of V0 derived from the two lines are very different, however: 55 km/s and 35 km/s respectively. The results of high-speed photometry have been published by B. Warner and M. Crocker (Mon. Not. Roy. Astron. Soc., 203, 909, 1983) and the system has also been discussed by M.C. Cook and C.C. Brunt (ibid., 205, 465, 1983). System946Orbit1End System947Orbit1Begin This is the fainter component of A.D.S. 10345, for which a number of orbits have been computed. Even the period of the visual pair is uncertain, however, except for the fact that it is to be measured in centuries. The component A is similar in magnitude and spectral type. Ishida finds evidence for a low-amplitude variation in the velocity of B, which he ascribes to binary motion. Confirmation is desirable. There is also a companion C, 13.8m at about 13". System947Orbit1End System948Orbit1Begin Lucy & Sweeney confirm the reality of the orbital eccentricity. An 8.9m companion at 3" is listed in I.D.S. System948Orbit1End System949Orbit1Begin The spectrum is classified as A1 from the K line and A7 from the metallic lines. System949Orbit1End System950Orbit1Begin System950Orbit1End System951Orbit1Begin Epoch is T0 for primary component. Circular orbit was assumed. Emission observed at H and K in spectra of both components at all phases. Reasonable combinations of spectral types and luminosity classes indicate 1.0<=Delta m<=1.3, consistent with the difficulty of measurement of the secondary. J.G. Stacy, R.E. Stencel and E.J. Weiler (Astron. J., 85, 858, 1980) observed the system as a possible RS CVn object and find evidence for a period change since the observations of Bennett et al. According to I.D.S. there is a 13m companion at 33". System951Orbit1End System952Orbit1Begin All elements of this cataclysmic variable must be considered uncertain, since there is doubt about the period. Photometric observations by A.V. Baidak et al. (Inf. Bull. Var. Stars, No. 2676, 1985) lead to a period of about 0.114d. The magnitude is variable and the one given in the Catalogue is an approximate indication of the system's brightness. The epoch is the time of inferior conjunction of the emission-line source and the orbit is assumed circular. System952Orbit1End System953Orbit1Begin The epoch is T0 and a circular orbit is assumed. This `atypical' W UMa system has attracted several photometric observers and investigators. Light-curves have been published by L. Binnendijk (Astron. J., 66, 27, 1961) who also gave the spectral types as F2 and F6, B.B. Bookmyer (Publ. Astron. Soc. Pacific, 84, 566, 1972), E.J. Woodward and R.E. Wilson (Astrophys. Space Sci., 52, 387, 1977) and T.A. Nagy (Publ. Astron. Soc. Pacific, 97, 1005, 1985). Analyses of these light-curves were made by the observers and by P.G. Niarchos (Astrophys. Space Sci., 47, 79, 1977, 58, 301, 1978) and S.R. Jabbar and Z. Kopal (ibid., 92, 99, 1983). All agree in finding an orbital inclination roughly within the range 75 deg to 80 deg and a fractional luminosity (in yellow) for the larger star of about 0.89. The star is the brighter component of A.D.S. 10408: B is 12.0m at 4.5". The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System953Orbit1End System954Orbit1Begin A few photographic observations were included in the period determination; otherwise the elements are derived entirely from photoelectric observations. System954Orbit1End System955Orbit1Begin Epoch is T0.Lucy & Sweeney adopt a circular orbit. An orbit was published earlier by R.F. Sanford (Astrophys. J., 53, 201, 1921). Agreement between the two orbits is good except for the value of K1 (Sanford finds K1=29.64 km/s). Since the formal probable errors of both solutions are small, the matter should be further investigated. The discrepancy is perhaps partly due to Sanford's inability to resolve the circumstellar Ca I line detected by Deutsch in the spectrum of both components of the visual binary. From his spectroscopic data, Deutsch inferred the masses of the three stars (alpha Her A, and the two components of the spectroscopic binary) to be 15 MSol, 4.1 MSol and 2.5 MSol, and their absolute visual magnitudes to be 2.4m, 0.3m and +1.8m, respectively. The spectral type of the fainter component of the spectroscopic binary is inferred to be A3 V. The system is one of the fainter components of A.D.S. 10418: A is 3.5m at 4.6". Two other much fainter components are listed in I.D.S. Deutsch's discovery of circumstellar lines in the spectra of both A and B leaves no doubt that these two stars form a physical system. System955Orbit1End System956Orbit1Begin Other spectroscopic studies have been published by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 138, 1919), A. Abrami, (Trieste Contr., No. 283, 1958, rediscussed by A. Krancj, Publ. Bologna Univ. Obs., 7, No. 11, 1959), D.M. Popper and R. Carlos (Publ. Astron. Soc. Pacific, 82, 762, 1970) and D. Holmgren (Bull. Am. Astron. Soc., 19, 709, 1987). Plaskett, Pearce and Popper and Carlos all agree well together; Abrami and Holmgren derive somewhat lower values of K1 and K2. Holmgren's observations were made with a Reticon, but he has not yet published enough details for an assessment to be made. Pearce's observations have the smallest formal errors of the older sets, but Popper and Carlos used higher dispersion and are almost certainly correct in treating the orbit as circular. The masses derived are scarcely affected by the choice between these two sets of observations. J.A. Eaton and D.H. Ward (Astrophys. J., 185, 921, 1973) have published photoelectric light-curves obtained from OAO-2. R.H. Koch and C.A. Koegeler (Astrophys. J., 214, 423, 1977) have also published a photoelectric study and have questioned the usual assumption that the hotter, more massive star is the more luminous (see, however, D.M. Popper, Astrophys. J., 220, L11, 1978, for comments on this matter). Koch and Koegeler also suggested that apparent changes in the period might be explained by the presence of a third body with an orbital period of about 42 years. B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) reanalyzed the photometric observations and found an orbital inclination close to 88 deg and a fractional luminosity of 0.63 (at lambda 4250) for the hotter star. G.V. Coyne S.J. (Ric. Astron. Spec. Vatican, 8, 105, 1950) found variable polarization in the light of this star. The maximum V magnitude given in the Catalogue is from R.W. Hilditch and G. Hill (Mem. Roy. Astron. Soc., 79, 101, 1975): that at minimum is from G.F.G. Knipe (Republic Obs. Circ., 8, 6, 1971). The star is the brighter component of A.D.S. 10428: B is 13.0m at 20.4". System956Orbit1End System957Orbit1Begin Earlier orbital studies have been published by R.H. Baker (Publ. Allegheny Obs., 1, 77, 1909) rediscussed by E.F. Carpenter (Publ. Astron. Soc. Pacific, 43, 30, 1920), W.J. Luyten et al. (Publ. Yerkes Obs., 7, 251, 1939), B. Smith (Astrophys. J., 102, 500, 1945) and B.J. Kovachev and W. Seggewiss (Astron. Astrophys. Supp., 19, 395, 1975). The various sets of elements agree fairly well. The minimum magnitude given is an approximate estimate. The spectral types are inferred from the solution of the light-curve, but are within the range defined by the various direct classifications to be found in the literature. The epoch is the time of primary minimum. Hilditch assumed a circular orbit after an elliptical solution gave an eccentricity smaller than its mean error. This brings the velocity-curve into agreement with the light-curve, although most earlier spectroscopic investigators have believed the small eccentricity to be real. Hilditch uses observations obtained over an interval of 37 years and points out that, if the eccentricity were real, there should have been detectable apsidal motion in that time. In fact, all the observations define one velocity-curve (including a rotation effect) very clearly. The velocities of the secondary component show a much larger scatter than those of the primary. The value of K2 given in the Catalogue is determined by Irwin's method separately from the orbital solution for the primary star (Irwin's method gives a slightly higher value for K1 and leads to a different value for V0). Hilditch has also analyzed the light-curves (approximately B, V) published by P. Rovithis and H. Rovithis-Livaniou (Astrophys. Space Sci., 70, 483, 1980). He finds an orbital inclination of about 79 deg and a visual-magnitude difference of 1.63m. Other recent photometric discussions are by B. Cester et al. (Astron. Astrophys., 61, 469, 1977) S. Soderhjelm (ibid., 66, 161, 1978), G. Giuricin, F. Mardirossian and M. Mezzetti (Astron. Nachr., 304, 37, 1983) and P. Provoost (Astron. Astrophys., 81, 17, 1980). Of particular interest is J.A. Eaton's (Acta Astron., 28, 601, 1978) discussion of OAO light-curves, which show the primary component to be variable. Hilditch suggests that it may be a beta Cep star. System957Orbit1End System958Orbit1Begin The V magnitude is estimated from the results of unpublished measurements on the Copenhagen system. System958Orbit1End System959Orbit1Begin The new observations supersede earlier ones by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 207, 1920) which were rediscussed by R.H. Baker (Publ. Univ. Missouri Obs., No. 31, 1921) and by Luyten. The epoch given is the time of primary minimum and the orbit was assumed circular. Popper's results have led to an appreciable reduction of the masses of the two components. The magnitudes given for minimum and maximum light are derived from Popper's own UBV observations. He classifies the primary spectrum as A5 from the K line and A8-F0 from the metallic lines: its metallicism had not previously been recognized. From the B V colours he infers the F0 spectral type for the secondary. His discussion of the light-curve is based on his own observations and the analysis of more complete ones by R.A. Botsula (Izv. Astron. Obs. Engelhardt, 36, 240, 1968). He gives i=87.0deg and the fractional luminosity of the hotter stars (in V) is 0.64 (compare Petrie(I) Delta m=0.80). He comments on instabilities in the light-curve and points out that the observed ratio of surface brightnesses (1.58) is nearly 25 percent greater than expected from scales of stellar fluxes and the observed colours. Another photoelectric light obtained by M. Vetesnik and J. Papousek (Bull. Astron. Inst. Csl, 24, 57, 1973) and re-analyzed by B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978) gives very similar results. Vetesnik and Papousek also present evidence for a periodic variation in the period. If it is real and caused by a third body, the orbital period is about 48 years. System959Orbit1End System960Orbit1Begin Magnitude and spectral type are variable since this is a Cepheid and the orbital motion has had to be separated from the pulsational velocity-variation. System960Orbit1End System961Orbit1Begin W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 238, 1935) found no need to revise the period, but he did suggest the value of K2 might need to be increased. New observations by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976), however, agree so well with Parker's elements that those investigators adopted the old elements. Petrie(II) found Delta m=0.58. System961Orbit1End System962Orbit1Begin A triple system consisting of a short-period pair of A0 stars accompanied by the G star which forms the secondary of the long-period system. For the long-period pair the value of K1 refers to the centre of mass of the close pair. The two members of the short-period pair are practically indistinguishable in mass and luminosity and the epoch adopted is T0 with one star arbitrarily chosen as the primary. The value of V0 for the short-period pair is variable. McLaughlin believed that the two orbits were not coplanar. System962Orbit1End System963Orbit1Begin A triple system consisting of a short-period pair of A0 stars accompanied by the G star which forms the secondary of the long-period system. For the long-period pair the value of K1 refers to the centre of mass of the close pair. The two members of the short-period pair are practically indistinguishable in mass and luminosity and the epoch adopted is T0 with one star arbitrarily chosen as the primary. The value of V0 for the short-period pair is variable. McLaughlin believed that the two orbits were not coplanar. System963Orbit1End System964Orbit1Begin System964Orbit1End System965Orbit1Begin Magnitudes are from the fourth edition of the G.C.V.S. No indication of spectral type is given, but the star is a U Gem variable. Ranges are given for both semi-amplitudes, and the values in the Catalogue are means. These elements can be no more than a rough indication of the characteristics of the orbit. No information is given about the epoch. Reference: W.Wargau \& N.Vogt, Mitt. A.G., 55, 77, 1982 System965Orbit1End System966Orbit1Begin Luyten computed very similar elements from these observations but commented that the uncertainty in omega was probably much greater than Christie's published value. Lucy & Sweeney adopt a circular orbit. System966Orbit1End System967Orbit1Begin The star was studied as a possible optical counterpart of the X-ray source 3U 1727 33. No definite connection has been established. The scatter of individual velocity measurements is very large. Penny et al. do not give a numerical value of V0; we have estimated one from their velocity-curve. There is no certain evidence of any variation in light. Three companions are listed in I.D.S.: 9.6m at 4.4", 11.5m at 14.6", and 9.4m at 58.7". The radial velocity, spectral type, and apparent magnitude of B are consistent with it being physically related to the spectroscopic binary. System967Orbit1End System968Orbit1Begin The spectral types are not exactly known and that of the secondary is determined from IUE observations. The epoch is T0 and the orbit was assumed circular after a preliminary solution showed that the eccentricity could not be significantly determined. The value of K2 is derived from a rather small number of observations. Light variations displayed by this chromospherically active giant star are ascribed to starspots. System968Orbit1End System969Orbit1Begin This is the visual binary Sigma 2173 or A.D.S. 10598. It was first resolved spectroscopically by F.R. West (Astron. J., 71, 186, 1966). The period of 46.08y and periastron passage of 1916.06 were assumed from the orbit by R.L. Duncombe and J. Ashbrook (Astron. J., 57, 92, 1952), together with the value given for e and omega. The quality classification refers only to the spectroscopically determined values of K1, K2 and V0. In fact the quantity determined spectroscopically is the maximum velocity difference (12.36 km/s). The value of V0 is estimated from unresolved plates, and K1 and K2 have been assumed equal, although the astrometric measurements show a slight difference between the masses (consistent with the observed Delta m=0.1). The total mass found spectroscopically agrees well with that found astrometrically. A new orbit by R.H. Wilson (Mon. Not. Roy. Astron. Soc., 177, 645, 1976) is similar to that by Duncombe and Ashbrook except that P is given as 46.40y and T as 1962.46. System969Orbit1End System970Orbit1Begin Elements have also been independently determined by W.I. Beavers and J.J. Salzer (Publ. Astron. Soc. Pacific, 95, 79, 1983) whose results agree well with those of Lucke and Mayor, despite uncertainty of a few days in the period. There is also a visual companion (A.D.S. 10607) of approximately equal brightness. System970Orbit1End System971Orbit1Begin The elements given for this cataclysmic variable are derived from measures of the H-alpha emission. The He II emission line at lambda 4686 gives a similar value for the semi-amplitude but a very different value (+81 km/s) for V0. No information is given about the epoch. System971Orbit1End System972Orbit1Begin New observations by Stickland and Weatherby permit a refinement of the period. The other elements agree well with those determined by J.W. Campbell (Publ. Astron. Soc. Pacific, 2, 159, 1922), whose observations were used in the derivation of the new elements. Lucy & Sweeney accepted the small eccentricity, found also by Campbell. The star is now recognized as a mercury-manganese star. System972Orbit1End System973Orbit1Begin The epoch is primary minimum, and the orbit was assumed to be circular, in accord with the light-curve. Bell and Malcolm derive an orbital inclination close to 65 deg and find Delta V=0m. Similar spectroscopic elements were deduced by J. Andersen, B. Nordstrom and R.E. Wilson (Astron. Astrophys., 82, 225, 1980). The system is a member of the open cluster N.G.C. 6383. System973Orbit1End System974Orbit1Begin The binary nature of this star was pointed out by R.J. Trumpler (Publ. Astron. Soc. Pacific, 42, 342, 1930) but he could not decide between the possible periods of 3.368d and 4.920d. Two independent and nearly simultaneous studies demonstrated that the shorter value was more nearly correct (W. Seggewiss and M. de Groot, Astron. Astrophys., 51, 195, 1976; P.S. Conti et al. Publ. Astron. Soc. Pacific, 87, 327, 1975). The new study by Lloyd Evans is characterized by a slightly smaller observational scatter and has been preferred. There is evidence for a variation in V0, over a range of 16 km/s, suggesting that the system may be triple. The light of the star is slightly variable (Delta Vapprox 0.04m) and the system appears to be an ellipsoidal variable (J.C. Thomas, Bull. Am. Astron. Soc., 7, 533, 1975). The two components are closely similar in brightness and the orbital inclination is around 46 deg. The star is a member of the cluster N.G.C. 6383 and two faint companions are listed in I.D.S. System974Orbit1End System975Orbit1Begin The orbit of this A-type W UMa system was assumed circular, in accord with the light-curve. The epoch is the time of primary minimum. The value of K2 is very uncertain. Schoffel finds that the orbital inclination is close to 82 deg and the ratio of luminosities (in visual light) is 0.31. Other discussions of the light-curve have been published by K.-C. Leung and D.P. Schneider (Astrophys. J., 222, 917, 1978) and by Z. Kopal and S.R. Jabbar (Astrophys. Space Sci., 92, 99, 1983). System975Orbit1End System976Orbit1Begin The new elements are considered by Abt and Levy to be an improvement over those previously published by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961). The period, however, is still uncertain in the first decimal. The eccentricity given is less than its own uncertainty. The spectral type is given as A2.5, A8 and F1, according to the K line, hydrogen lines and metallic lines, respectively. The star has a common proper motion with nu 1 Dra, also an A-type star and of almost the same brightness. Together they form A.D.S. 10628, nu 2 being conventionally designated A. The separation of A and B is 61.9". System976Orbit1End System977Orbit1Begin Lucy & Sweeney adopt a circular orbit. System977Orbit1End System978Orbit1Begin We have adjusted Young's value for the epoch to make it T0. A 13.0m companion at 25.1" is listed in I.D.S. System978Orbit1End System979Orbit1Begin The scatter of observations about the velocity-curve is large, but a similar period and range of variation were suspected in other data studied by K. Kodaira (Publ. Astron. Soc. Japan, 23, 159, 1971). There may be a short-period variation superposed on the orbital motion. A 12m companion listed in I.D.S. at 116" is probably optical. System979Orbit1End System980Orbit1Begin There is a systematic difference between the Haute Provence observations and the Mount Wilson observations which might indicate that V0 is variable. System980Orbit1End System981Orbit1Begin The new elements obtained by Abt and Levy are preferred to the old ones of A.B. Turner (Lick Obs. Bull., 4, 163, 1907) because the later observers successfully resolved the secondary spectrum. The agreement between the two sets is good for K1 and V0. Since e is small the differences in omega are not important. Both Luyten and Lucy & Sweeney have revised the original computations by Turner and have adopted circular orbits, but Abt and Levy find a larger value for e than Turner did. A brief report on UV emission-line variability in the spectrum of this star was published by R.A. Stern (Bull. Am. Astron. Soc., 15, 665, 1983). A 13.2m companion at 72.3" is listed in I.D.S.: according to Abt and Levy it shares a common proper motion with the spectroscopic binary. System981Orbit1End System982Orbit1Begin The scatter of the photoelectrically determined radial velocities, although absolutely small, is large compared with the value of K. Nevertheless, the velocity curve is well covered. General Note on I.C. 4655: Six of the next eleven stars listed in the Catalogue are members of the cluster I.C. 4655 in which H.A. Abt et al. (Astrophys. J., 171, 259, 1972) found a large fraction (over 80 percent) of spectroscopic binaries. A later study by D. Crampton et al. (Astrophys. J., 204, 502, 1976) did not confirm all the orbital elements found by Abt et al. We have excluded from the Catalogue those stars for which Abt et al. published orbital elements, but whose binary nature was not confirmed by Crampton et al. namely: H.D. 161184, 161572, 161677, 161698, and 162028. In addition, we have excluded H.D. 161603 for which Abt et al. gave orbital elements, but Crampton et al. could find no period. Those systems that were found to be binaries by both investigators have been included. We adopted the elements found for them by Crampton et al. We also included those systems for which Abt et al. determined elements but which Crampton et al. did not observe. Because of the uncertainty generated by two discordant studies, all these orbital elements have been assigned low grades of reliability. In the notes that follow `Abt et al.' and `Crampton et al.' refer to the papers cited in this note. System982Orbit1End System983Orbit1Begin One of the most uncertain sets of elements amongst the entries for I.C. 4655 (see General Note above). Abt et al. Abt et al. (Astrophys. J., 171, 259, 1972) found P=17.4d, Crampton et al. (Astrophys. J., 204, 502, 1976) could not determine a unique period, but found 5.882d to be the most probable. All the orbital elements are doubtful, and in particular the non-zero eccentricity is not regarded as significant, and the value of omega is therefore meaningless. System983Orbit1End System984Orbit1Begin The velocity variation is of a low amplitude and the scatter of observations is large. The spectrum is described as `shell' by Abt et al. (Astrophys. J., 171, 259, 1972). See General Note above. System984Orbit1End System985Orbit1Begin This is not a member of I.C. 4665. Popper's new observations supersede the earlier work by R.M. Petrie (Publ. Dom. Astrophys. Obs., 4, 81, 1928). The epoch is the time of primary minimum. Circular orbits were adopted, since the light-curve shows e cos omega to be negligibly small. The spectrum is only weakly that of an Am star and has also been classified as silicon-enhanced A-type spectrum. The minimum magnitude given is a graphical estimate. A V light-curve was published by R. Zissell (Astron. J., 77, 610, 1972). Popper re-analyzed these observations and found an orbital inclination close to 80 deg and a value of 0.80m for Delta V, although the effective temperatures of the two stars are similar. A 9.3m companion at 40" is listed in I.D.S. The relative motion is rather large for the separation, suggesting that the stars do not form a physical pair. System985Orbit1End System986Orbit1Begin This star is also not a member of I.C. 4665. The case for velocity variation depends rather heavily on a small number of Reticon observations. Confirmation is desirable, especially since the star is a supergiant. The star has a 13m companion at 37.5". System986Orbit1End System987Orbit1Begin Abt et al. find the same period but a rather higher amplitude (60.9 km/s) than that given by Crampton et al. See General Note above. Objective-prism observations have been published by F. Gieseking (Astron. Astrophys. Supp., 43, 33, 1981). System987Orbit1End System988Orbit1Begin This appears to be the star identified as H.D. 161575 by Abt et al. They find a different period (12.6d) for this system but Crampton et al. can represent the observations of Abt et al. on their period. See General Note above. System988Orbit1End System989Orbit1Begin The orbit by Crampton et al. appears well determined and includes the observations by Abt et al. who had found a different period (15.58d). See General Note above. Objective-prism observations have been published by F. Gieseking (Astron. Astrophys. Supp., 43, 33, 1981). System989Orbit1End System990Orbit1Begin This is not a member of I.C. 4665. Elements have also been published for this `mercury- manganese' star by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976). He refines P to 12.4515d and adopts a circular orbit. He also finds a somewhat larger value of K1 (59.7 km/s). Although Aikman's work is based on plates of higher dispersion, we have preferred Hube's elements which are based on many more spectrograms. The epoch he gives is T0. System990Orbit1End System991Orbit1Begin The new spectroscopic observations by Andersen supersede the earlier ones published by J. Sahade and J.L. Dessy (Astrophys. J., 115, 53, 1952). Differences between orbital elements derived from the hydrogen lines and the helium lines, ascribed by Sahade and Dessy to the effects of gas streaming, are shown by Andersen to have been primarily caused by the incomplete resolution of the two spectra. The minimum magnitude given is an estimate. The epoch is the time of primary minimum. The eccentricity, although small, is real and was determined from the light-curve. There is photometric evidence for apsidal motion, but no period can yet be determined. J.V. Clausen (Astron. Astrophys. Supp., 36, 45, 1979) published a V light-curve and derived an orbital inclination of 85 deg and a light- ratio of 0.64. Similar results were derived by G. Giuricin, F. Mardirossian and M. Mezzetti (Astron. Astrophys. Supp., 39, 255, 1980) from BV observations by G.F.G. Knipe (Astron. Astrophys., 14, 70, 1971). A 9.3m companion at 12.6" is listed in I.D.S. Spectroscopic observations by Andersen still leave open the question whether or not it is physically associated with the eclipsing pair. The system does not belong to I.C. 4665. System991Orbit1End System992Orbit1Begin The epoch is T0, the orbit having been assumed circular after an elliptical solution was found to give no significant reduction in the residuals. The star is the brighter member of A.D.S. 10782. The companion (9.7m at 7.9") shares a common proper motion with the spectroscopic pair and has a radial velocity close to the value of V0. The system does not belong to I.C. 4665. System992Orbit1End System993Orbit1Begin The last member of I.C. 4665 to be listed in the Catalogue (see General Note above). The variation in velocity seems fairly well established. System993Orbit1End System994Orbit1Begin The epoch is T0 and the orbit is assumed circular. The orbit depends on objective-prism velocities, but the plate has been calibrated so that V0 may be estimated. The star belongs to the open cluster M7 (N.G.C. 6475). System994Orbit1End System995Orbit1Begin Epoch is T0. Luyten's recomputation is preferred to the original elements derived by W.E. Harper (Publ. Dom. Astrophys. Obs., 1, 125, 1919) because Harper had to fix the value of omega to obtain a solution. Harper later revised P to 2.82374d (Publ. Dom. Astrophys. Obs., 6, 239, 1935). The mass-function from Harper's solution has been retained, since the value of K was hardly changed by Luyten. Lucy & Sweeney agree with Luyten in adopting a circular orbit. System995Orbit1End System996Orbit1Begin This is a very approximate orbit for a recurrent nova. The epoch is the date of a plate obtained near the maximum velocity. System996Orbit1End System997Orbit1Begin The epoch is the time of superior conjunction of the emission-line source. The orbit has been assumed to be circular. Even the period is known only approximately. System997Orbit1End System998Orbit1Begin Eight of the next eleven entries in the Catalogue are for stars believed to be members of the cluster N.G.C. 6475. Many of them have also been studied by F. Gieseking (Astron. Astrophys., 60, 9, 1977). He roughly confirms the elements given for this system by Abt et al., except that he finds a slightly lower value of K1 (53.4 km/s). The epoch is the time of maximum positive radial-velocity. System998Orbit1End System999Orbit1Begin These elements are not confirmed by Gieseking, who finds the velocity to be constant (see previous note). Although Abt et al. classify the spectrum as Ap, the star is not listed by either Bertaud and Floquet or Curchod and Hauck. The elements should be considered very uncertain. System999Orbit1End System1000Orbit1Begin This is not one of the stars in N.G.C. 6475. A circular orbit was assumed after an elliptical solution was found not to give a significant value for the eccentricity. The epoch is T0. Although no M-K spectral type has been published, Griffin suggests, on the basis of colours and proper motion, K1 III. System1000Orbit1End System1001Orbit1Begin The evidence for variability of the velocity of this star depends on one observation. Gieseking finds the velocity to be constant (see note for HD 162515). System1001Orbit1End System1002Orbit1Begin This star was included by H.A. Abt et al. (Astrophys. J., 159, 919, 1970) in their study of binaries in N.G.C. 6475, but Gieseking's elements are based on more observations and seem preferable (see note for HD 162515). The principal difference between the two sets is the lower eccentricity (0.23) found by Abt et al. Although Gieseking's observations were made with an objective prism he has established the absolute velocity of the centre of mass by measurements of reference stars on the same plate. Abt et al. thought that V0 varied. System1002Orbit1End System1003Orbit1Begin The epoch is T0. The reality of this low-amplitude variation should be checked. Unfortunately, Gieseking was unable to observe this star (see note for HD 162515). System1003Orbit1End System1004Orbit1Begin The evidence for the duplicity of this Cepheid variable is described as marginal by Abt and Levy themselves. The elements, including the period, are highly uncertain. This is not amongst the stars considered to belong to N.G.C. 6475. System1004Orbit1End System1005Orbit1Begin The observation of two spectra puts the binary nature of this star beyond doubt, but the scatter of individual observations is large. Unfortunately, Gieseking could not measure his spectrograms of this star. See note for HD 162515. System1005Orbit1End System1006Orbit1Begin This star is not a member of N.G.C. 6475. Attention was first drawn to a periodicity of 88 days in the velocities of 88 Her by the same authors as are cited in the Catalogue (Bull. Astron. Inst. Csl, 23, 218, 1972). Although the scatter of individual observations is large, the binary hypothesis is only one possible explanation and is perhaps made less probable by the most recent observations. P. Harmanec et al. (Bull. Astron. Inst. Csl, 29, 278, 1978) find light variations of about 0.2m, which are certainly not caused by eclipses. The spectral type is also found to vary between B6 V and B8 V. R. Hirata (Inf. Bull. Var. Stars, No. 1496, 1978) and M. Nakagiri and R. Hirata (ibid., No. 1565, 1979) identify the star as a shell star. System1006Orbit1End System1007Orbit1Begin The scatter of observations about the proposed velocity-curve is large and Gieseking finds a constant velocity. See note for HD 162515. System1007Orbit1End System1008Orbit1Begin This is the last of the stars that belong to N.G.C. 6475 listed in the Catalogue (see note for HD 162515). Abt et al. believe that V0 varies, but the observations could almost be represented by a constant velocity. System1008Orbit1End System1009Orbit1Begin K.C. Gordon and G.E. Kron (Astrophys. J., 70, 100, 1965) find from their photoelectric light-curve i=82.7 deg and the light-ratio (in yellow light) is about 0.05 and Delta m=3.3. There are difficulties in the solution of the light-curve, however, and it is not possible to satisfy both minima, in two colours, with one set of elements. The secondary component is apparently underluminous and undermassive, although overluminous for its mass. Its spectral type must be approximately F5 to G0. Lucy & Sweeney adopt a circular orbit. System1009Orbit1End System1010Orbit1Begin Earlier investigations were published by M.L. Humason and S.B. Nicholson (Astrophys. J., 67, 341, 1928); and O. Struve (Astrophys. J., 99, 210, 1944). All results are in good agreement and the adopted elements are derived from a discussion of both the old and new observations. J.B. Hutchings (Publ. Astron. Soc. Pacific, 87, 245, 1975) has published additional spectroscopic observations: he has revised the period to 12.0059d (more in accord with the light-curve) and made a corresponding adjustment to the time of periastron passage. Apart from these changes he has adopted the elements given in the Catalogue for the primary star. The most important of Hutchings' results, however, is the detection of the absorption-line spectrum of the secondary star. Sahade and Frieboes-Conde had detected only emission lines which they ascribed to the secondary and from which they deduced K2=168 km/s. The value deduced by Hutchings (110 km/s) is given in the Catalogue since it seems more likely to represent the motion of the star itself. It implies that the secondary star is more massive. Hutchings also confirms the unusual strength of lines of N II and N III and weakness of lines of C III and O II pointed out by N.R. Walborn (Astrophys. J., 176, 119, 1972). L.G. Cane, C.D. McKeith and P.L. Dufton (Mon. Not. Roy. Astron. Soc., 194, 537, 1981) find evidence for anomalous abundances of carbon, nitrogen and oxygen that are consistent with the loss of about 50 percent of the mass of the primary star by stellar winds and mass transfer. The UBV photoelectric light-curves have recently been published by B.F. Madore (Astron. Astrophys., 40, 451, 1975) and E.J. Woodward and R.H. Koch (Publ. Astron. Soc. Pacific, 87, 901, 1975). The curves, obtained, in different years, are similar in appearance: Woodward and Koch also analyze their curve for the photometric elements. They find that i=73.1 deg and that the primary gives 0.87 of the light in V. They also give what is probably the best ephemeris for predicting phases of future observations: Pr. Min.=J.D. 2,442,218.74+12.00597E. Hutchings discusses possible changes between these light-curves and earlier photographic ones by S. Gaposchkin (Astrophys. J., 89, 125, 1939; Ann. Harv. Coll. Obs., 113, No. 2, 1953). He also discusses the possible evolutionary status of the system. A 12.4m companion at 13.5" is listed in I.D.S. System1010Orbit1End System1011Orbit1Begin Individual velocities show a large scatter about the velocity-curve, partly because of the difficulty of separating the pulsations of this variable supergiant from any orbital motion that may exist. Some support for the hypothesis that this star is a binary is derived from observations of an infrared excess (F.C. Gillet, A.R. Hyland and W.A. Stein, Astrophys. J., 162, L21, 1970 and R.M. Humphreys and E.P. Ney, Astrophys. J., 187, L75; 190, 339, 1974), which is consistent with the presence of an M-type companion. System1011Orbit1End System1012Orbit1Begin The new spectroscopic results supersede the earlier work by J.F. Heard (J. Roy. Astron. Soc. Can., 59, 258, 1965) and the suggested emendations to it by J.B. Hutchings (Astrophys. J., 180, 501, 1973). The epoch is the time of primary minimum. The system has attracted many photometric investigators in recent years. Observations or solutions of the light-curve have been published by L. Binnendijk (Vistas in Astron., 21, 359, 1977), B.B. Bookmyer (Publ. Astron. Soc. Pacific, 88, 473, 1976), T.A. Nagy (ibid., 89, 366, 1977), P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978), S.J. Lafta and J.F. Grainger (ibid., 114, 23, 1985) and J.A. Eaton (who used IUE photometry -- Acta Astron., 36, 275, 1986). Binnendijk has shown the results of light-curve solutions to be somewhat model- dependent, but there seems general agreement that the orbital inclination is around 80 deg and that the larger component gives about 80 percent of the light. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). New results by G. Hill and D. Holmgren are in press. System1012Orbit1End System1013Orbit1Begin Considering the spectral types of the components, the orbital elements are unusually well determined. There are also high-quality photometric observations (J.V. Clausen, K. Gyldenkerne and B. Gronbech, Astron. Astrophys., 58, 121, 1977) which have been augmented and rediscussed by Andersen and Gimenez. These enable the values of e and omega to be fixed from contemporary light-curves. There is slow apsidal motion in the system (apsidal period about 592 years) and the value given for omega is that appropriate to the time of observation while that for T refers to an earlier date adopted as the initial epoch for the apsidal period. The two values, therefore, are not quite mutually consistent. The orbital inclination is very close to 90 deg and the visual magnitude difference between the components is 0.34m. A 9.1m companion at about 7" separation is, on the basis of its radial-velocity and likely spectral type, probably physically related to the eclipsing pair. System1013Orbit1End System1014Orbit1Begin These orbital elements are derived from objective-prism plates and the value of V0 has been set arbitrarily at zero. The epoch is the time of primary minimum and the period was determined photometrically. A discussion of ULBV observations by J. Grygar and T.B. Horak (Bull. Astron. Inst. Csl, 31, 297, 1980) leads to a value close to 89 deg for the orbital inclination and a fractional luminosity of the brighter star (in V) of about 0.68. System1014Orbit1End System1015Orbit1Begin Epoch is T0 for the primary component, a circular orbit was assumed. An earlier investigation was published by W.S. Adams and A.H. Joy (Astrophys. J., 49, 179, 1919) who found K1=88.2 km/s and K2=101.8 km/s. Popper's results are preferred because they were derived from plates of higher dispersion. The Ca II emission lines were discussed by W.A. Hiltner (Astrophys. J., 106, 481, 1987); they vary in phase with the secondary spectrum, but give V0=44.4 km/s and K2=97.7 km/s. Popper's value of K2 is a mean derived from both absorption and emission lines. The system is now regarded as an RS CVn binary, and a more recent study of the emission lines in its spectrum has been published by E.J. Weiler (Mon. Not. Roy. Astron. Soc., 182, 77, 1978). There is also a new study of the spectroscopic orbit by M.B. Babayev and D.Ch. Salmanova (Bulletin Abastumani Obs., No. 58, 163, 1985) who found K1=92.5 km/s and K2=100 km/s. They used plates of several different (and mainly low) dispersions, however, and Popper's results still seem to us to be preferable. From photometric observations, Popper derived an orbital inclination of 84 deg and a visual magnitude difference of 0.9 (cf. Petrie(II) Delta m=0.4). System1015Orbit1End System1016Orbit1Begin These are the first spectroscopic elements derived for this W UMa system which appears to be of Binnendijk's type A. The orbit was assumed circular, in accordance with the light-curve and the epoch is T0 for the brighter component. The difference found in the systemic velocities derived from the two components is not explained. Although several photoelectric light-curves have been published (P. Rovithis and H. Rovithis-Livaniou, Astrophys. Space Sci., 96, 283, 1983, E. Lapasset and J.G. Funes, ibid., 113, 83, 1985 and E. Lapasset, Inf. Bull. Var. Stars, No. 2828, 1985) no modern analysis of them appears to have been undertaken. Lu estimates that, in the photographic region, Delta m=0.57. System1016Orbit1End System1017Orbit1Begin The secondary component can be measured only because the H and K lines in its spectrum are seen in emission. (The system belongs to the RS CVn group). The eccentricity is very small and the values of T and omega are correspondingly uncertain. The light-curve by V.P. Tsessevich (Izv. Odessa Obs., 4, No. 2, 116, 1954) has been superseded by a photoelectric one obtained by J.R. Sowell et al. (Astrophys. Space Sci., 90, 421, 1983) who derived the two spectral types given, from their photometric data. They also found an orbital inclination of about 86 deg and a magnitude difference (in V) of 0.35m. System1017Orbit1End System1018Orbit1Begin This system has the second shortest period known for a Wolf-Rayet binary. The orbit is assumed circular and the epoch is the time of inferior conjunction of the W-R component. No value is given for V0. The magnitude given is a mean magnitude on the v scale. The star's light is variable in the same period as the radial-velocity. The light-curve suggests that the star is an eclipsing variable. Isserstedt and Moffat suggest that the invisible secondary is a neutron star. System1018Orbit1End System1019Orbit1Begin Reports of the variability of the velocity of this star go back to S.A. Mitchell (Science, 34, 529, 1911) who claimed to see 4 components in the spectrum. Subsequent observations yielded conflicting results and, rather surprisingly for so bright a star, these are the first orbital elements to be published. Koubsky et al. see three components in the spectrum, so V0 is probably variable -- although no period is yet known either for V0 or for the other close pair in the system. The light of the star is also slightly variable. System1019Orbit1End System1020Orbit1Begin Lucy & Sweeney adopt a circular orbit. System1020Orbit1End System1021Orbit1Begin These are the first elements for an early-type binary whose double-lined nature was discovered by P.S. Conti (Astrophys. J., 187, 539, 1974). The orbital eccentricity is probably not significant. Morrison and Conti estimate that the semi-amplitudes should be increased by about 7 percent each to allow for the effects of pair-blending. The spectrum indicates that the two components are nearly identical in luminosity and spectral type. System1021Orbit1End System1022Orbit1Begin High-dispersion spectroscopic observations by Batten, Fletcher and Campbell supersede the earlier work by A.H. Batten and E.L. van Dessel (Publ. Dom. Astrophys. Obs., 14, 345, 1976) and L. Berman (Lick Obs. Bull., 16, 24, 1932). The visual observations still supply the best values for the period (88.13y), time of periastron (1984.05), eccentricity and longitude of periastron. These values are taken from the study by M.D. Worth and W.D. Heintz (Astrophys. J., 193, 647, 1974) who also give a=4.545" and i=121.15 deg. A revised orbit, making use of both visual and spectroscopic observations is in press at the time of writing (W.D. Heintz, J. Roy. Astron. Soc. Can., 82, 140, 1988). Only K1, K2 and V0 are determined directly from the spectroscopic observations which, however, leave no doubt that the values of e and omega are close to those adopted. A few observations of the secondary star near periastron confirm that the spectroscopic and visual orbits give closely similar values for the masses of the two components. The total mass is very well determined. The mass-ratio depends on the value of V0 which must remain uncertain until the other node is covered by observations of similar precision. A quarter of a century of high-dispersion spectroscopic observation has removed all evidence for a short-period variation in the system, that could be ascribed to the effects of a third body detectable by conventional photographic spectroscopy. System1022Orbit1End System1023Orbit1Begin This is a triple system containing three dwarfs in which the long-period orbit (P=20.25y) is that of a visual binary and has the highest known orbital eccentricity, while the short-period orbit has a period of less than a day and is nearly circular. This close pair (which forms the visual primary) is also known to be an eclipsing binary (V772 Her) -- see C.D. Scarfe (Inf. Bull. Var. Stars, No. 1357, 1977). The systemic velocity of the close pair is, of course, variable, although the geometry of the visual orbit means that for much of the 20-year period the close pair and the triple system have nearly the same systemic velocity. The orbital elements for the long-period pair have been derived simultaneously from visual and spectroscopic observations. These elements are the first given for this visual pair as a spectroscopic system. The elements given in the Catalogue for the eclipsing pair are an improvement on those previously given by C.L. Morbey et al. (Publ. Astron. Soc. Pacific, 89, 851, 1977). The secondary spectrum of the eclipsing pair is not visible; the star is probably an M-type dwarf. The two visible stars show relatively rapid rotation and an appreciable lithium abundance and also display H and K emission in their spectra. This all suggests that the stars are young (F.C. Fekel, Astrophys. J., 246, 879, 1981): G.A. Bakos and J. Tremko (I.A.U. Colloq. No. 69, p. 67, 1982), who confirm the existence of eclipses, suggest that the invisible star is a T Tau star. The system is also known as a source of soft X-rays (R.A. Stern and A. Skumanich, Astrophys. J., 267, 232, 1983). The magnitude given refers to the combined light of both visual components (maximum separation 0.5"). Several other companions are listed as members of A.D.S. 11060, but the present evidence suggests that most, if not all, of them are optical. System1023Orbit1End System1024Orbit1Begin This is a triple system containing three dwarfs in which the long-period orbit (P=20.25y) is that of a visual binary and has the highest known orbital eccentricity, while the short- period orbit has a period of less than a day and is nearly circular. This close pair (which forms the visual primary) is also known to be an eclipsing binary (V772 Her) -- see C.D. Scarfe (Inf. Bull. Var. Stars, No. 1357, 1977). The systemic velocity of the close pair is, of course, variable, although the geometry of the visual orbit means that for much of the 20-year period the close pair and the triple system have nearly the same systemic velocity. The orbital elements for the long-period pair have been derived simultaneously from visual and spectroscopic observations. These elements are the first given for this visual pair as a spectroscopic system. The elements given in the Catalogue for the eclipsing pair are an improvement on those previously given by C.L. Morbey et al. (Publ. Astron. Soc. Pacific, 89, 851, 1977). The secondary spectrum of the eclipsing pair is not visible; the star is probably an M-type dwarf. The two visible stars show relatively rapid rotation and an appreciable lithium abundance and also display H and K emission in their spectra. This all suggests that the stars are young (F.C. Fekel, Astrophys. J., 246, 879, 1981): G.A. Bakos and J. Tremko (I.A.U. Colloq. No. 69, p. 67, 1982), who confirm the existence of eclipses, suggest that the invisible star is a T Tau star. The system is also known as a source of soft X-rays (R.A. Stern and A. Skumanich, Astrophys. J., 267, 232, 1983). The magnitude given refers to the combined light of both visual components (maximum separation 0.5"). Several other companions are listed as members of A.D.S. 11060, but the present evidence suggests that most, if not all, of them are optical. System1024Orbit1End System1025Orbit1Begin The variation of radial velocity was first discovered by D.P. Hube (Publ. Astron. Soc. Pacific, 83, 805, 1971) who also derived a preliminary value of the period (Inf. Bull. Var. Stars, No. 671, 1972) and suggested the system might show eclipses. The latter suggestion was confirmed by G.F.G. Knipe (Mon. Notes Astron. Soc. South Africa, 32, 116, 1973) and a light-curve has also been published by Young and Etzel. The epoch is the time of primary mid-eclipse. The two eclipses are almost equal in depth. The small orbital eccentricity is probably spurious. The light-curve is variable and has not yet been analyzed. The two components appear to be of similar spectral types. A faint visual companion is reported. System1025Orbit1End System1026Orbit1Begin A cataclysmic variable of the DQ Her type. Orbital elements are based on two nights of observation and apparently depend on measurements of H-beta in emission, but the information given in the paper about the radial-velocity measurements is sketchy. An arbitrary zero phase, not expressed by Julian date, was adopted. System1026Orbit1End System1027Orbit1Begin Earlier spectrographic observations have been published by A.H. Joy (Publ. Astron. Soc. Pacific, 39, 234, 1927); C.A. Bauer (Astrophys. J., 101, 208, 1945) and O. Struve (Publ. Astron. Soc. Pacific, 65, 185, 1953). Of these investigators, only Bauer attempted to derive the orbital elements. The elements presented in the Catalogue are derived from measures of the Mg II line, since the hydrogen emission and other shell lines were obviously unreliable. Later work (J.L. Greenstein et al. Inf. Bull. So. Hemisphere, No. 16, 40, 1970), however, shows that even the Mg II line is affected at some phases by emission and the eccentricity derived is probably spurious. The period is known to be increasing by about 14 seconds per year (R.H. Koch and E.F. Guinan Inf. Bull. Var. Stars, No. 1483, 1978). The light-curve is also very difficult to interpret (D.J.K. O'Connell, Lembang Ann., 8, 22, 1937, C.R. Lynds, Astrophys. J., 126, 81, 1957). Primary eclipse is about 1 m deep, but the light-curve does not repeat itself and cannot be explained by eclipses alone. There is variable intrinsic polarization (A. Kruszewski, Acta Astron., 22, 405, 1972)). An international campaign in 1966 led to the publication of many papers mainly in Inf. Bull. So. Hemisphere, Nos. 9, 10, 11, 15 and 16. See also R.C. Hall (Astron. J., 72, 302, 1967) and A.M. van Genderen (Astron. Astrophys. Supp., 9, 157, 1973). More recently, observation of the far UV spectrum with IUE has brought greater understanding of the system (M. Plavec and R.H. Koch, Inf. Bull. Var. Stars, No. 1482, 1978; M.J. Plavec and P.J. Sakimoto, Bull. Am. Astron. Soc., 10, 609, 1978; W. Strupat Mitt. Astron. Gesells., 62, 275, 1984, 63, 194, 1985). Plavec (I.A.U. Symp. No. 88, p. 251, 1980) sees W Ser as the prototype of a group of systems, similar in their UV spectra but diverse in their optical spectra, in the rapid phase of mass transfer, and destined to become Algol systems. System1027Orbit1End System1028Orbit1Begin The single spectrum shows the H and K lines of Ca II in emission. They give similar velocities to those derived from the absorption lines. System1028Orbit1End System1029Orbit1Begin The results of Smak's thorough discussion of his own observations and earlier ones by J.L. Greenstein and R.P. Kraft (Astrophys. J., 130, 99, 1959) and by J.B. Hutchings, A.P. Cowley and D. Crampton (Astrophys. J., 232, 500, 1979) are preferred to either of these earlier investigations. The epoch is the time of minimum and, together with the period (which is variable) is taken from the photometric investigation by J. Patterson, E.L. Robinson and R.E. Nather (Astrophys. J., 224, 570, 1978). The value of V0 is approximate. Smak estimates the orbital inclination at 77 deg. The V magnitude is taken from the photometric work of M.F. Walker Astrophys. J., 123, 68, 1956; 127, 319, 1958). Important papers on high-speed photometry of the system were published by R.E. Nather and B. Warner (Mon. Not. Roy. Astron. Soc., 143, 145, 1969); B. Warner and R.E. Nather (ibid., 152, 219, 1971) and B. Warner et al. (ibid., 159, 321, 1972). A brief discussion of polarization of light from the system was published by E.A. Dibai and N.M. Shakhovskoi (Astron. Zh., 43, 1319, 1966). Other more recent studies have been published by J.A. Petterson (Astrophys. J., 241, 247, 1980), M.E. Sulkanen, L.W. Brasure and J. Patterson (ibid., 244, 579, 1981) and E.S. Dmitrienko and A.M. Cherepashchuk (Astron. Zh., 57, 749, 1980) who discuss the light-curves published by Walker and by M.R. Nelson and E.C. Olson (Astrophys. J., 207, 195, 1976). A companion is listed in I.D.S. System1029Orbit1End System1030Orbit1Begin The magnitude is an estimated V magnitude, based on unpublished photometry on the Copenhagen system, available to Griffin. Although no M-K classification of the spectrum appears to have been made, the star is probably a giant. System1030Orbit1End System1031Orbit1Begin From the relative line intensities, Conti et al. deduce a visual magnitude difference of 0.4m. Note that the fainter secondary star appears to be the more massive. System1031Orbit1End System1032Orbit1Begin No measure of Delta m is available. Star is fainter component of A.D.S. 11061: A is 41 Dra, 5.68m at about 19". A third component is listed in I.D.S. at 221". The light of 40 Dra has been suspected of variability. System1032Orbit1End System1033Orbit1Begin Earlier investigations were published by N. Ichinohe (Astrophys. J., 26, 157, 1907) and by Kohl himself (Astron. Nachr., 219, 213, 1923), based on Ichinohe's observations. Kohl's 1923 results included K=66.82 km/s, V0=8.23 km/s. It is not clear how far these differences are real. Twenty Mount Wilson coude spectrograms measured by L. Lowen (Publ. Astron. Soc. Pacific, 62, 63, 1950) and obtained between 1939 and 1949 agree with Kohl's elements except that Lowen recommends the value of P be changed to 180.55d. The H-alpha line is seen in emission and H-beta emission is also suspected. The intensity of the He I line, lambda 4471 increases during eclipse, that of the Mg II line, lambda 4481 is unaffected. The primary is classified as B8 Iap in Bright Star Catalogue. Evidence that the secondary star is the hotter component of the system is discussed by M. Plavec (Inf. Bull. Var. Stars, No. 1598, 1979) and by M.J. Plavec and J.L. Weiland (Bull. Am. Astron. Soc., 12, 869, 1980). No solution for the photometric elements appears to have been attempted. Star is brightest member of A.D.S. 11169: closest companion is 11.5m at 16.9". System1033Orbit1End System1034Orbit1Begin The Durchmusterung number is from the C.P.D. Thackeray and Hutchings give three sets of elements obtained from permitted emission lines, absorption lines and forbidden emission lines. The set given in the Catalogue is derived from the permitted emission lines. These were adopted as being likely to be less affected by gas streaming than are the elements obtained from the absorption lines. There is some evidence for an M-type secondary spectrum, but it has not been possible to obtain a value of K2. The primary spectrum is of early type, the cF absorption spectrum is believed to arise in a stream travelling from the M-type secondary to the primary. The time of periastron passage is given by Thackeray and Hutchings as 52 days after mid-eclipse according to the ephemeris by M.W. Mayall (Ann. Harv. Coll. Obs., 105, 491, 1937). We have added 40 periods and 52 days to Mayall's time of minimum. More recent UBV photometry by P.J. Andrews (Mon. Not. Roy. Astron. Soc., 167, 635, 1974) leads to the ephemeris: mid-eclipse=J.D. 2,420,321+604.6E. Discussions of the UV spectrum of this system have been published by J.B. Hutchings and A.P. Cowley (Publ. Astron. Soc. Pacific, 94, 107, 1982), J.B. Hutchings et al. (Astrophys. J., 275, 271, 1983) and W. Strupat (Mitt. Astron. Gesells., 62, 275, 1984). They do not help to determine the orbital elements more precisely. System1034Orbit1End System1035Orbit1Begin The new elements supersede the work of A. Colacevich (Oss. e Mem. Arcetri, 59, 33, 1940) and J. Sahade (Astrophys. J., 109, 116, 1949). The spectral type of the secondary is inferred from the few lines that can be recognized in the combined spectrum. The value of K2 is approximate and depends on measures of the K line alone. The epoch appears to be the time of minimum velocity of the hotter star. The small eccentricity is probably not real, since even the helium lines used for measurement may be affected by gas-stream effects. Variable emission has been detected at H-alpha. The best discussion of the light-curve still seems to be that by R.L. Baglow (Mon. Not. Roy. Astron. Soc., 108, 343, 1948) of R.O. Redman's (ibid., 105, 212, 1945) photographic observations. Baglow found an orbital inclination of about 82 deg and a fractional luminosity for the larger star of 0.86. He did not regard these results as well determined. Spectroscopic results have improved to the point where the system should be observed photometrically with modern equipment and the results submitted to full analysis. The period may be variable. Three companions are listed in I.D.S., the closest is 9.7m at 38.9". System1035Orbit1End System1036Orbit1Begin This is the former Nova Her 1963 and is of interest in being the first nova to erupt, after Kraft's classic work on cataclysmic variables, that has been shown to be binary. The period is uncertain -- a value around 0.17d is also possible. The epoch is T0 and the orbit is assumed circular. The magnitude is still variable; that given in the Catalogue is an approximate mean for the year 1978, on a scale close to the B scale. (E.L. Robinson and R.E. Nather, Astrophys. J., 273, 255, 1983). System1036Orbit1End System1037Orbit1Begin The epoch is the time of conjunction (hotter star in front). The orbit is assumed circular. The visual magnitude difference between the two stars was estimated at 0.6m. The minimum masses would be substantially increased by corrections for pair-blending. A 13.0m companion at 8.4" is listed in I.D.S. System1037Orbit1End System1038Orbit1Begin System1038Orbit1End System1039Orbit1Begin Original observations by W.E. Harper (Publ. Dom. Astrophys. Obs., 1, 307, 1921). Luyten's recomputation is preferred because Harper fixed the value of T. Epoch is T0. No measure of Delta m has been made, but Harper described the two spectra as quite similar. He later revised the period to 2.04765d (Publ. Dom. Astrophys. Obs., 6, 239, 1935). Star is brightest member of A.D.S. 11213. The other three faint components form a compact group at about 95". System1039Orbit1End System1040Orbit1Begin The elements given in the Catalogue supersede those of A.P. Cowley, W.A. Hiltner and C. Berry (Astron. Astrophys., 11, 407, 1971) and W.A. Hiltner (Astrophys. J., 102, 492, 1945), although allowance must be made, in comparing these investigations, for the different lines used from the Wolf-Rayet spectrum. The upper line of the Catalogue refers to the W-R component. The epoch is the time of inferior conjunction of the W-R star, and the orbit is assumed circular. Note that the times of conjunction derived from each component differ slightly (43399.7 for the secondary). The star is notorious for having at one time displayed eclipses (R.M. Hjellming and W.A. Hiltner, Astrophys. J., 137, 1080, 1963) which later appeared to have stopped (K. Stepien, Acta Astron., 20, 13, 1970; L.V. Kuhi and F. Schweizer, Astrophys. J., 160, L185, 1970). Although R. Schild and W. Liller (Astrophys. J., 199, 432, 1975)) suggested that the appearance of eclipses was an artifact of the ephemeris used to represent the observations, the matter does not seem to have been settled to the satisfaction of all those who have studied the system. The orbital inclination is therefore uncertain. According to Massey and Niemela, the secondary star's spectrum is certainly of O-type and the minimum mass is close to the expected value for that type -- suggesting an inclination near 90 deg, while the absence of eclipses indicates i<82 deg. The stars are probably of much the same luminosity and the system may belong to the Ser OB2 association. System1040Orbit1End System1041Orbit1Begin This star has come to be the prototype of a sub-class of cataclysmic variables. The magnitudes given represent the approximate range between the system's high and low states. Characteristic of the system, besides the X-ray flux, are the circular polarization (S. Tapia, Astrophys. J., 212, L125, 1977; J. Bailey and D.J. Axon, Mon. Not. Roy. Astron. Soc., 194, 187, 1981) of its visible light and the evidence for strong magnetic fields. The epoch given is the time when the velocity of the emission-line source is equal to V0 and increasing. Earlier discussions of the orbital elements have been published by W.C. Priedhorsky (Astrophys. J., 212, L117, 1977), A.P. Cowley and D. Crampton (ibid., L121 and Publ. Astron. Soc. Pacific, 89, 374, 1977 and J.L. Greenstein et al., Astrophys. J., 218, L121, 1977). The spectrum in the low state is different from that in the high state and the elements given in the Catalogue are derived from means of the Balmer lines measured (H-beta, H-gamma and H-delta) which were relatively narrow at the time of observation. The velocity-curve is therefore relatively well defined for a cataclysmic variable, although its relation to the orbital motion of the white dwarf remains obscure. In the high state, there are also broad emissions that give a different velocity-curve (J.L. Greenstein et al., Astrophys. J., 218, L121, 1977). The spectral type given for the secondary is derived from infrared observations (P. Young and D.P. Schneider, Astrophys. J., 230, 502, 1979), who found K2=68 km/s. J.B. Hutchings, D. Crampton and A.P. Cowley (Astrophys. J., 247, 195, 1981) agree closely with this value, but Young, Schneider and Shechtman find much higher values (close to 200 km/s) from the weak absorption features they measured in the photographic region of the spectrum. A discussion of the spectrum has also been published by A.N. Burenkov and N.F. Voikhanskaya (Astron. Zh., 57, 65, 1980). The IUE spectrum is briefly described by J.C. Raymond et al. (I.A.U. Symp. No. 88, p. 467, 1980). J. Patterson and C. Price have published results of spectrophotometry during the 1980 low state (Publ. Astron. Soc. Pacific, 93, 71, 1981). L. Crosa et al. (Astrophys. J., 247, 984, 1981) made a detailed simultaneous study of the system in the high state. System1041Orbit1End System1042Orbit1Begin An 8.6m companion at 3.3" is listed in I.D.S. System1042Orbit1End System1043Orbit1Begin The new observations and results supersede the earlier work of W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 198, 1925 and 6, 240, 1935). Closely similar elements have been computed from the observations made by Scarfe et al. by A. Abad and A. Elipe (Astrophys. J., 302, 764, 1986). System1043Orbit1End System1044Orbit1Begin These results supplement Sahade's own earlier work (Astrophys. J., 102, 470, 1945). Different values for omega, e, K1 and V0 are obtained from the two investigations. The earlier elements were based on measures of the K line and Mg II (lambda 4481) only. Modern photoelectric observations (G.F.G. Knipe, Mon. Not. Roy. Astron. Soc., 167, 369, 1974 and N. Kappelmann and K. Walter Astron. Astrophys. Supp., 38, 161, 1979) leave no doubt that the true orbit is circular. Lucy & Sweeney also adopted a circular orbit for their new spectroscopic solution. The spectral type is computed from the photometric solution (B. Cester et al., Astron. Astrophys. Supp., 36, 273, 1979, recomputed a solution from Knipe's light-curves and G. Russo and C. Sollazzo, Inf. Bull. Var. Stars, No. 1827, 1980, recomputed one from those obtained by Kappelmann and Walter) but the G-type spectrum can be seen during totality and J. Smak (Acta Astron., 15, 327, 1965) deduced K2=160 km/s, from measures of the D lines, yielding masses of 1.8 MSol and 0.26 MSol. All investigators agree on an orbital inclination close to 88 deg and a fractional luminosity for the hotter star (in V) in the neighbourhood of 0.8. System1044Orbit1End System1045Orbit1Begin New observations by Abt and Levy yield elements that agree very well with those of Z. Daniel and L.F. Jenkins (Publ. Allegheny Obs., 3, 147, 1914). The agreement is the chief reason for giving these elements a b category. Nevertheless, there is a very considerable difference in the two values of K2 (Daniel and Jenkins found K2=101.7 km/s). The value obtained by Abt and Levy from more modern material is preferred. The epoch is T0; formal solution for the orbital elements gave e=0.001, which is negligibly small. Abt and Levy give the spectral types as A2.5, A8 and F2 from the K line, hydrogen lines and metallic lines respectively. Petrie(II) found Delta m=0.78. System1045Orbit1End System1046Orbit1Begin The observations on which this orbit is based were obtained at the Lick Observatory from 1899-1951. Despite the long period the velocity-curve seems well determined except for some disturbing residuals near the ascending node. Reference: J.Grobben & R.P.Michaelis, Ric. Astr. Spec. Vatic., 8, 33, 1969 System1046Orbit1End System1047Orbit1Begin The epoch is T0. Lucy & Sweeney confirm that the orbit should be regarded as circular. There is evidence of blending effects of the secondary spectrum, especially in the lines of He I. The more luminous star is in front at the deeper minimum, so the secondary star must have the earlier spectral type. S. Gaposchkin (Ann. Harv. Coll. Obs., 113, 139, 1953) estimated from the light-curve Delta m=2.3. System1047Orbit1End System1048Orbit1Begin Another determination of K1 (70 km/s) was published almost simultaneously by K.O. Mason et al. (Mon. Not. Roy. Astron. Soc., 200, 793, 1982). Cowley, Crampton and Hutchings give a more complete set of orbital elements, so their values have been preferred. The value of K1 is determined from measures of the base of the emission line He II lambda 4686; that of K2 is determined from measures of H-delta absorption -- which appears to be associated with the secondary component. Mason et al. were unable to measure the H-delta line on their spectrograms. The epoch is the time of optical minimum and the orbit is assumed circular. There is some uncertainty whether or not optical and X-ray minima are coincident. Studies of the X-ray and optical variation have been published by P. Charles, J.R. Thorstensen and P. Barr (Astrophys. J., 241, 1148, 1980), K.O. Mason et al. (ibid., 242, L109, 1980) and N.E. White et al. (ibid., 247, 994, 1981). Results of spectrophotometry and a model are given by K.O. Mason and F.A. Cordova (Astrophys. J., 255, 603, 1982). System1048Orbit1End System1049Orbit1Begin Earlier spectroscopic observations by D.M. Popper (Astrophys. J., 97, 394, 1943) were insufficient for the derivation of orbital elements. A new spectroscopic study has been published by M.Yu. Skul'skii (Bulletin Abastumani Obs., No. 58, 101, 1985 -- see also the spectrophotometric study by M.B. Babayev, ibid., 105). Skul'skii has more observations than were available to Cowley and Hutchings, but his measures show a large scatter. Although he does not give orbital elements, his diagram shows that he agrees with Cowley and Hutchings on the value of K1 (for the brighter but less massive star) but finds a very much smaller value of K2. Beyond the facts that this is a very massive system and a radio source (V.A. Hughes and A. Woodsworth, I.A.U. Circ., No. 2488, 1973, R.M. Hjellming et al., Nature Phys. Sci., 242, 84, 1973) we still know rather little about it. The ultraviolet spectrum has been briefly described by R.H. Koch (Inf. Bull. Var. Stars, No. 1580, 1979). The epoch is the time of primary minimum as used by Cowley and Hutchings (the orbit is assumed circular). A modern ephemeris would be best derived from the UBV observations published by F. Ciatti et al. (Astron. Astrophys. Supp., 41, 143, 1980) and analyzed by L. Milano et al. (Astron. Astrophys., 100, 59, 1981) and G. Giuricin and F. Mardirossian (ibid., 101, 138, 1981). The orbital inclination is around 75 deg and the fractional luminosity of the hotter component (in V) is 0.56. System1049Orbit1End System1050Orbit1Begin The star has long been known for its composite spectrum. Griffin and Griffin succeeded in disentangling both spectra and determined the orbit of each component thus showing the system to be of the zeta Aur type. Indeed, subsequent work (R.E.M. Griffin, J. Roy. Astron. Soc. Can., 82, 49, 1988) has shown that the system undergoes eclipses, although no photometric observations are yet available and no variable-star designation has yet been given. The spectral types given are those derived by Griffin and Griffin. They are at pains to emphasize, however, the uncertainty that attaches to any attempt to separate the components of a composite spectrum. Their classification is confirmed by the observations of the late-type spectrum during eclipse. The orbit of the late-type component depends primarily on photoelectric measures of its radial velocity. The semi-amplitude of the secondary is determined from a relatively small number of high-dispersion spectrograms from which the late-type component has been subtracted. System1050Orbit1End System1051Orbit1Begin The minimum magnitude is estimated from fragmentary unpublished photometric observations of the primary eclipse. The spectra are similar although the depths of eclipses suggest a surface-brightness ratio of 0.76 -- rather larger than would be expected from the mass-ratio. Popper emphasizes the need for a complete light-curve. The orbit is assumed circular and the epoch is the time of primary minimum. System1051Orbit1End System1052Orbit1Begin The work of Hansen and McNamara completely supersedes the orbital elements derived earlier by F.J. Neubauer and O. Struve (Astrophys. J., 101, 240, 1945) but still leaves many problems unsolved. The stellar spectrum is distorted by the spectrum of gas streams and emission is visible at H-alpha (D.H. McNamara, Publ. Astron. Soc. Pacific, 69, 574, 1957). Hansen and McNamara tried to correct for these effects when deriving the orbital elements. The epoch is the time of primary minimum and the orbit is assumed to be circular in accordance with the light-curve. According to V.G. Karetnikov (Astron. Zh., 44, 22, 1967) the spectral type of the primary component varies. The type of the secondary is derived from the UBV light-curves obtained by S.K. Wilcken, D.H. McNamara and H.K. Hansen (Publ. Astron. Soc. Pacific, 88, 262, 1976). These authors find the light-curves difficult to solve but derive an orbital inclination of 84 deg and a fractional luminosity (in V) for the primary component of 0.89. Relatively small changes in the quantities derived from both the spectroscopic and photometric data could bring the masses and luminosities into accord with expectations based on the mass-luminosity relation. Photometric data were also published by M. Kitamura and K. Sato (Publ. Astron. Soc. Japan, 19, 575, 1967). A new model of the system as a double-contact binary has recently been proposed by R.E. Wilson, W. van Hamme and L.E. Pettera (Astrophys. J., 289, 748, 1985). System1052Orbit1End System1053Orbit1Begin The epoch is T0. Photoelectric light-curves published by Zha Disheng and Huang Yinliang (Astron. Sinica, 21, 158, 1980) confirm that the orbit is circular. A solution of these light-curves by K.-C. Leung, Zha Disheng and Huang Yinliang (Acta Astrophys. Sinica, 2, 144, 1982) gives an orbital inclination close to 79 deg and a fractional luminosity (in yellow light) for the primary component of 0.91. Struve reported a visual companion, but it is not listed in I.D.S. System1053Orbit1End System1054Orbit1Begin System1054Orbit1End System1055Orbit1Begin This is a complicated system, the spectroscopically triple star being the brighter component of A.D.S. 11353. The fainter component, 7.7m at 3.8", is probably physically related and may also be a spectroscopic binary. The spectrum of the brighter star in the visual pair is composite, and R. Tremblot (Comptes Rendues, 207, 491, 1938) and D.B. McLaughlin (Astrophys. J., 88, 356, 1938) independently discovered the duplicity of the A-type component. The short-period orbit is that of the two A-type stars. The epoch is T0, deduced from Tilley's published list of phases. The value of V0, of course, varies. The magnitude given is a photoelectric (V) magnitude, but it refers to the combined light of the visual pair. There is some evidence of a variation of about 0.3m in the light. The velocity-curve in the long-period orbit is poorly defined near its maximum. The value of K2 (for the centre of mass of the two A-type stars) has been estimated from the corrections needed to bring into agreement the values obtained in successive years for the systemic velocity of the short-period pair. The epoch given is T, estimated from Tilley's published list of phases. An additional visual component at 0.1" from A, observed once according to I.D.S., could conceivably be one of the components in the long-period system. System1055Orbit1End System1056Orbit1Begin This is a complicated system, the spectroscopically triple star being the brighter component of A.D.S. 11353. The fainter component, 7.7m at 3.8", is probably physically related and may also be a spectroscopic binary. The spectrum of the brighter star in the visual pair is composite, and R. Tremblot (Comptes Rendues, 207, 491, 1938) and D.B. McLaughlin (Astrophys. J., 88, 356, 1938) independently discovered the duplicity of the A-type component. The short-period orbit is that of the two A-type stars. The epoch is T0, deduced from Tilley's published list of phases. The value of V0, of course, varies. The magnitude given is a photoelectric (V) magnitude, but it refers to the combined light of the visual pair. There is some evidence of a variation of about 0.3m in the light. The velocity-curve in the long-period orbit is poorly defined near its maximum. The value of K2 (for the centre of mass of the two A-type stars) has been estimated from the corrections needed to bring into agreement the values obtained in successive years for the systemic velocity of the short-period pair. The epoch given is T, estimated from Tilley's published list of phases. An additional visual component at 0.1" from A, observed once according to I.D.S., could conceivably be one of the components in the long-period system. System1056Orbit1End System1057Orbit1Begin The spectrum shows enhanced lines of Si. The velocity variation is beyond doubt, but the period is uncertain. W.R. Beardsley et al. (Publ. Allegheny Obs., 8, No. 7, 1969) find the old Allegheny observations fit a period of 127.85d, although they discuss the possibility of a shorter one. They find K1=30 km/s. Abt and Snowden could not fit older observations with their period. The elements are therefore very provisional. The star is the brighter member of A.D.S. 11311 which is apparently a physical pair near periastron (separation less than 1"). System1057Orbit1End System1058Orbit1Begin These observations and orbital elements supersede those determined by W.H. Wright (Astrophys. J., 11, 131, 1900), by R.T. Crawford (Lick Obs. Bull., 13, 176, 1928), and even the excellent orbital elements derived by J.M. Vinter-Hansen (Lick Obs. Bull., 19, 141, 1942). Other investigations that confirmed Vinter-Hansen's were published by M. Spite (Ann. Astrophys., 30, 211, 1967) and H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 276, 1973). The principle improvements made by the new observations are a complete determination of the secondary velocity-curve obtained by observing in the red and near infrared, and the use of speckle-interferometric observations to give a good determination of the astrometric orbit. Previously only Spite had succeeded in observing the secondary spectrum -- and then only a few times. Observations of the secondary have been used to determine only K2 and V0 (which differs insignificantly from the value obtained from observations of the primary). Similarly, the spectroscopic values of P, T and e were adopted in the analysis of the astrometric orbit. This orbit, like its spectroscopic counterpart, supersedes earlier work (H.L. Alden, Astron. J., 45, 113, 1936; L.A. Breakiron and G. Gatewood, Publ. Astron. Soc. Pacific, 86, 448, 1974) and confirms the conclusion by W.J. Luyten (Publ. Minnesota Obs., 2, 15, 1934) that there is no third body in the system. The orbital inclination is 75 deg, the major semi-axis is 0.122" and the parallax is 0.120". The stars have masses of 1.03 MSol and 0.75 MSol and their luminosities are consistent with their being slightly metal-poor and 8E9 years old. Two faint companions are listed in I.D.S. at about 150". System1058Orbit1End System1059Orbit1Begin Hube found no convincing evidence for changes in the orbital elements in the past 51 years, although the most recent velocities fall systematically below the velocity curve. This no doubt contributes to the rather large scatter of individual observations. Hube interprets sharp absorption features sometimes found in the violet wings of the hydrogen and helium lines as evidence for mass loss. The features cannot be identified with the secondary spectrum. System1059Orbit1End System1060Orbit1Begin System1060Orbit1End System1061Orbit1Begin Popper did not measure the hydrogen lines, the two components of which blend with each other. This probably accounts for the fact that he found higher values for the semi-amplitudes than did J.F. Heard and D.C. Morton (Publ. David Dunlap Obs., 2, 255, 1962). A circular orbit is assumed and the epoch is the time of primary minimum. A more up-to-date ephemeris is given by J.V. Clausen, A. Gimenez and C.D. Scarfe (Astron. Astrophys., 167, 287, 1986) who analyze light- curves by A. Colacevich (Contr. Capodimonte Oss., Ser. II, 4, No. 12, 1953) and J.V. Clausen et al. (Astron. Astrophys. Supp., 68, 141, 1987). They show that there is a small but real eccentricity of 0.013 and apsidal motion in a period of about 180 years. They find an orbital inclination of about 86 deg and give a visual magnitude difference of 0.77 -- rather larger than expected from the appearance of the secondary spectrum. System1061Orbit1End System1062Orbit1Begin System1062Orbit1End System1063Orbit1Begin System1063Orbit1End System1064Orbit1Begin The chief interest of this system is its high velocity and probable metal deficiency. System1064Orbit1End System1065Orbit1Begin The epoch is T0 and a circular orbit is assumed -- in accordance with modern light-curves. Individual spectral types are assigned by Popper on the basis of B-V colours: the observed spectral type is A0. Earlier investigations by H. Shapley (Astrophys. J., 40, 399, 1914) and by R.H. Baker and E.E. Cummings (Laws Obs. Bull., 2, 151, 1916) were based on three spectrograms and can be ignored. R.F. Sanford (Astrophys. J., 68, 51, 1928) found lower values of K1 and K2 than Popper did -- probably because Sanford used a lower dispersion. Photometric investigations have been published by F.B. Wood (Astrophys. J., 110, 465, 1948), N.I. Magalashvili (Bulletin Abastumani Obs., No. 15, 1, 1953) and K.W. Jeffreys (Astron. Astrophys. Supp., 42, 285, 1980). The first-named was re-analyzed by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978). Jeffreys found an orbital inclination of 85 deg and a fractional luminosity (in V) for the brighter star of 0.62. System1065Orbit1End System1066Orbit1Begin System1066Orbit1End System1067Orbit1Begin This star is extremely metal-deficient and is described by Jasniewicz and Mayor as `apparently the most metal-deficient star of the halo with known orbital elements'. This may account for divergent classifications ranging from sdF5 to sdK1. The low metal abundance has made the spectrum harder to measure with CORAVEL than is usual for spectra of the same general type. These elements are in large measure confirmed by D.W. Latham et al. (Astron. J., 96, 567, 1988). System1067Orbit1End System1068Orbit1Begin Petrie did not measure Delta m for this pair, but he stated `the two spectra are much alike, it being sometimes difficult to differentiate between them'. Curchod and Hauck list the star, but give only the K-line spectral type of A8. A 10.5m companion at 26.6" is listed in I.D.S. System1068Orbit1End System1069Orbit1Begin The new observations by Vogt and Fekel, combined with the earlier ones by B.W. Bopp and D.S. Evans (Mon. Not. Roy. Astron. Soc., 164, 343, 1973) have led to an improvement in our knowledge of this system, whose duplicity was discovered by W. Krzeminski and R.P. Kraft (Astron. J., 72, 307, 1967). The intrinsic variations in the light of the star, usually ascribed to both spots and flares, make it difficult to obtain orbital elements of very high quality. Vogt and Fekel derive a luminosity ratio at lambda 6500 of 1.93. A detailed photometric study of the system was published by V. Oskanyan et al. (Astrophys. J., 214, 430, 1977). S.S. Vogt (ibid., 240, 567, 1980) has shown that, contrary to previous results, complex line profiles in this and similar systems are not the result of Zeeman splitting and there is no evidence for large magnetic fields. The emission lines of Ca II were shown not to vary with the 3.8d rotation period of the primary star (B.W. Bopp and G. Ferland, Publ. Astron. Soc. Pacific, 89, 69, 1977). The spectra of the components have also been discussed by P.C. Keenan (ibid., 92, 548, 1980). System1069Orbit1End System1070Orbit1Begin Petrie found Delta m=0.18. He estimated i=29 deg from the mass-luminosity relation, using the cluster parallax of the Ursa Major cluster, to which the system belongs. System1070Orbit1End System1071Orbit1Begin The reality of the velocity variation of this alleged long-period, low-amplitude binary should be checked. It has not been confirmed by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976) nor are radial velocities measured by A.H. Batten consistent with the elements presented here. The spectrum shows the Hg:Mn peculiarity. The star is the brighter component of A.D.S. 11504: companion is 10.7m at 7.3". System1071Orbit1End System1072Orbit1Begin Griffin quotes spectral types of both K0 III and K1 III. System1072Orbit1End System1073Orbit1Begin The period is 33,527.6d or 91.8y. The system is a visual binary, discovered by F.G.W. Struve when the separation was close to its maximum value of about 0.4". The spectroscopic observations cover only the eighteen months or so around nodal passage when the two spectra are resolved. Consequently, V0 is not as well determined as is desirable and, while K1+K2 is accurately known, the individual values K1 and K2 are subject to uncertainty. On the other hand, the visual observations lead to a good knowledge of P, T, e and omega. The spectral type given is the mean of the two components. It is difficult to separate the two spectra but they could be as different as G8 III-IV and F8 IV, the brighter being of later type. The difference in V between the two components is similarly uncertain but around 0.8m. There is a third component at a distance of just over 14" from the close pair and nearly 2m fainter. It has a radial velocity close to the systemic velocity of the close pair, and changes in the position angle suggest a slow orbital motion. It seems likely that all three stars are of about solar mass and well evolved. System1073Orbit1End System1074Orbit1Begin The orbital elements are derived from the absorption lines of He I, Si III, N II, Si IV, and O II. Other lines give very different velocity amplitudes and Hutchings and Redman themselves are very cautious about supposing that they have derived the true orbital elements. Undoubtedly some sort of extended envelope surrounds the star. The failure to detect the secondary spectrum is also considered surprising by the investigators. System1074Orbit1End System1075Orbit1Begin Possible traces of the secondary spectrum were observed, but no reliable value of K2 could be determined. System1075Orbit1End System1076Orbit1Begin There is no M-K classification of the spectrum and the type given is from the H.D. Catalogue. Primarily because of the star's colour, Griffin estimates that the type should be M. I.D.S. lists a 10.4m companion at 60.2" separation. Griffin has measured its radial velocity and found the star not to be physically related to the spectroscopic pair. System1076Orbit1End System1077Orbit1Begin The values found for K1 and K2 by Aikman are lower than those found by R.M. Petrie (Publ. Dom. Astrophys. Obs., 6, 285, 1935), but since Aikman's are derived from spectrograms of higher dispersion they are probably the more reliable. The values of e, omega and V0 obtained in the two investigations agree reasonably well. Petrie(I) found Delta m=0.29. He estimated i=23 deg. System1077Orbit1End System1078Orbit1Begin These new observations and the results derived from them supersede the earlier work of B.W. Baldwin (Astrophys. J., 226, 937, 1978) and W.A. Hiltner (ibid., 104, 396, 1946). Baldwin's work and the critique of it by J. Smak (Acta Astron., 31, 25, 1981) also stimulated interest in the making of photometric observations (J. van Paradijs et al., Astron. Astrophys., 111, 372, 1982; E.C. Olson and J.P. Hickey, Astrophys. J., 264, 251, 1983; D. Forbes and C.D. Scarfe, Publ. Astron. Soc. Pacific, 96, 737, 1984). Precise spectral classification of the two late-type components is difficult. The orbital elements, hard to obtain by conventional spectroscopy, have been found from photoelectric velocity measurements. The orbit was assumed circular after a preliminary solution showed the eccentricity to be much smaller than its own uncertainty: the epoch is T0 for the K-type star. Photometric and spectroscopic (emission-line) observations provide evidence of a disk surrounding the hotter star, yet both stars appear to be well within their Roche lobes. The orbital inclination is probably close to 90 deg. The larger star gives nearly 0.6 of the light in V. Interpretation of the system is still controversial. System1078Orbit1End System1079Orbit1Begin Previous studies of the system have been published by F.C. Jordan (Publ. Allegheny Obs., 1, 115, 1909), W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 240, 1935) and H.A. Abt (Astrophys. J. Supp., 6, 37, 1961). Jordan's results are in good agreement with the latest investigation and the other two led only to minor revisions. It is the constancy of the derived elements over a long period of time, rather than the quality of the individual investigations, that leads to the a classification. The spectral type is given by Abt and Levy as A6, A8 and F1 from the K line, hydrogen lines and metallic lines respectively. The epoch is T0. The eccentricity is smaller than its uncertainty and probably should be ignored -- no value is given for omega. The star is the brightest member of A.D.S. 11639; the principal companion (zeta 2 Lyr) is 5.74m at 43.7". System1079Orbit1End System1080Orbit1Begin The epoch is T0 and the eccentricity is smaller than its uncertainty. No value for omega is given and the orbit should be regarded as circular. The spectral types are A2, A3 and A6 from the K line, hydrogen lines and metallic lines respectively. The star is the brightest member of A.D.S. 11667: companions 7.9m at 13.0" and 11.3m at about 26" (probably optical). System1080Orbit1End System1081Orbit1Begin New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. System1081Orbit1End System1082Orbit1Begin Epoch is T0, since the light-curve and velocity-curve agree in showing the orbit to be very nearly circular. The A-type component appears to depart appreciably from the mass-luminosity relation and Popper finds that it is the brighter star. Its velocity-curve is relatively well defined; that of the B-type star is less so. Popper also obtained photometric observations and, assuming an orbital inclination of 90 deg, found Delta m=0.8. B. Cester et al. (Astron. Astrophys., 61, 469, 1977) find, from the same observations, that the inclination is about 85 deg and the hotter component gives 0.65 of the light in V (they disagree with Popper about which star is brighter). G.L. Clements and J.S. Neff (Astrophys. J. Supp., 41, 1, 1979) draw attention to an ultraviolet excess in the light of the system. System1082Orbit1End System1083Orbit1Begin The elements obtained by Lucy & Sweeney are very similar to those obtained by J. Sahade himself from the same observations (Astrophys. J., 102, 470, 1945). The new elements, computed by Sterne's method and showing the eccentricity to be negligible, are preferred to the old ones computed by the Wilsing-Russell method. The epoch is T0. The period is increasing. The scatter about the velocity-curve is large, but the coverage is good. The V magnitudes given in the Catalogue are estimated from the data published by C. Blanco and S. Cristaldi (Publ. Astron. Soc. Pacific, 86, 187, 1974) in their discussion of the light-curve. They find that the light-curve varies, but estimate the secondary spectrum to be G0 and find the system can be represented as a typical Algol system. Earlier, Z. Kopal (Close Binary Systems, p. 497, 1959) had assigned this system to the class of those containing undersize subgiants. I.W. Roxburgh (Astron. J., 71, 133, 1986) further suggested that the secondary was still contracting to the main sequence. Light-curves (in UBV) obtained by T. Hayasaka (Publ. Astron. Soc. Japan, 31, 271, 1979) lead to a value for the radius of the secondary component that is smaller than the Roche lobe, although other observations by C. Cristescu, G. Oprescu and M.D. Suran (Inf. Bull. Var. Stars, No. 1916, 1981) give again a larger radius. Perhaps the chief need is for a modern velocity-curve. Hayasaka found an orbital inclination of 84 deg and a fractional luminosity for the brighter component (in V) of 0.93. His results were closely confirmed by a re-analysis of his results by G. Giuricin and F. Mardirossian (Astron. Astrophys. Supp., 45, 85, 1981). System1083Orbit1End System1084Orbit1Begin The observations were made with an objective prism, and the value of V0 is arbitrarily set at zero. The scatter of observations is large and omega is poorly defined (Gieseking gives omega=80 deg 90 deg). The epoch is denoted by T0, but it is unclear whether or not this symbol is used in the sense defined in Sterne's method. System1084Orbit1End System1085Orbit1Begin The epoch is the time of primary minimum and the orbit is assumed circular, in accordance with the light-curve. The spectral type (taken from the fourth edition of the G.C.V.S.) appears to refer to the primary component. BVRI light-curves were published by D.A.H. Buckley (Inf. Bull. Var. Stars, No. 1867, 1980) and analyzed by him (Astrophys. Space Sci., 99, 191, 1984). He found an orbital inclination of 87 deg and a fractional luminosity for the brighter star (in V) of 0.87. He gave effective temperatures of 7,000 K and 4,749 K for the two components. System1085Orbit1End System1086Orbit1Begin The epoch is an arbitrary zero of phase: T0 is about 0.08d later. No trace of the secondary spectrum has been reported. The star is Nova Aql 1918 and its light is still variable. The V magnitude given in the Catalogue is from A.U. Landolt (Publ. Astron. Soc. Pacific, 80, 481, 1968). Photometry in the far UV has been reported by J.S. Gallagher and A.V. Holm (Astrophys. J., 189, L123, 1974). More recently, light variations that can be interpreted as eclipses have been reported by J. Rahe et al. (Astron. Astrophys., 88, L9, 1980) and M.H. Slovak (I.A.U. Circ., No. 3493, 1980). The interpretation of these variations has been questioned by M.C. Cook (Mon. Not. Roy. Astron. Soc., 195, 51P, 1981). W. Wargau, H. Drechsel and J. Rahe (Acta Astron., 33, 149, 1983) have published measurements of the far ultraviolet continuum flux. System1086Orbit1End System1087Orbit1Begin The H.D. spectral type is K0: Radford and Griffin suggest that the type lies in the range K5 to M0 III. The type given in the Bright Star Catalogue is K2 Ib, which apparently is taken from T.E. Lutz and J.H. Lutz (Astron. J., 82, 431, 1977). See the Note added by Radford and Griffin to their paper for a discussion of this. The star is the brightest member of A.D.S. 11719: its two companions are 12.3m at 23" and 8.7m at 114". Radford and Griffin have shown that the radial-velocity of the latter is very different from the systemic velocity of the spectroscopic binary. System1087Orbit1End System1088Orbit1Begin Original observations were made by R.F. Sanford (Astrophys. J., 53, 201, 1921), but Tanner was able to show that Sanford's value of the period was incorrect. Some doubt still remains about the period because of the great similarity between the spectra of the two components. Only 105 cycles are covered by the observations, so the determination of the period is necessarily imprecise. The orbit was assumed circular and the epoch is T0. It is the F5 component of the composite spectrum that is double (F2 according to Sanford). The A-spectrum presumably arises from the visual secondary at less than 1", and often unresolved. These stars probably form a real triple system. Together with a faint, distant, and probably optical companion they form the system A.D.S. 11698. System1088Orbit1End System1089Orbit1Begin The ascending branch of the velocity-curve is poorly defined. System1089Orbit1End System1090Orbit1Begin Variability of the velocity of this star was pointed out by R.E. Wilson and A.H. Joy (Astrophys. J., 111, 221, 1950), but no attempt was made to determine orbital elements until the accidental observation of the star in eclipse (the light-curve is not completely observed and the minimum magnitude is unknown). The present elements, being based on only five observations should be viewed with reserve, but they are consistent with the only two observed eclipses. The epoch is the approximate time of primary minimum. Turner and Perderos discuss the possibility that this system is a companion to the Cepheid BB Sgr. System1090Orbit1End System1091Orbit1Begin Photoelectric (B and V) observations were published by D. Korsch and K. Walter (Astron. Nachr., 291, 231, 1968) from which the magnitudes given in the Catalogue were taken. Korsch and Walter find evidence for gas streams in the system, but this is not fully corroborated by the spectroscopic observations. The orbital eccentricity found spectroscopically appears to be genuine, and the difference found between the time of mid-eclipse and of spectroscopic conjunction is not statistically significant. F. Mardirossian et al. (Astron. Astrophys. Supp., 39, 235, 1980) re-analyzed the photometric observations by Korsch and Walter and obtained results in general agreement with theirs. In particular, the orbital inclination is 84 deg and the fractional luminosity of the hotter star (in V) is 0.56. The secondary may not completely fill its Roche lobe. The eclipsing system belongs to A.D.S. 11729 of which, except during primary eclipse, it is the brighter member. The companion, at 4.7", must be brighter than the 10.8m given for it in I.D.S. and is bright enough to affect both the photometric and spectroscopic observations. System1091Orbit1End System1092Orbit1Begin It is impossible in a short note even to attempt to give a comprehensive list of just the spectroscopic investigations of one of the most-studied binary systems in the sky. Readers are therefore referred to the review by J. Sahade (Space Science Rev., 26, 349, 1980) for a discussion of work to that date, including the extensive studies of the far UV spectrum. The orbit of the primary star is well determined from the metallic lines and there is little to choose between the elements given in the Catalogue and those derived by J. Sahade et al. (Trans. Amer. Phil. Soc. NS, 49, 1, 1959). The chief difference between them, about 2 km/s in the value of V0, probably reflects only a systematic difference between observatories. Since the period is known to be increasing by about 18 s/yr, the period and epoch (T0) are approximate for 1974 and should not be used for phase predictions. Although various claims to have observed and measured the secondary spectrum have been made, none has won general acceptance. The star is the brightest component of A.D.S. 11745: according to H.A. Abt and S.G. Levy (Astron. J., 81, 659, 1976), components B and E may be physically associated with beta Lyr, although all components are separated by more than 40" from the principal star. (The orbit of beta Lyr B, that was included in the Seventh Catalogue is withdrawn by Abt and Levy.) J.J. Dobias and M.J. Plavec (Astron. J., 90, 773, 1985) use this physical association to derive an estimated absolute visual magnitude for the system of 4.7 and they suggest a spectral classification for the primary of B8.5 or B9 II-Ib. R.E. Wilson and E. Lapasset (Astron. Astrophys., 95, 328, 1981) have explored further the agreement of the photometric observations with the disk model and suggest that the `disk' is a torus. M. Hack et al. (Astron. Astrophys., 126, 115, 1983) have published details of the BUSS spectrogram of this star. Discussions of anomalous CNO abundances have been published by V.V. Leushin and L.I. Snezhko (Pis. Astron. Zh., 6, 171, 1980) and S. Balachandran et al. (Mon. Not. Roy. Astron. Soc., 219, 479, 1986) Known variations in the emission lines are discussed by V.I. Burnashev and M.Y. Skul'skii (ibid., 6, 587, 1980) and by Skul'skii alone (ibid., 6, 628, 1980). System1092Orbit1End System1093Orbit1Begin The epoch is T0. Lucy & Sweeney also adopted a small orbital eccentricity. The luminosity class III is perhaps questionable in view of the short period. Sahade and Cesco classified the primary spectrum as between B5 and B8. D.S. Hall and G.S. Hubbard (Publ. Astron. Soc. Pacific, 83, 459, 1971) have published UBV light-curves of this system and estimate a spectral type of A4 for the secondary star. They find i=88.7 deg and the fractional luminosity of the primary star to be 0.92 in V. G. Giuricin and F. Mardirossian (Astrophys. Space Sci., 76, 111, 1981) find similar results from the same observations. The secondary eclipse is asymmetric, especially in U. The rapid apsidal motion suggested by Hall and Hubbard has not been confirmed (C.D. Scarfe and D.J. Barlow, Publ. Astron. Soc. Pacific, 86, 181, 1974). System1093Orbit1End System1094Orbit1Begin These elements are an amendment of those given by the same author in Lick Obs. Bull., 12, 165, 1926. Luyten has recomputed the elements, as have Lucy & Sweeney. All agree in adopting the eccentric orbit. The primary spectrum is Ap, showing enhancement of manganese and mercury lines. The secondary spectrum is estimated partly from the line strengths and partly from the colour. C.E. Seligman (Publ. Astron. Soc. Pacific, 82, 128, 1970) has detected the secondary spectrum and deduces a mass-ratio of 2.06+/-0.17. New velocities have also been measured by P.S. Conti (Astrophys. J., 160, 1077, 1970); they agree well with Meyer's orbital elements, although a slight increase in period is indicated by both these and Seligman's results. T.S. Galkina (Bulletin Abastumani Obs., No. 58, 265, 1985) has published results from spectrograms obtained at 36A/mm dispersion. She finds different values for the elements from the ionized magnesium line (lambda 4482) and the Balmer lines. She also finds variations with phase in equivalent widths and primary spectral type. These findings suggest that the system is more complicated than it has appeared to be heretofore. System1094Orbit1End System1095Orbit1Begin This star was identified with the X-ray source 4U 1839 31 by J.E. Steiner et al. (I.A.U. Circ., No. 3529, 1980), who also derived the period and approximate magnitude. The orbit is assumed circular and the epoch is the time of superior conjunction of the emission-line source. The value of K1 is given by Penning as lying between 50 km/s and 75 km/s. He gives no value for V0. He estimates the orbital inclination to lie between 15 deg and 27 deg. System1095Orbit1End System1096Orbit1Begin Popper's new observations and analysis supersede both A. McKellar's original work (Publ. Dom. Astrophys. Obs., 8, 235, 1949) and the re-discussion of it by R.M. Petrie, D.H. Andrews and C.D. Scarfe (I.A.U. Symp. No. 30, p. 221, 1967), and also the brief discussion by O. Struve et al. (Astrophys. J., 111, 658, 1950). Popper has also analyzed the BV observations made by D. Ya. Martynov and Kh. F. Khaliullin (Astrophys. Space Sci., 71, 147, 1980). He finds an orbital inclination of 89 deg and a fractional luminosity (in V) for the brighter component of 0.59. His values for the effective temperatures are slightly different for the two stars. The system has recently attracted interest because the observed apsidal motion is much less than the expected relativistic motion (which dominates the expected classical motion) -- see E.F. Guinan and F.P. Maloney (Astron. J., 90, 1519, 1985). This has been interpreted as support for J.W. Moffat's new theory of gravitation (Astrophys. J., 287, L77, 1984), although the interpretation is questioned by Kh. F. Khaliullin (Astrophys. J., 299, 668, 1985). System1096Orbit1End System1097Orbit1Begin These results complement and supersede Harper's earlier work (J. Roy. Astron. Soc. Can., 9, 165, 1915). The old results yielded a slightly lower value of K1 (75.77 km/s). The two spectra are described by Harper as being of `nearly, though not quite equal' intensity. Luyten also recomputed the elements. The observations are published in Publ. Dom. Obs., 2, 123, 1915 and 4, 364, 1919. System1097Orbit1End System1098Orbit1Begin Lucy & Sweeney also adopt an eccentric orbit. The star is the brightest component of A.D.S. 11799: B is 7.9m at 34.2" and does not share the proper motion of A, C is 11.5m at 139.4" and receding from A. System1098Orbit1End System1099Orbit1Begin An earlier investigation was published by F.C. Jordan (Publ. Allegheny Obs., 3, 119, 1914). He found K=33.68 km/s, V0=25.85 km/s. Part, at least of the differences between these values and those of Richardson and McKellar seems to be real. The differences are not accounted for. The light of the system has been suspected of variability. There is 9.2m companion at 174.6" listed in I.D.S. System1099Orbit1End System1100Orbit1Begin The original observations were made by R.E. Wilson (Lick Obs. Bull., 7, 106, 1913). Luyten's recomputation is preferred because Wilson derived the orbital elements graphically. The epoch is T0. Lucy & Sweeney have derived very similar elements. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) confirm these elements. It is the G-type spectrum that displays binary motion, the A-type spectrum arises from an unresolved companion. The system is A.D.S. 11820 with visual companions, each of 11.1m, at 35.4" and 37.8". System1100Orbit1End System1101Orbit1Begin New observations, both photometric and spectroscopic, supersede the work of E.A. Vitrichenko (Izv. Krym. Astrofiz. Obs., 40, 82, 1969 and 43, 76, 1971) and V.I. Burnashev and E.A. Vitrichenko (Peremm. Zvezdy, 17, 502, 1971). The system is a difficult one, however, and coverage of the velocity-curve is not good. Bell, Hilditch and Adamson have shown that both spectra are visible. The epoch is the time of primary minimum and the orbit is assumed circular, in accord with the light-curve. The orbital inclination is found to be about 61 deg and the visual magnitude difference between the components is 1.3m. Bell, Hilditch and Adamson also discuss the evolutionary status of the system. System1101Orbit1End System1102Orbit1Begin System1102Orbit1End System1103Orbit1Begin Using Petrie's method, Thackeray and Tatum found Delta m=0.50. The value of K2 is not well defined. System1103Orbit1End System1104Orbit1Begin Imbert's spectroscopic observations led to the conclusion that the photometric period should be doubled. Apparently, no solution of the light-curve has been made. System1104Orbit1End System1105Orbit1Begin Imbert estimates that the invisible secondary has a spectral type between K5 V and M2 V. A solution for an elliptical orbit gives a formal eccentricity of 0.003, which has been ignored. The epoch, therefore, is T0. The value of omega from the solution is 266.7deg +/- 31deg. System1105Orbit1End System1106Orbit1Begin The observations of this single spectrum W UMa system show a greater scatter than is usual, even for these systems. Different elements are obtained from different lines, and all measurements yield appreciable orbital eccentricities although the photometric orbit is clearly circular. The elements given in the Catalogue were derived by Tapia and Whelan from the mean velocities for each plate weighted according to phase in such a way as to try to minimize the effects of gas streams. The eccentricity thus obtained is an upper limit. No value is given for omega and the epoch is the time of primary minimum. Tapia and Whelan discuss several available photometric studies and adopt i=70 deg. They find a total mass of 1.65 MSol and a mass-ratio of 0.1. They discuss at some length the nature of the secondary star. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System1106Orbit1End System1107Orbit1Begin The primary star is a Cepheid variable (P=4.47d) and may also have a magnetic field. New observations by T. Lloyd Evans (Mon. Not. Roy. Astron. Soc., 199, 925, 1982) confirm the orbital period. Star is brighter component of A.D.S. 11884: B is 11.1m at 6.8". System1107Orbit1End System1108Orbit1Begin There are two earlier investigations of this system by P. Bacchus (Ann. Astrophys., 13, 89, 1950) and D.P. Hube (J. Roy. Astron. Soc. Can., 64, 98, 1970). Hube thought there was marginal evidence for changes in some of the orbital elements, but this was not confirmed by Gorza except for the possibility that omega is changing with time. System1108Orbit1End System1109Orbit1Begin Although the star's spectrum was originally a standard in the M-K system for K2 III, it appears to be somewhat earlier in type and to display CN and Ba anomalies. Two faint companions are listed in I.D.S. each separated from the primary by more than 100". System1109Orbit1End System1110Orbit1Begin System1110Orbit1End System1111Orbit1Begin This is another star whose spectrum shows mild barium enhancement. System1111Orbit1End System1112Orbit1Begin The light of this star has been suspected of variability. System1112Orbit1End System1113Orbit1Begin A new orbit has been published by T.M. Rachkovskaja (Izv. Krym. Astrofiz. Obs., 58, 56, 1978) who finds appreciably higher semi-amplitudes (124 km/s and 140 km/s) than did Pearce. The scatter of the new observations of the secondary is very large, however, and we have preferred to retain Pearce's elements, downgrading them in the quality classification. Further spectroscopic observations are desirable; in particular, the small eccentricity probably should be ignored. Photoelectric UBV light-curves were published by N.I. Magalashvili and Ya.I. Kumsishvili (Bulletin Abastumani Obs., No. 34, 3, 1966). Although the eclipses are shallow, the value of 46.7 deg deduced for the orbital inclination seems low. Kumsishvili and Magalashvili find that the primary star gives 0.7 of the total light. (Rachkovskaja estimates Delta V=1.24m). The U light-curve is different from the other two and cannot be represented by the same elements. System1113Orbit1End System1114Orbit1Begin Although they give elements for this Wolf-Rayet binary, Lamontagne, Moffat and Seggewiss describe it only as a `possible' binary. The orbit is assumed circular and the epoch is the time of inferior conjunction of the Wolf-Rayet star. The value of K1 is a mean value derived from measures of all emission lines. The He II line at lambda 4686 gives K1=22 km/s. No value is given for V0. It is suggested that the invisible secondary may be a compact object. System1114Orbit1End System1115Orbit1Begin Although Wing's study remains the only one in which orbital elements have been deduced, important papers have been published by M.W. Feast (Mon. Not. Roy. Astron. Soc., 135, 275, 1967) and A.M. van Genderen et al. (Mon. Not. Roy. Astron. Soc., 167, 283, 1974). Several photometric investigations have appeared in volumes 25, 28, 30 of Mon. Notes Astron. Soc. South Africa: see especially A.J.W. Cousins, (25, 40, 1966). The minimum V magnitude given in the Catalogue is approximate. The high velocity, large distance from the galactic plane, and the supergiant spectrum make the system a particularly interesting `run-away' object, although van Genderen et al. find the distance from the galactic plane may not be as large as at first thought. The origin of the TiO bands seen in eclipse is still not clear. An M-type secondary two magnitudes fainter than the primary (in V) would fit the infrared colours, but the TiO bands might still have their origin in atmospheric effects during the eclipse. Van Genderen et al. give a rough estimate of i=68 deg. System1115Orbit1End System1116Orbit1Begin Although J.S. Plaskett and J.A. Pearce (Publ. Dom. Astrophys. Obs., 5, 1, 1935) recognized this star as a spectroscopic binary, no orbital elements have been determined until now. The orbit was assumed circular after a preliminary solution showed the eccentricity to be very small, and the epoch is T0. The classification of the secondary spectrum depends on equivalent-width measures, which also give the visual magnitude difference as just over 1m. System1116Orbit1End System1117Orbit1Begin Popper's spectrographic observations supersede those by J.F. Heard and D.C. Morton (Publ. David Dunlap Obs., 2, 255, 1962) and, similarly, the new photometric discussion by D.M. Popper and P.B. Etzel (Astron. J., 86, 102, 1981) supersedes the light-curve obtained by A. Fresa (Mem. Soc. Astron. Ital., 23, 231, 1954) and the rediscussion of it by B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978). A circular orbit was assumed, in agreement with the light-curve, and the epoch is the time of primary minimum. The spectral types are given by Popper elsewhere (Ann. Rev. Astron. Astrophys., 18, 115, 1980). The orbital inclination is close to 86 deg and the visual magnitude difference approximately 1m. System1117Orbit1End System1118Orbit1Begin The light-curves (obtained in B and V, also by Yavuz) indicate a circular orbit. The epoch is the time of primary minimum. A correction of about 14 km/s should be made to V0 to take account of line-curvature. The photometric observations have been re-analyzed by G. Giuricin and F. Mardirossian (Astron. Astrophys. Supp., 45, 499, 1981). They find an orbital inclination of about 87 deg and a fractional luminosity (in V) for the primary component of 0.88. They believe both stars to lie on the main-sequence and suggest spectral types of A0 V+F. An 8.9m companion at 10.5" is listed in I.D.S. Yavuz finds its radial velocity to be the same as that of the centre of mass of the close pair. Reference: I.Yavuz, Abh. Hamburger Sternw.,, Bd.8; No. 5, 1968 System1118Orbit1End System1119Orbit1Begin The epoch is T0. The star's light is slightly variable; the system is probably an ellipsoidal variable. System1119Orbit1End System1120Orbit1Begin Epoch is T0. The value of V0 seems to disqualify the star as a member of the Sco-Cen association. The two spectra are described by Thackeray and Hutchings as `of very similar type and intensity'. Note that the component with the slightly stronger spectrum is also of slightly later type. System1120Orbit1End System1121Orbit1Begin The elements of this system have been recomputed by Luyten and by Lucy & Sweeney. In both recomputations a circular orbit was adopted. Luyten suggested that the true period might be in the neighbourhood of 0.97d, but this possibility does not appear to have been investigated. System1121Orbit1End System1122Orbit1Begin The new results supersede those published by V. Albitzky (Pulkovo Obs. Circ., No. 7, 1933). The small orbital eccentricity appears to be genuine. There is a possibility that the period has decreased since the star was first recognized as a binary. A 10.5m companion at about 22" is listed in I.D.S. System1122Orbit1End System1123Orbit1Begin It has been difficult to decide whether or not to include this orbit. Elements based on a period of 49.09d were published by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976) and were criticized recently by C.L. Morbey and R.F. Griffin (Astrophys. J., 317, 353, 1987). Independently, however, Dworetsky had suggested the period given in the Catalogue and derived alternative elements, which we have accepted with caution. The epoch is T0 . The star is the brightest member of A.D.S. 12061. Of the several components, according to Abt and Levy, only B -- 13.7m at 3.2" -- shares the proper motion of A. SB9 correction: In the Washington Double Star, component B is a 9.1 mag star located 3.7" away from A. System1123Orbit1End System1124Orbit1Begin The orbital elements derived for this ellipsoidal variable are described as `preliminary' by Burke and Abt, who believe that the system may be double-lined although they have failed to resolve the two spectra. They estimate that the two stars are of similar mass and luminosity and that the orbital inclination is around 40 deg. System1124Orbit1End System1125Orbit1Begin The M5 V spectrum can be seen on infrared spectrograms of this nova-like system. The orbit is assumed circular and the epoch is the time of inferior conjunction of the emission-line source. The values given for K1 and V0 are means for the emission lines H-beta and H-gamma, observed during the `low' state (i.e. the star was near the lower limit of its brightness). The helium emission lines give different values. The star may be a soft X-ray source (K.O. Mason, S.M. Kahn and C.S. Bowyer, Nature, 280, 568, 1979). System1125Orbit1End System1126Orbit1Begin Elements were recomputed by Luyten, who found a rather smaller eccentricity. Harper later revised the period to 4.8126d (Publ. Dom. Astrophys. Obs., 6, 241, 1935). The spectra are of nearly equal intensity. System1126Orbit1End System1127Orbit1Begin Original observations were made by W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 7, 1930), who found no need to revise his orbit later (Publ. Dom. Astrophys. Obs., 6, 242, 1935). He had to fix the value to T to obtain a solution, and Luyten's recomputation has therefore been preferred. Epoch is T0. Star is brighter member of A.D.S. 12075: B is 8.9m at 1.4". System1127Orbit1End System1128Orbit1Begin Young described the star as a subgiant: emission is visible in the H and K lines of Ca II. Lucy & Sweeney obtained similar orbital elements for the system. System1128Orbit1End System1129Orbit1Begin This object, still to our knowledge unique, attracted so much attention for a few years that already it is impossible to attempt a complete listing of papers even on spectroscopy, let alone those on radio and X-ray observations. The best guide to the literature up to 1984 is the review article by B. Margon (Ann. Rev. Astron. Astrophys., 22, 507, 1984). Among significant papers published since then may be cited a model discussed by G.W. Collins II and G.H. Newsom (Astrophys. J., 308, 144, 1986); observations of the optical continuous spectrum (R.M. Wagner, ibid., 308, 152, 1986); observations of the absolute variability of the emission lines (S.S. Asadullaev and A.M. Cherepashchuk, Astron. Zh., 63, 94, 1986) and observations of the X-ray spectrum (M.G. Watson et al., Mon. Not. Roy. Astron. Soc., 222, 261, 1986) and M. Matsouka, S. Takano and K. Makishima, ibid., 605, 1986). The generally accepted model remains that of a binary system, probably containing a compact component and accretion disk, ejecting a pair of relativistic precessing jets. A preliminary orbit for the binary was published by D. Crampton, A.P. Cowley and J.B. Hutchings (Astrophys. J., 235, L131, 1980). The orbital elements given are derived from measures of the emission line of He II at lambda 4686. Different elements are obtained from the H-beta emission and Fe II absorption lines. The epoch is T0 for the He II-line source and the orbit is assumed circular. Some of the light variation may be due to eclipses and a thorough discussion of UBV photometric observations has been published by E.M. Leibowitz et al. (Mon. Not. Roy. Astron. Soc., 206, 751, 1984) and E.M. Leibowitz (ibid., 210, 279, 1984). System1129Orbit1End System1130Orbit1Begin A circular orbit is assumed since the scatter of the observations does not permit a meaningful discussion of the orbital eccentricity. The epoch is the time of inferior conjunction of the Wolf-Rayet component. The elements are derived from several emission lines. Although the semi-amplitude of the velocity variation is small, the binary nature is probably established. The period remains uncertain but is close to 2.4 d. The star is of interest for its high systemic velocity (the highest known for a galactic W-R binary) and relatively high galactic latitude. The star is surrounded by expanding H II luminosity. System1130Orbit1End System1131Orbit1Begin Griffin comments that the colours indicate a spectral type slightly later than G5 V. The star is conventionally denoted as A.D.S. 12160 C. The primary component of this multiple `system' is H.D. 179588. Griffin points out, however, that the spectroscopic binary is not physically related to this star, which is about 2.0' away. System1131Orbit1End System1132Orbit1Begin The new orbital elements derived by Popper, Lacy and Frueh completely supersede the old ones derived for the primary component by O. Struve et al. (Astrophys. J., 111, 658, 1950). The photometric (V, R) observations published in the new paper likewise supersede earlier work. The epoch is the time of primary minimum and the orbit is assumed circular, in accord with both earlier spectroscopic work and a negligibly small photometric value of e cos omega. The secondary spectral type is estimated from the value of V R. The orbital inclination is found to be about 86 deg and the visual magnitude difference between the components is estimated at 1.46m. System1132Orbit1End System1133Orbit1Begin The magnitude given is for a phase near maximum light; eclipses are about 2m deep. A circular orbit is assumed and the epoch is the time of mid-eclipse. The value of K1 is derived from measures of the emission lines H-beta and H-gamma. The value of V0 depends strongly on the lines measured. Downes et al. estimate an orbital inclination of 78 deg. System1133Orbit1End System1134Orbit1Begin This is a triple system and there is also a visual orbit for the long-period pair, A.D.S. 122214 (W.H. van den Bos, Union Obs. Circ., 6, 378, 1961). The period adopted in the visual orbit (18.55y) is shorter than that found spectroscopically. The short-period pair is the visual secondary, although its total mass is greater than that of the visual `primary'. Fekel (private communication) has revised the elements (including the period) since publication of his paper, having now followed the long-period orbit through periastron. The revised elements are given in the Catalogue. The spectral types assigned are also based on a private communication from Fekel and were originally assigned by P. Schmidtke. The value K1=10.0 km/s refers to the centre of mass of the short-period pair, as also does the value omega=2.6 deg. According to van den Bos i=78.4 deg. The spectral types and luminosity classes quoted take into account the colours and parallax of the system and are not purely spectroscopic classifications. The determination of the short-period orbit is straightforward. The value of V0 refers to 1974.4. From the information obtained from the long-period orbit Fekel obtains i=74.5 deg for the close pair. System1134Orbit1End System1135Orbit1Begin This is a triple system and there is also a visual orbit for the long-period pair, A.D.S. 122214 (W.H. van den Bos, Union Obs. Circ., 6, 378, 1961). The period adopted in the visual orbit (18.55y) is shorter than that found spectroscopically. The short-period pair is the visual secondary, although its total mass is greater than that of the visual `primary'. Fekel (private communication) has revised the elements (including the period) since publication of his paper, having now followed the long-period orbit through periastron. The revised elements are given in the Catalogue. The spectral types assigned are also based on a private communication from Fekel and were originally assigned by P. Schmidtke. The value K1=10.0 km/s refers to the centre of mass of the short-period pair, as also does the value omega=2.6 deg. According to van den Bos i=78.4 deg. The spectral types and luminosity classes quoted take into account the colours and parallax of the system and are not purely spectroscopic classifications. The determination of the short-period orbit is straightforward. The value of V0 refers to 1974.4. From the information obtained from the long-period orbit Fekel obtains i=74.5 deg for the close pair. System1135Orbit1End System1136Orbit1Begin The elements of the orbit of this very low-amplitude binary are described as marginal by Abt and Levy themselves. The star is the brightest component of A.D.S. 12197, but the two companions (9.2m at 28.1" and 11.1m at 161") are probably optical. System1136Orbit1End System1137Orbit1Begin This is not strictly a `spectroscopic' binary since our knowledge of the orbit depends entirely on the variations in the period of the pulsar component produced by the light-time in the orbit. Consequently V0 cannot be determined at all. On the other hand, the other elements are known with unusually high accuracy. No eclipses are observed and it seems likely that the unseen companion is also a collapsed object. It has been pointed out that since very small changes in omega would be detectable, the system could be used as a test of the theory of general relativity (A.R. Masters and D.H. Roberts, Astrophys. J., 195, L107, 1975; K. Brecher, ibid., L113, 1975). Observations consistent with apsidal advance have been published (J.H. Taylor et al., Astrophys. J., 206, L53, 1976) but an unambiguous test of general relativity is not yet possible. The magnitude is that assigned to an optical object in coincidence with a radio source (J. Kristian and J.A. Westphal, I.A.U. Circ., No. 3242, 1978, P. Crane, J.E. Nelson and J.A. Tyson, Nature, 280, 367, 1979). No spectral type is given. System1137Orbit1End System1138Orbit1Begin This system belongs to A.D.S. 12239. The two principal visual components are separated by less than 1" and differ by only 0.1m in brightness. Thus the spectrum of the spectroscopic binary is influenced by that of the companion, especially at low dispersion. Since many of Hube's spectrograms are of low dispersion, he regards the orbital elements as preliminary. Although the brighter star's spectral type of B5 III is given in the Catalogue Hube believes the A-type component of the visual pair is the spectroscopic binary. A third component (8.6m at 47.6") is listed in I.D.S. System1138Orbit1End System1139Orbit1Begin These orbital elements are described as marginal by Abt and Levy themselves. The star is the brightest member of A.D.S. 12243: companions are 11.6m at 39.1" and 12.8m at 43.6". System1139Orbit1End System1140Orbit1Begin The epoch is T0. Luyten assumed the orbit to be circular, but there is now some photometric evidence for the value of e (0.053) found by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 141, 1919). Observations by J. Sahade and O. Struve (Astrophys. J., 102, 480, 1943) are also satisfied by Plaskett's elements, although W.H. Stilwell (Publ. Am. Astron. Soc., 10, 318, 1943), found a much larger eccentricity (0.154) while agreeing with Plaskett's value of K1. D.M. Popper (Publ. Astron. Soc. Pacific, 74, 129, 1962) confirmed Plaskett's value of K2 from measures of the D lines. Since the original values of K1, K2 and V0 have been confirmed, the elements are classified as b quality, but the value of the orbital eccentricity remains uncertain. The spectral type of the secondary was classified as A2 by Sahade and Struve, but Popper (Astrophys. J. Supp., 3, 107, 1957) points out that the colours during eclipse correspond to a G-type spectrum -- and this is confirmed by more detailed analysis of the light- curve. According to Koch et al., none of the available observed light-curves is completely satisfactory. J.B. Hutchings and G. Hill (Astrophys. J., 166, 373, 1971 and 167, 137, 1971) encountered difficulties in satisfying the photographic observations of M.I. Lavrov (Peremm. Zvezdy, 10, 9, 1954). The most recent rediscussion of the light-curve (B. Cester et al., Astron. Astrophys., 61, 469, 1977) results in a value of about 85 deg for the orbital inclination, a fractional luminosity (in B) of 0.98 for the primary star, and an estimated spectral type of G0 III-IV for the secondary. Modern observations, both spectroscopic and photometric, are desirable. System1140Orbit1End System1141Orbit1Begin Lucy & Sweeney adopt a circular orbit. System1141Orbit1End System1142Orbit1Begin The values of the elements for the primary component are taken from the study by D.H. McNamara cited in the Catalogue. This supersedes earlier work by M. Fowler (Publ. Allegheny Obs., 3, 14, 1912) and A.H. Joy (Astrophys. J., 71, 336, 1930) although some doubt remains about the reality of the small eccentricity. McNamara found different elements from measures of the hydrogen lines and of the other lines, and this is the principal reason for the d classification. The important value, K1, is, however, reasonably well known. The epoch given is the time of primary minimum, taken from J. Tomkin (Astrophys. J., 231, 495, 1979) who first succeeded in measuring a reliable value of K2. That value, confirmed by J.J. Dobias and M. Plavec (Publ. Astron. Soc. Pacific, 97, 138, 1985), is given (together with Tomkin's value of V0 ), in the Catalogue. The spectral types are those given by Dobias and Plavec. The spectroscopic mass-ratio does not, according to W. van Hamme and R.E. Wilson (Astron. J., 92, 1168, 1986) agree with the light-curve. Another important recent photometric study is by D.H. McNamara and K.A. Feltz (Publ. Astron. Soc. Pacific, 88, 688, 1976) who assumed an orbital inclination of 90 deg and found a fractional luminosity for the primary component (in y) of 0.87. B. Cester et al., (Astron. Astrophys., 61, 469, 1977) found similar results, making the primary somewhat brighter (relative to the secondary). E.C. Olson (Publ. Astron. Soc. Pacific, 94, 79, 1982) finds evidence for changes in size in one of the components. M. Plavec (Bull. Astron. Inst. Csl, 18, 93, 1967) established that the rotation of the primary is somewhat faster than would be required for orbital synchronism. Dobias and Plavec (loc. cit.) have found anomalous line strengths of C II that could be evidence that matter involved in nuclear processing has been brought to the surface. The magnitudes given are derived from the data of B. Cester and M. Pucillo (Mem. Soc. Astron. Ital., 43, 501, 1972). Variable polarization in the light of the system has been reported by O. Shulov (Astron. Tsirk. Kazan, No. 385, 5, 1966). D.S. Hall and F.G. van Landingham (Publ. Astron. Soc. Pacific, 82, 749, 1970) conclude that the star does not belong to the cluster Collinder 399. A 9.5m companion at 92" is listed in I.D.S. System1142Orbit1End System1143Orbit1Begin System1143Orbit1End System1144Orbit1Begin The orbital eccentricity is amongst the highest known for spectroscopic binaries. Franklin tested for eclipses, but with inconclusive results. There is an 11.1m companion listed in I.D.S. at 116". It is probably optical. System1144Orbit1End System1145Orbit1Begin The values of K2 and m2sin^3i depend on only four observations of the secondary component. Harper proposed later (Publ. Dom. Astrophys. Obs., 6, 242, 1935) to increase the period by 0.0009d. There is clearly an error, however, either in this figure or in the resulting value for the revised period. Petrie(II) found Delta m=1.25. System1145Orbit1End System1146Orbit1Begin The spectral type given is from the H.D. Catalogue. Griffin writes that the spectrometer traces suggest a type of F8 V. The star forms a spectacular optical pair with H.D. 181601. A faint and even more distant companion is also listed in I.D.S. System1146Orbit1End System1147Orbit1Begin Other investigations include a determination of orbital elements by R.E. Wilson (Lick Obs. Bull., 8, 132, 1914) in good agreement with those obtained by Seydel; by D.B. McLaughlin (Publ. Am. Astron. Soc., 9, 224, 1939) and by O.J. Eggen et al. (Publ. Astron. Soc. Pacific, 62, 171, 1951), who also confirm the elements. J.L. Greenstein published two extensive spectrophotometric studies (Astrophys. J., 91, 438, 1940; 111, 20, 1950). The visible spectrum of this hydrogen-deficient star shows features of both B8 and F2 types, but the two sets of lines are displaced in phase with respect to each other. Recent studies of the far UV spectrum indicate the presence of a hotter (O-type) component. For discussion of some of this work, see: H. Duvignan, M. Friedjung and M. Hack (Astron. Astrophys., 71, 310, 1979), M. Parthasarathy, M. Cornachin and M. Hack (ibid., 166, 273, 1986), M. Hack, U. Flora and P. Santin (I.A.U. Symp. No. 88, p. 271, 1980) and M.J. Plavec (Inf. Bull. Var. Stars, No. 1598, 1979). A light variation was discovered by S. Gaposchkin (Astron. J., 51, 109, 1945), who ascribed it to eclipses. This was confirmed by Eggen et al. who, however, pointed out a difference between the photometric and spectroscopic times of conjunction. G.J. Malcolm and S.A. Bell (Mon. Not. Roy. Astron. Soc., 222, 543, 1986) find a 21-day approximate periodicity in the light variation which is consistent in nature with some form of pulsation. Their observations neither demonstrate nor rule out the supposed eclipses. System1147Orbit1End System1148Orbit1Begin The epoch is T0 and a circular orbit was assumed. An earlier investigation by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 251, 1920) yielded K1=96.35 km/s, K2=213.74 km/s. Popper's own values are given in the Catalogue although he adopted 92 km/s and 219 km/s, respectively, for the computation of masses. From his own photoelectric light-curve he determined i=88 deg, Delta m=1.2 (c.f. Petrie(II) Delta m=1.09) and spectral types of B4 and B6. Similar results for the inclination and relative luminosities were obtained by H. Minti and R. Dinescu (Stud. si Cerc. Astron., 14, 177, 1968). B. Cester et al. (Astron. Astrophys., 61, 469, 1977) re-analyzed Popper's photometric observations and those of P. Broglia (J. Observateurs, 47, 99, 1964). They also found an inclination close to 89 deg and a fractional luminosity (in V) for the primary star of 0.95. They deduced a somewhat earlier type for the primary than Popper finds by direct classification. The star is the brighter member of A.D.S. 12538: B is 9.8m at 25.2". System1148Orbit1End System1149Orbit1Begin Luyten's recomputation of the orbit is preferred to the original analysis by R.K. Young (Publ. Dom. Obs., 4, 55, 1917) of his own observations. Luyten assumed a circular orbit and the epoch is T0. W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 243, 1935) revised the period to 7.3919d. The star is classified as A2 from the K line, and A7 from the metallic lines. According to Petrie(II), Delta m=0.65. System1149Orbit1End System1150Orbit1Begin Although no M-K classification was available to Griffin, he believes the star to be a giant. System1150Orbit1End System1151Orbit1Begin The recent history of this irregular variable is well known and several references to studies of the star are given by Yamashita and Maehara. Although the star was once considered an M-K standard for the type M7 III, it is now recognized as showing also a blue continuum and emission lines of ionized metals. This alone strongly argues for its binary nature, but the elements given here depend on heterogeneous data and are correspondingly uncertain. The lines of ionized metals are displaced approximately 0.25m out of phase with those of the M-type spectrum. The former satisfy a circular orbit, with the same value of V0 as the M-type star and a K1 equal to 9.0 km/s. System1151Orbit1End System1152Orbit1Begin Lucy & Sweeney derived similar elements from these observations. Although the spectrum is classified as A3p by Evans et al. the star is not listed by Bertaud and Floquet, or by Curchod and Hauck. System1152Orbit1End System1153Orbit1Begin The period is long and the amplitude of velocity variation low. Abt and Snowden themselves remark that more observations are needed `before the reality of this binary motion is assured'. System1153Orbit1End System1154Orbit1Begin Because of the difficulty of separating pulsational velocities of this Cepheid from orbital motion, and because of the use of heterogeneous data from several sources, the elements are only approximately determined. The secondary component is believed to be of spectral type A2. The star is the brightest member of A.D.S. 12503: companions are 11.7m at 1.5" and 13.2m at 35.2". System1154Orbit1End System1155Orbit1Begin Radford and Griffin believe that the star may be a little brighter than the 7.5m given in the H.D. Catalogue. System1155Orbit1End System1156Orbit1Begin The spectral type of B8 V is a mean of the types of the two components in this system. D.M. Popper (Publ. Astron. Soc. Pacific, 93, 318, 1981) has pointed out that the helium lines are displaced out of phase with the others; he estimates that the two stars are B3 and B9 and suspects that the magnitude difference is less than would be expected for two main-sequence stars of these types. T.M. Rachkovskaja (Izv. Krym. Astrofiz. Obs., 64, 81, 1981) also estimates spectral types of B2.5 and B9.5. Popper gives a semi-amplitude of 126 km/s from the hydrogen lines and 196 km/s from the line of Mg II at lambda 4481. He found it impossible to derive the velocity-amplitude of the component producing the helium lines. Rachkovskaja, like Popper, assumed a circular orbit and derived K1=140 km/s, K2=113km/s. For the time being, FitzGerald's elements are accepted, but they are clearly only provisional and they have been reclassified from c to d. The epoch is T0. Observations at H-alpha have been published by V. Ya. Alduseva and E.A. Kolotilov (Astron. Tsirk., No. 1212, 1982). A time of minimum was published by D.S. Hall (Publ. Astron. Soc. Pacific, 79, 630, 1967) and a photoelectric light-curve by V. Ya. Alduseva and V.M. Kovalenko (Astron. Tsirk., No. 956, 1977), but no photometric analysis appears to have been undertaken. A systematic study of this relatively bright binary is desirable. The star is the brighter member of A.D.S. 12538: B is 9.8m at 25.2". System1156Orbit1End System1157Orbit1Begin The spectral type given is from the H.D. Catalogue and is a mean for the two stars. Imbert suggests individual types of F7 V and G0 V. The epoch is T0 for the brighter component: the orbit was assumed circular. No detailed analysis of the light-curve seems to have been made. From considerations of the spectral type, duration of eclipses, minimum masses and ratio of luminosities, Imbert deduces an orbital inclination of 89 deg and a visual magnitude difference of 0.4m. System1157Orbit1End System1158Orbit1Begin The orbit is assumed circular and the epoch is T0. Coverage of the velocity-curve is not complete. System1158Orbit1End System1159Orbit1Begin The period is not well determined because only a few cycles have been observed. Lucy & Sweeney adopt a circular orbit. System1159Orbit1End System1160Orbit1Begin The magnitude given is an approximate out-of-eclipse value. The system is still subject to appreciable changes of brightness (it was Nova Sge 1783) independently of the eclipses. The epoch is the time of primary minimum. A circular orbit was assumed. It is suggested that the secondary component is an M-type dwarf. System1160Orbit1End System1161Orbit1Begin Although the star is described as having a composite spectrum, Sanford pointed out that the hydrogen lines show the same Doppler displacements as do the other lines. He failed to detect a suspected short-period variation in the velocities. Lucy & Sweeney adopt a circular orbit. System1161Orbit1End System1162Orbit1Begin This star was adopted as an I.A.U. velocity standard for many years, although suspicions of its variability were voiced by R.M. Petrie and J.A. Pearce (Publ. Dom. Astrophys. Obs., 12, 1, 1961). The present orbit is based almost exclusively on measurements with the radial-velocity spectrometer. The traces from the two components are properly resolved only at one node, and the elements given depend on successfully deconvolving the traces at the other node. The ratio of the `dips' produced by each component, which is approximately the ratio of their luminosities at photographic wavelengths, is 0.78. System1162Orbit1End System1163Orbit1Begin The new observations by Walker and Jones agree quite well with the earlier ones by H.A. Abt (Astrophys. J., 133, 910, 1961) which are included in the present solution. The spectrum is classified as A3, A8, and F2 III from the K line, the hydrogen lines, and the metallic lines respectively. The star is included in H.W. Babcock's Catalogue of Magnetic Stars (Astrophys. J. Supp., 3, 141, 1958). Its light has been suspected of variability, and Walker and Jones discuss the possibility of a small-amplitude, short-period variation in the velocity which might perhaps indicate that the primary component is a delta Sct star. System1163Orbit1End System1164Orbit1Begin The magnitude given is from the H.D. Catalogue: photoelectric measures show that the star varies in brightness through a range of 0.15m (in V), twice in the orbital period. The star belongs to the RS CVn class. The unpublished elements given in the Catalogue are an improvement on the preliminary ones published by B.W. Bopp et al. (Astron. J., 87, 1035, 1982). Reference: F.C.Fekel,,,, (Unpublished) System1164Orbit1End System1165Orbit1Begin An earlier investigation by F.C. Jordan (Publ. Allegheny Obs., 3, 189, 1916) yielded results in good agreement with those of Luyten et al. The epoch is T0 and a circular orbit was assumed. O. Struve (Astrophys. J., 85, 41, 1937) discussed the variation of line intensities in the spectrum of the fainter star. C.C. Wylie (Astrophys. J., 56, 232, 1922) made photometric observations from which he deduced i=71.7 deg on the assumption that Delta m=0.31. Petrie(I) found Delta m=0.81. A new analysis of Wylie's observations by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) confirmed his value of the inclination and gave a fractional luminosity of 0.78 for the hotter star. The star is the brighter member of A.D.S. 12737: B is 12.1m at 47.8". System1165Orbit1End System1166Orbit1Begin The spectrum of this ex-nova shows hydrogen and (weak) helium lines in emission, and a late- type spectrum (probably G or K) in absorption. The epoch is T0 as determined from the absorption lines (which give the smaller value of K on the lower line of the Catalogue entry). The emission lines do not vary precisely 180 deg out of phase with the absorption lines. The orbit was assumed to be circular. The dispersion employed was necessarily low, and individual observations show a large scatter. The magnitudes quoted in the Catalogue give only an approximate idea of the variation in brightness. According to Robinson, both the shape and depth of the eclipses vary considerably. Furthermore, the system is subject to eruptions of up to 2.0m, approximately every 20 days, and to flickering on time scales of a few minutes. Robinson estimates the orbital inclination to be in the neighbourhood of 63 deg. New optical and infrared light-curves obtained by R.F. Jameson, A.R. King and M.R. Sherrington (Mon. Not. Roy. Astron. Soc., 195, 235, 1981) lead to an estimate of 69 deg for the inclination. These authors also estimate that the secondary component is a K2 V star. System1166Orbit1End System1167Orbit1Begin The spectrum may be somewhat later than K2 and the star is probably a giant. The observations cover only one cycle. Griffin suggests that the components might be resolvable by speckle interferometry. System1167Orbit1End System1168Orbit1Begin The system is of interest because of the rarity of double-lined spectroscopic binaries composed of two giants. The types and intensities of the two spectra are closely similar. System1168Orbit1End System1169Orbit1Begin The spectroscopic observations by Andersen et al. supersede earlier work by M.S. Snowden and R.H. Koch (Astrophys. J., 156, 667, 1969) and by W.E. Harper, (Publ. Dom. Astrophys. Obs., 1, 157, 1919 and 6, 243, 1935). The effective temperatures, and therefore the spectral types, are closely similar. The epoch is the time of primary minimum. Several light-curves have been published and are discussed together by Andersen et al. They used the spectroscopically evaluated luminosity-ratio to obtain a determinate solution, and found an orbital inclination close to 87 deg and a visual magnitude difference between the components of 0.07m. There is evidence for apsidal motion with a period of about 10,000 years (Kh.F. Khaliullin, Astron. Tsirk., No. 1262, 1983). System1169Orbit1End System1170Orbit1Begin Elements were also computed from these observations by Luyten, and Lucy & Sweeney who adopted a circular orbit. Photometric and spectroscopic observations were published by P. Guthnick (Sitzb. Preuss. Akad. Wiss., 1930, p. 497 and 1934, p. 521). He could not fit his photometric observations meaningfully to Hill's value of the period, but found that they showed two eclipses when plotted on the period P=2.5133d. In the second of his papers he stated that both the Victoria, and the Berlin measures of radial velocity could be represented on this period. He also suggested a somewhat higher value of K, but did not derive orbital elements. New elements have been derived by D.S. Holmgren (Bull. Am. Astron. Soc., 19, 709, 1987) who finds K1=58.4 km/s, but his results are not yet published in sudegcient detail to be assessed fully. The values he gives for K1 and f(m) imply a value close to Guthnick's for the period. The spectrum is difficult to measure and the residuals are large. The eclipsing binary is one member of a close visual binary (Kuiper 93) which was unresolvable in 1961. G.F.G. Knipe (Publ. Astron. Soc. Pacific, 83, 352, 1971) has shown that the period changed very sharply about then. It is, however, apparently again close to 2.5133d. System1170Orbit1End System1171Orbit1Begin Identification is from the Cordoba Durchmusterung. The new observations by Haug and Drechsel almost certainly rule out the period of approximately 0.21d adopted by A.P. Cowley, D. Crampton and J.E. Hesser (Astrophys. J., 214, 471, 1977). The system is a cataclysmic variable and an X-ray source. The light variations do not appear to arise from eclipses. The elements given are determined from the absorption lines of H-beta, H-gamma and H-delta in the white-dwarf spectrum. If measurements made only on symmetrical line profiles are used in the analysis, the value of K1 is reduced to 199 km/s. The epoch is superior conjunction of the white dwarf and the orbit is assumed circular. The absorption lines of He I at lambda lambda 4388 and 4922 give velocities that vary out of phase with those obtained from the hydrogen lines, but not by 180 deg. It is, therefore, questionable whether or not these lines are part of the secondary spectrum. For the results of spectrophotometry, see R.J. Panek (Astrophys. J., 234, 1016, 1979) and for a description of the UV spectrum, see E.F. Guinan and E.M. Sion (ibid., 258, 217, 1982). System1171Orbit1End System1172Orbit1Begin The magnitude is variable and the star is a Cepheid. Despite the difficulties of separating the two stellar motions (orbital and pulsational), these elements appear to be well determined. From the mass-function, Imbert deduces that the invisible secondary is a B-star. He also computes the radius of the Cepheid (by Wesselink's method) as 43.9 RSol. System1172Orbit1End System1173Orbit1Begin Massey's observations supersede earlier work by K.S. Ganesh and M.K.V. Bappu (Kodaikanal Bull., Series A, 185, 1968) and W.A. Hiltner (Astrophys. J., 101, 356, 1945). The elements given for the W-R component (upper line) are derived from measures of the He II emission line lambda 4686. Lines of N V give different values and, specifically, lower values for K1. The epoch given is the time of inferior conjunction of the W-R star. The orbit was assumed circular after a preliminary solution showed any eccentricity to be comparable in size with its uncertainty. The spectral type of the O star can be only approximately determined: this star is about 1.3m brighter than the W-R component. The minimum masses derived suggest that the system may be eclipsing. Some discussion of the UV spectrum has been published by J.B. Hutchings and P. Massey (Publ. Astron. Soc. Pacific, 95, 151, 1983). System1173Orbit1End System1174Orbit1Begin No completely satisfactory set of orbital elements has yet been published for this bright long-period system. The elements given here are derived from observations that cover less than a complete cycle. Nevertheless, they are an improvement on the elements published by W.H. Christie (Astrophys. J., 83, 433, 1936) and D.B. McLaughlin, E.B. Weston and M. Chadwick (Publ. Astron. Soc. Pacific, 64, 300, 1952) as well as the more recent set published by D. Reimers and K.-P. Schroder (Astron. Astrophys., 124, 241, 1983). Determination of elements of the M-type component is made difficult by occasional large residuals (in each direction) from the velocity-curve, which appear to have their origin in motions in the atmosphere of this bright giant. Although the spectrum of the early-type component is clearly visible from about H-epsilon to shorter wavelengths, separating and measuring it has not yet proved possible. A.H. Batten and W.A. Fisher (Publ. Astron. Soc. Pacific, 93, 769, 1981) confirmed the observation by McLaughlin et al. that the system undergoes at least an atmospheric eclipse. Reimers and Schroder (loc. cit.) and D. Reimers and R.P. Kudritzki (Proc. 2nd. European IUE Conf. ESA SP-157, 1980, p. 229) describe the far UV spectrum and discuss the rate of mass loss from the giant star. The system has been resolved by speckle interferometry (H.A. McAlister et al., Astrophys. J. Supp., 54, 251, 1984). System1174Orbit1End System1175Orbit1Begin This Wolf-Rayet star is associated with a ring nebula and shows light and velocity variations in the same period. The magnitude given is an approximate mean V magnitude. The orbit is assumed circular and the epoch is the time of minimum light, which corresponds approximately to the time of inferior conjunction of the W-R star. Values given for K and V0 are approximate; the velocities are the means of measures of emission lines lambda 4686 He II and lambda 4604 & 4619 N V. Antokhin, Aslanov and Cherepashchuk suggest that the companion may be a neutron star. System1175Orbit1End System1176Orbit1Begin Radford and Griffin give reasons for supposing that the companion is a main-sequence star of early B spectral type. They suggest that the system may show eclipses and that it is analogous to systems of the zeta Aur type. System1176Orbit1End System1177Orbit1Begin The new observations confirm the earlier work of P.W. Merrill (Astrophys. J., 110, 59, 1949). Just as he did, Hutchings and Redman find a component of the hydrogen lines that yields a constant velocity about 70 km/s more negative than that of the system, while the Balmer emission shows a different variation about a value some 80 km/s more positive than the velocity of the system. Light variations are complex but may include shallow eclipses, and the orbital inclination may be close to 90 deg. J.B. Hutchings and P.G. Laskarides (Mon. Not. Roy. Astron. Soc., 155, 357, 1972) discuss the shell around the star, and spectrophotometric studies have also been published by N.L. Ivanova and A.H. Khotyanskii (Astrofiz., 12, 623, 1976). System1177Orbit1End System1178Orbit1Begin The system has been known to be a two-spectra binary since the work of J.S. Plaskett and J.A. Pearce (Publ. Dom. Astrophys. Obs., 5, 1, 1930), but no orbital elements were published until the work of P. Mayor and D. Chochol (Publ. Astron. Soc. Pacific, 93, 608, 1981), who also demonstrated that the system displays nearly equal eclipses of about 0.15m depth in V. Hill and Fisher were able to detect the secondary spectrum (on Victoria spectrograms obtained between 1924 and 1983) because they measured them by cross-correlation. Mayor and Chochol find some evidence for slow apsidal motion in the system, which is not contradicted by the available spectroscopic material. Preliminary analysis of the photometric observations leads Hill and Fisher to adopt an orbital inclination of about 84 deg and a visual magnitude difference between the components of about 3m. The system belongs to Cyg OB5. System1178Orbit1End System1179Orbit1Begin This is a symbiotic star also believed to be a long-period eclipsing binary. Measures of the TiO bands and of the Balmer emission lines show velocity variations of opposite phase from each other. The epoch is the time of primary minimum. The orbit is assumed circular. Nova-like outbursts, as well as eclipses are observed in the system. System1179Orbit1End System1180Orbit1Begin The orbital elements of the primary component are now very well known, with investigations by W.E. Harper (Publ. Dom. Astrophys. Obs., 1, 257, 1920 and 6, 244, 1935), D.M. Popper (Astrophys. J., 109, 100, 1949), Z. Daniel (unpublished) and A.H. Batten (Publ. Dom. Astrophys. Obs., 12, 91, 1962) all agreeing except for the variable quantity omega. The last-named investigation depends, in large measure, on the same material as was used for that in the Catalogue. Batten's identification and measurement of features in the secondary spectrum was questioned by D.M. Popper (Astrophys. J. Supp., 47, 339, 1981) and C.H. Lacy (Inf. Bull. Var. Stars, No. 2489, 1984) but measurements by cross-correlation have confirmed the reality of the features and improved the accuracy of measurement. Nevertheless, the orbital elements of the secondary are definitely less well-known than those of the primary. The spectral types given are based on consideration of the UV spectrum and measurement of the equivalent widths, rather than on traditional methods of classification. Photometric (I. Semeniuk, Acta Astron., 18, 1, 1968, P. Battistini et al., Astrophys. Space Sci., 30, 163, 1974) and spectroscopic measurements agree in indicating apsidal motion in a period of the order of 1500 years -- about the value to be expected. Although no complete modern light-curve has been published, analysis of the available photoelectric observations suggests an orbital inclination of about 80 deg and a visual magnitude difference between the components of 2.9m. Several uncertainties about this system do now seem to have been cleared up. System1180Orbit1End System1181Orbit1Begin The epoch is T0 and the orbit was assumed circular. Lucy & Sweeney also derived a circular orbit. Light-curves on the UBV system have been published by C.R. Chambliss (Astron. J., 77, 672, 1972). He finds that the period is apparently steadily decreasing. He also finds an inclination of between 79 deg and 80 deg, and a fractional luminosity (in V) of the primary star of 0.88. Despite the difference in spectral types (Chambliss gives G6-8 IV for the secondary) the two stars are nearly equal in size. A new discussion of the available photometric material (M. Mezzetti et al., Astron. Astrophys. Supp., 39, 273, 1980) gives similar results. System1181Orbit1End System1182Orbit1Begin The components of this system, which resemble in some respects those of dwarf binaries in the Hyades, have a high metal abundance. The magnitude difference between the stars is estimated to be less than 0.1m. Fekel and Beavers suggest that a search be made for eclipses. The star is the brightest component of A.D.S. 13072, but the 10.3m `companion' is optical. System1182Orbit1End System1183Orbit1Begin The secondary spectrum is very faint, and the values of K2, m1sin^3i and m2sin^3i are correspondingly uncertain. System1183Orbit1End System1184Orbit1Begin Only an approximate magnitude is known for this star. No trace of the secondary spectrum is seen; Griffin speculates that it might be that of a main-sequence star of type F. System1184Orbit1End System1185Orbit1Begin Earlier investigations were published by T.S. Jacobsen (Lick Obs. Bull., 13, 112, 1928) who detected the long-period variation, but was unable to determine its period, and J.A. Aldrich (Publ. Michigan Obs., 4, 75, 1932) who determined provisional elements similar to those in the Catalogue. Herbig and Moore succeeded in separating the two radial-velocity variations involved in the orbital motion (P=676.2d) and in the Cepheid pulsation (P=8.38d). The spectral type varies between the limits shown, during the Cepheid cycle. A detailed discussion of emission lines in the spectrum is given by Herbig (Astrophys. J., 116, 369, 1952). No trace of the secondary spectrum has been found. System1185Orbit1End System1186Orbit1Begin The recomputation of the orbital elements by Lucy & Sweeney is preferred to W.E. Harper's own analysis (Publ. Dom. Astrophys. Obs., 6, 245, 1935) because Harper had to fix T to obtain a solution. Like Luyten, who recomputed Harper's (Publ. Dom. Astrophys. Obs., 2, 179, 1922) earlier orbital solution, Lucy & Sweeney adopted a circular orbit. The epoch is T0. System1186Orbit1End System1187Orbit1Begin These elements are based on the same observations as the elements derived by R.F. Griffin (Observatory, 97, 15, 1977). They provide a rare example of an elliptical orbit that was wrongly assumed to be circular. The star is a visual binary (A.D.S. 13125) consisting, presumably, of approximately equal components with an orbital period of 26 years (G. van Biesbroeck, Publ. Yerkes Obs., 5, part 1, 246, 1927). Both of these components contribute to the observed spectrum, so the velocity amplitude is not well determined. There is some evidence for a variation in V0, which, of course, is to be expected. System1187Orbit1End System1188Orbit1Begin System1188Orbit1End System1189Orbit1Begin A circular orbit was assumed for this cataclysmic variable and the epoch is the time of inferior conjunction of the emission-line source. System1189Orbit1End System1190Orbit1Begin The significance of T is not defined. The quality is assigned on the basis of the number of spectrograms measured and the published probable errors. The promised full account apparently never appeared in the Lick Obs. Bull.. Reference: R.E.Wilson & C.M.Huffer, Pop. Astr., 29, 85, 1921 System1190Orbit1End System1191Orbit1Begin This star has been known to be a binary since at least 1928, but no orbital elements (except P and V0) were published for it until the values obtained by P.M. Millman in that year were included in the Sixth Catalogue. Later, because of difficulties in reconciling old and new observations from Victoria, as well as a series of observations made from Allegheny (W.L. Beardsley, Publ. Allegheny Obs., 8, No. 7, 1969) the system was withdrawn from the Seventh Catalogue. The revision to the period has reconciled the different observations, although the period given can only be regarded as approximate. The `peculiarity' of the spectrum is primarily an appearance, at some phases, that the hydrogen lines are too strong for the assigned type. This appearance may arise from blending with the secondary spectrum, which most investigators have thought they could see but have been unable to measure. This blending may also explain why the hydrogen, helium and metal lines give different orbital elements. In particular, if the hydrogen-line measures were omitted from the mean velocities, K1 would be appreciably higher. J. Tomkin (private communication) confirms the visibility of the secondary spectrum and suggests that the star producing it is hotter than the so-called primary. If this is correct, it invalidates the prediction of eclipses made by Batten, Fisher and Fletcher. An 8.5m companion at 64.6" is listed in I.D.S. System1191Orbit1End System1192Orbit1Begin The eccentricity and longitude of periastron found by Heard and Morton are confirmed by Lucy & Sweeney and were supported by the photoelectric light-curve obtained by A. Fresa (Mem. Soc. Astron. Ital., 27, 187, 1956). More modern light-curves, however, indicate a much smaller eccentricity (M. Rodono, Mem. Soc. Astron. Ital., 38, 465, 1967, A.Y. Ertan, Astrophys. Space Sci., 77, 391, 1981). Rodono's observations have also been analyzed by F. Mardirossian et al. (Astron. Astrophys. Supp., 39, 235, 1980). All agree on a fractional luminosity (in V), for the hotter star, of at least 0.95, but estimates of the orbital inclination range from 77 deg to 87 deg. System1192Orbit1End System1193Orbit1Begin These elements of Cyg X-1 are a refinement of the earlier study by C.T. Bolton (Astrophys. J., 200, 269, 1975) in which references to still earlier studies may be found. The system remains the one, out of all claimed to contain a black hole, that seems most probable to do so. Gies and Bolton have looked for changes in the period, including those that might arise from apsidal motion if the eccentricity were not quite zero, but have detected none. The epoch is the time of inferior conjunction of the component producing the absorption lines. Measures of hydrogen and helium lines lead to different values of the orbital elements. The system is an ellipsoidal variable. The light-curve is discussed by R.E. Wilson and R.K. Fox (Astron. J., 86, 1259, 1981) who also give references to earlier photometric work. The orbital inclination is probably in the range 30 deg to 40 deg. Wilson and Fox found a non-zero eccentricity and evidence for apsidal motion -- but neither are supported by the spectroscopic results. Optical emission lines vary out of phase with the absorption lines; J.B. Hutchings et al. (Astrophys. J., 182, 549, 1973 and 191, 743, 1974) deduce a mass-ratio of about 1.6 and certainly less than 2 -- with the visible star being the more massive. Measures by O.E. Aab (Pis. Astron. Zh., 9, 606, 1983), based on the He II emission line lambda 4686 give an estimated mass-ratio, in the same sense, of 1.5. Work by G.A.H. Walker, S. Yang and J.W. Glaspey (Astrophys. J., 226, 976, 1978) shows the intensity of this emission line to be variable. The H-alpha line has been studied by J.B. Hutchings, D. Crampton and C.T. Bolton (Publ. Astron. Soc. Pacific, 91, 796, 1979) and results from IUE spectra were published by A.K. Dupree et al. (Nature, 275, 400, 1978) and R. Davis and L. Hartmann (Astrophys. J., 270, 671, 1983). J.C. Kemp, L.C. Herman and M.S. Barbour (Astron. J., 83, 962, 1978) find some evidence for a longer periodicity than the orbital period, in polarization observations, but H.A. Abt, P. Hintzen and S.G. Levy (Astrophys. J., 213, 815, 1977) could find no evidence for a detectable third body in the system. System1193Orbit1End System1194Orbit1Begin Lucy & Sweeney adopt a circular orbit. The star is the brighter component of A.D.S. 13256: B is 7.8m at 4.0". System1194Orbit1End System1195Orbit1Begin Popper's observations and orbital elements agree well with those published earlier by P. FitzGerald (Publ. David Dunlap Obs., 2, 417, 1964). A circular orbit was assumed (now confirmed by the light-curve) and the epoch is the time of primary minimum. Several photoelectric (BV) light-curves have been published: N. Gudur et al. (Astron. Astrophys. Supp., 36, 65, 1979) also analyzed by G. Russo et al. (Astrophys. Space Sci., 79, 359, 1981); D. Chis et al. (Inf. Bull. Var. Stars, No. 1794, 1980) published in more detail by C. Cristescu et al. (Acta Astron., 31, 505, 1981) and D.M. Popper and P.J. Dumont (Astron. J., 82, 216, 1977) analyzed by D.M. Popper and P.B. Etzel (ibid., 86, 102, 1981). All analyses agree that the orbital inclination is very close to 90 deg and the two components are within a few percent of equality of brightness. System1195Orbit1End System1196Orbit1Begin This is another mercury-manganese star that appears to be binary. Both the velocity variation and the approximate period were known before the work of Stickland and Weatherby. System1196Orbit1End System1197Orbit1Begin The epoch is T0. The orbit was assumed circular, an assumption later confirmed by Lucy & Sweeney. Photoelectric UBV light-curves have been published by D.S. Hall and A.S. Wawrukiewicz (Publ. Astron. Soc. Pacific, 84, 541, 1972) who find i=87.3 deg and that the brighter star gives 0.9 of the total V light of the system. The secondary spectrum can be seen in primary eclipse and was classed simply as G by Struve. The type given in the Catalogue is deduced from the UBV colours by Hall and Wawrukiewicz. The new photometric solution makes it appear less likely that this system contains an `undersize' subgiant. The photometric results are confirmed by a new analysis of the same observations by M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 265, 1980). System1197Orbit1End System1198Orbit1Begin Lucke and Mayor suggest that this system might be eclipsing. The star is the brighter member of A.D.S. 13344: companion is 11.0m at 2.3". System1198Orbit1End System1199Orbit1Begin This is another X-ray cataclysmic binary of the AM Her sub-group. The magnitude given is an isolated measurement by J.A. Nousek et al. (Astrophys. J., 277, 682, 1984), who also published values of K1 and V0. The star's light is subject to variations of about one magnitude, due to eclipses, and to other variations as well. The epoch is the time of the linear polarization pulse: inferior conjunction of the emission-line source is 0.20m later. The orbit is assumed circular. The elements given are derived from measures of the emission line H-beta. Other lines give very different values for both V0 and K. Results of IUE observations are presented and discussed by K. Mukai et al. (Mon. Not. Roy. Astron. Soc., 221, 839, 1986). K. Mukai and P.A. Charles have measured the Na I doublet lambda lambda 8183--94 in the spectrum of the secondary component and deduce K2=209km/s +/-28 km/s, V0=17km/s +/-23 km/s. System1199Orbit1End System1200Orbit1Begin The new observations by Popper show several disagreements with the older ones by J.A. Pearce (Publ. Dom. Astrophys. Obs., 10, 447, 1958) although they probably represent an improvement in our knowledge of the system. Popper adopted the value of e found photometrically by D.J.K. O'Connell (Vistas in Astron., 12, 271, 1970). The system shows well-established apsidal motion in a period of 349 years (in good agreement with Pearce's spectroscopic estimate of 400 years) and the value of omega given in the Catalogue is a rough mean for the interval 1956--1965 during which Popper's plates were obtained. In fact, according to O'Connell's ephemeris, omega varied from 136.5 deg to 147.0 deg during this interval. The secondary spectrum is too weak to be easily classified. Popper's F2, somewhat earlier than Pearce's F5, appears to be deduced from the photometric colours. Of several photoelectric studies of the system, O'Connell's UBV light-curves are the most recent and thorough. Apart from the result on apsidal motion, he deduces i=88 deg and the light of the larger star (in V) is 0.85 of the total. Fourier analyses of other light-curves by H.M.K. Al Naimiy (Astrophys. Space Sci., 59, 3, 1978) yield similar results. System1200Orbit1End System1201Orbit1Begin Epoch is T0 for the B-type component: circular orbit assumed. Note the large difference in the values of V0 required to satisfy the observations of each component. The upper line refers to the Wolf-Rayet component. New elements have been published by D. Fraquelli (J. Roy. Astron. Soc. Can., 71, 407, 1977), but with insufficient detail for a decision whether or not they represent an improvement. Star is probably a member of the cluster N.G.C. 6871 which is also A.D.S. 13374. System1201Orbit1End System1202Orbit1Begin The spectral types come from a spectrophotometric study by L.V. Glazunova, V.G. Karetnikov and S.V. Kutsenko (Astron. Zh., 63, 702, 1986) who also note asymmetries and anomalies in the profiles of both the hydrogen and helium lines. They detect emission at H-alpha. Petrie's measurements of the secondary spectrum probably do not represent the true motion of the star. The only published light-curve (based on visual observations) was discussed by J. Ashbrook (Harvard Obs. Bull., No. 916, 7, 1942). It is not clear whether eclipses are total or partial. Assuming primary eclipse to be total, Ashbrook found i=79.5 deg and the light-ratio to be about 0.43. Petrie found Delta m=0.2 from measures of the H-gamma absorption in each spectrum but earlier (II) found Delta m=0.64. His orbital determination appears to supersede the list of Delta m values, and the components must be, spectroscopically, of nearly equal luminosity. This star is also a member of N.G.C. 6871. System1202Orbit1End System1203Orbit1Begin Seven new spectroscopic observations have been published by H.A. Abt et al. (Astron. J., 77, 138, 1972) which give K1=152 km/s. Pearce's results are preferred to one based on so few spectrograms, especially since D.M. Popper (Astrophys. J., 220, L11, 1978) reports that the published masses need little revision. Two UBV studies have been published by H.L. Cohen (Astron. Astrophys. Supp., 15, 181, 1974) and A.A. Wachmann (Astron. Astrophys., 34, 317, 1974). These, and the work of Abt et al. suggest that the period is somewhat longer (3.8898d) than Pearce found. Although the photometric eccentricity (0.02) is smaller than that found spectroscopically, Wachmann finds evidence for apsidal motion in a period of 71 years. Cohen's observations have also been analyzed by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) and by M. Kitamura and Y. Nakamura (Ann. Tokyo Obs., 21, 229, 1986). The orbital inclination is close to 86 deg and the brighter component gives 0.74 of the total light (in V). The star is a member of N.G.C. 6871. System1203Orbit1End System1204Orbit1Begin Several attempts have been made to determine the orbital elements of this recurrent nova: D. Crampton, J.B. Hutchings and A.P. Cowley (Astrophys. J., 234, 182, 1979), R.L. Gilliland and E. Kemper (ibid., 236, 854, 1980) -- who give a model -- and R.L. Gilliland, E. Kemper and N. Suntzeff (ibid., 301, 252, 1986). Some of these were made during the 1978 outburst and others during quiescence. This may partly account for the lack of agreement between them. Although the study by Walker and Bell was made during the outburst, it appears to be the most thorough. The epoch is the time of primary minimum. The elements given are derived from measures of the hydrogen absorption lines. No value is given for omega -- the shape of the velocity-curve suggests that omega is in the first quadrant. If the same measurements are made to fit a circular orbit (since e is probably spurious), neither K1 nor V0 is much changed. The He I and Ca II lines do give a somewhat (but not significantly) higher value for K1. The photometric behaviour of the system at minimum light is discussed in detail by E.L. Robinson, R.E. Nather and J. Patterson (Astrophys. J., 219, 168, 1978). Their deductions have, however, been criticized by A.C. Fabian et al. (Mon. Not. Roy. Astron. Soc., 184, 835, 1978) and H. Ritter and R. Schroder (Astron. Astrophys., 76, 168, 1979). A model has also been put forward by J. Smak (Acta Astron., 29, 325, 1979). The photometric behaviour during outburst is described by J. Patterson et al. (Astrophys. J., 248, 1067, 1981). System1204Orbit1End System1205Orbit1Begin The epoch is T0 and the small eccentricity probably is an artifact of the orbital solution. Both stars have peculiar spectra that show the Hg II line. The primary spectrum also shows Mn II lines, while the secondary does not. On the other hand, lines of Pt II and Y II are strong in the secondary spectrum, and weak or missing from the primary. Dworetsky compares the system to that of 46 Dra (H.D. 173524). System1205Orbit1End System1206Orbit1Begin The value of K2, and therefore the total mass of the system, must be considered as very poorly determined. The probable error of an average measure of the secondary component is 25 km/s. Petrie(II) found Delta m=0.48. Star is brightest component of A.D.S. 13405: companions are 9.7m at 0.9" and 14.6m at 5.4". System1206Orbit1End System1207Orbit1Begin Balmer emission lines are sometimes observed during primary eclipse, when the secondary spectrum is also visible. The circumstellar structure that produces these emissions also affects the light-curve (D.S. Hall and L.M. Garrison, Publ. Astron. Soc. Pacific, 84, 552, 1972) making its solution difficult. D.S. Hall et al. (Acta Astron., 29, 653, 1979) have also published new photoelectric and spectroscopic observations, but Struve's remains the only orbital determination. Other photoelectric observations were published by K. Walter (Astron. Astrophys. Supp., 13, 249, 1971) and were re-analyzed by M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 265, 1980) who found an orbital inclination of 87 deg and a fractional luminosity for the primary component of 0.8 (in yellow light). The period is increasing. System1207Orbit1End System1208Orbit1Begin Lucy & Sweeney derive similar elements but find a larger eccentricity (0.20). B.S. Whitney (Astrophys. J., 102, 202, 1945 and 108, 519, 1948) has analyzed photographic and visual light-curves and finds i=90 deg and a photographic light-ratio of about 0.6. Light-curves from different wavelength regions are not in full accord, however, and some modern photometry seems desirable. A partial rediscussion of the existing photometric observations has been published by G. Giuricin and F. Mardirossian (Astrophys. Space Sci., 76, 111, 1981). System1208Orbit1End System1209Orbit1Begin Lucy & Sweeney find e=0.07. System1209Orbit1End System1210Orbit1Begin Although the binary nature of this star was discovered by J.S. Plaskett and J.A. Pearce (Publ. Dom. Astrophys. Obs., 5, 1, 1935), these are the first elements to be determined. The orbit is assumed circular, since a preliminary solution showed the eccentricity not to be significant, and the epoch is the time of inferior conjunction of the primary component. The fairly large difference in the values of V0 for the two components is probably a consequence of the small number of measures of the secondary spectrum. Gies and Bolton estimate Delta m=1.12. The star is the brightest component of A.D.S. 13429: companions are 8.6m at 5.7" and 10.1m at 27.9". The brighter of these is H.D. 191566 and has a constant radial velocity close to the systemic velocity of the spectroscopic pair. System1210Orbit1End System1211Orbit1Begin Earlier investigations were made by R.H. Baker (Publ. Allegheny Obs., 2, 41, 1910); W.E. Harper (J. Roy. Astron. Soc. Can., 6, 265, 1912); and W.J. Luyten, O. Struve and W.W. Morgan (Publ. Yerkes Obs., 7, pt. IV, 1939). All these investigators found smaller values of K1 than that given in the Catalogue. This may be partly due to their inability to resolve the secondary spectrum completely. Cesco and Struve found that variations in the relative intensities of the two spectra, observed even on their high-dispersion spectrograms, could be interpreted as a blending effect. Petrie(I) found Delta m=1.26. A 13.0m companion is listed in I.D.S. at 113.7". System1211Orbit1End System1212Orbit1Begin Epoch is T0.circular orbit assumed. Original observations were made by W.E. Harper (Publ. Dom. Obs., 4, 199, 1918). Luyten's recomputation is preferred because Harper fixed the value of T. He later revised the period to 9.314d (Publ. Dom. Astrophys. Obs., 6, 246, 1935). System1212Orbit1End System1213Orbit1Begin These orbital elements supersede those published by D.P. Hube (J. Roy. Astron. Soc. Can., 70, 27, 1975) which were based on an incorrect value for the period. The new period removes the apparent evidence for variations in V0. The orbit should probably be regarded as circular, and the epoch given is T0. System1213Orbit1End System1214Orbit1Begin Epoch is time of primary minimum. All elements are estimated; a circular orbit would fit the observations nearly as well. Double emission lines are observed in the spectrum. The value of K2 is given by Popper in Astrophys. J., 141, 314, 1965. Popper also adopted there m1=5 MSol, m2=0.9 MSol and Delta m(bolometric)=0.3. The inclination, deduced from Popper's photometric observations, is about 86 deg. A Keplerian velocity-curve cannot represent all the observations. System1214Orbit1End System1215Orbit1Begin The work by Wright supersedes earlier determinations by W.H. Christie (Astrophys. J., 83, 433, 1936) and J.M. Vinter-Hansen (Astrophys. J., 100, 8, 1944). A. McKellar and R.M. Petrie (Publ. Dom. Astrophys. Obs., 11, 1, 1957) published a thorough discussion of the system and first suggested a period of around 3780d instead of the previously accepted value of just over 3800 d. The later spectroscopic and photometric observations have confirmed this value. The orbital elements of the primary component are now well-determined, although the difference between Wright's value for e and that found by Vinter-Hansen (0.131) is worrying and unexplained. Velocities of the secondary component are determined from intensity tracings after subtraction. Therefore K2 is correspondingly uncertain, and the difference between the values of V0 obtained for the two components is probably of no significance. Many photometric observations have been made, but analysis of this kind of system (with an extended atmosphere) is difficult and has not been fully satisfactorily achieved. The depth of eclipse in visible light is about 0.1m. The inclination is close to 90 deg ; A. Ollongren (Bull. Astron. Inst. Netherl., 12, 313, 1956) gives 88.8 deg. His solution included `third light' but led to the result that the B star gives 0.74 of the stellar light at lambda 3700. Wright deduces Delta mV=1.4. Observations in the ultraviolet (with IUE) are reported by R.E. Stencel, Y. Kondo, A.P. Bernat and G.McCluskey (I.A.U. Symp. No. 88, p. 555, 1980), A. Che, K. Hempe and D. Reimers (Astron. Astrophys., 126, 225, 1983) and K.-P. Schroder (ibid., 170, 70, 1986). Che et al. discuss the rate of mass loss, and Schroder derives a model for the density of the inner chromosphere. R.E. Stencel et al. (Astrophys. J., 281, 751, 1984) have published detailed photometric and spectroscopic observations of the 1982 eclipse. From measurements of four eclipses, they suggest that the period is 3794.34d +/-0.12d. The system is an X-ray source -- and a much stronger one than zeta Aur (G.E. McCluskey and Y. Kondo, Publ. Astron. Soc. Pacific, 96, 817, 1984). The star is the brightest member of A.D.S. 13554: several companions are listed in I.D.S. System1215Orbit1End System1216Orbit1Begin The new orbital elements supersede the earlier work by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 201, 1924 and 6, 247, 1935) and recomputations, by Luyten and by Lucy & Sweeney, that were based upon it. The orbit was assumed circular after a preliminary solution showed the eccentricity not to be significant: the epoch is T0. Observations with IUE reveal the secondary spectrum to be approximately B9, but with some enhanced absorptions; they have also shown the star to be an eclipsing binary of the zeta Aur type. The depth of the eclipse is less than 0.1m in V. At visual wavelengths, the secondary component is probably about three magnitudes fainter than the primary. System1216Orbit1End System1217Orbit1Begin The velocity-curve is apparently based on the Ca II lines alone; the velocities from the other lines show much more scatter. Balmer emission is seen during primary eclipse and Struve suspected real changes in the velocity-curve from day to day. The only available photoelectric (UBV) light-curve was published by M. Ammann, D.S. Hall and R.C. Tate (Acta Astron., 29, 259, 1979). It shows asymmetries consistent with the presence of circumstellar matter. The period is also variable (D.S. Hall and K.S. Woolley, Publ. Astron. Soc. Pacific, 85, 618, 1973). Ammann et al. find an orbital inclination close to 88 deg and a fractional luminosity (in V) of 0.81 for the primary star. System1217Orbit1End System1218Orbit1Begin Wright's observations supersede the original discussion by J.B. Cannon (Publ. Dom. Obs., 4, 151, 1918) and his own earlier work (Publ. Dom. Astrophys. Obs., 9, 189, 1952). A spectroscopic study by P. Wellmann (Astrophys. J., 126, 30, 1957) and results obtained by E.B. Weston (Astron. J., 58, 233, 1953) suggested that the period should be increased from the value of 1140.8d adopted by Wright in his first paper. Wright finds Delta m v=2.5. Photometric analysis of the shallow eclipses (depth 0.2m) is complicated, as in the case of 31 Cyg, by the extensive atmosphere of the supergiant component, and by intrinsic variations in the light of that star. Several investigators deduce a likely value for i of around 80 deg. A. Galatola (Astrophys. J., 175, 809, 1972) derives i=82 deg by a method which takes account of the extended atmosphere. A new analysis of the light-curve at the 1971 and 1974 eclipses, has been published by E.F. Guinan and G.P. McCook (Publ. Astron. Soc. Pacific, 91, 343, 1979) which leads to a lower value (about 74 deg) for the inclination and estimates of 0.93 and 0.98 for the fractional luminosity of the cool component at lambda lambda 4870 and 6575 respectively. Details of some spectrograms obtained at the 1981 eclipse have been published by Tan Hui-Song and Peng Song-Chuan (Acta Astrophys. Sinica, 25, 56, 1984). Several of the papers cited for 31 Cyg, especially those by Che et al., Schroder, and Stencel et al. (1980). A 9.7m companion at 208.9" is listed in I.D.S. System1218Orbit1End System1219Orbit1Begin Although the spectrum of this star was long recognized to display absorption lines typical of an OB spectrum, as well as the emission lines of a W-R star, the binary nature of the system remained uncertain because of the small range of velocity variation. Indeed, P. Massey suggested (Astrophys. J., 236, 526, 1980 and I.A.U. Symp. No. 88, p. 187, 1980) that emission and absorption lines arise from the same stellar atmosphere. Lamontagne et al. have been able to find a period in velocity measurements made on the emission line of N IV at lambda 4058, although the period is not unique. In particular a period of 0.39d is possible, however unlikely it may seem on physical grounds. Circular and elliptical orbital solutions were made from the data, and the former was adopted when the eccentricity of 0.19 was found not to be significant. Very different values of V0 are derived from different lines. The epoch is the time of inferior conjunction of the W-R star. Like Massey, Lamontagne et al. could not find a periodicity in the velocities derived from the rotationally very broadened absorption lines. They suggest that the companion in the 2.3d orbit is a neutron star and the close pair has an OB companion. They tentatively suggest an orbital period of 1763 d for this, but the triple nature of the system remains speculative. The star is the brighter member of A.D.S. 13641: companion is 12.1m at 4.4". System1219Orbit1End System1220Orbit1Begin The earliest investigation of this system is by W.A. Hiltner who classified the secondary spectrum as that of a Wolf-Rayet star. Later observations were published by A.B. Hart (Astrophys. J., 126, 463, 1957). Massey and Conti reclassify the secondary spectrum as that of an Of star. The difficulties of interpretation usual in systems of this kind are encountered. Emission lines and absorption lines in the secondary-spectrum give different values of K2 and V0. The Catalogue gives the values for the absorption-line O-type spectrum on the top line, and for the absorption lines in the Of spectrum on the bottom line. It remains unclear whether the velocity shifts of these lines or of the emission lines represent more nearly the true motion of the secondary star. It seems very probable that a stellar wind is affecting, to some extent, the velocities measured from all lines. The epoch appears to be the time of superior conjunction of the O7.5 star. System1220Orbit1End System1221Orbit1Begin Older observations depart a little from Osawa's velocity-curve, and there may have been some changes in the elements. New observations by S.B. Parsons (Astrophys. J. Supp., 53, 553, 1983) suggest a slightly longer period (2452.6d) but otherwise require no change to the elements. System1221Orbit1End System1222Orbit1Begin While no new complete orbital analysis has been published, D.M. Popper (Astrophys. J., 220, L11, 1978) has made known his conclusion that Pearce's values for the semi-amplitudes are too high, and that the system is therefore significantly less massive than it has been believed to be. Popper's values of K1 and K2, 255 km/s and 360 km/s respectively, probably should be used until a full orbital study is published. Popper also estimated a spectral type of O7 for the primary and remarked that there is no obvious difference of type between the components. Results of IUE observations are presented by R.H. Koch, M.J. Siah and N. Fanelli (Publ. Astron. Soc. Pacific, 91, 474, 1979), who also comment on the variable period. Photoelectric observations have been published by A.U. Landolt (Astrophys. J., 140, 1494, 1964 and Publ. Astron. Soc. Pacific, 87, 409, 1975). The latter set of observations has been re-analyzed by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978), who found an orbital inclination close to 84 deg and a fractional luminosity (in V) for the primary star of 0.58. An 11.4m companion at 11.4" is listed in I.D.S. System1222Orbit1End System1223Orbit1Begin Earlier studies of this triple system were published by P.W. Merrill (Lick Obs. Bull., 6, 6, 1910), H. Spencer Jones (Cape Annals, 10, pt. 8, 76, 1928) and -- the previous best -- R.F. Sanford (Astrophys. J., 89, 333, 1939). The work of Evans and Fekel provides a beautiful example of the power of occultation observations, in favourable circumstances, confirms Sanford's work, and represents a considerable improvement on it for the short-period binary. The long-period orbit, that of the K giant and the spectroscopic pair, is determined from both spectroscopic and occultation (and one speckle) observations. Therefore, the orbital inclination is known (84 deg) and the parallax can be accurately determined (0.0104"). The value of V0 for the short-period pair is variable. Since the masses and beta luminosities are well known, Evans and Fekel discuss the evolutionary status of the components. Two distant companions to the triple system are listed in I.D.S.: 6.2m at 205.3" and 9.0m at 226.6". System1223Orbit1End System1224Orbit1Begin Earlier studies of this triple system were published by P.W. Merrill (Lick Obs. Bull., 6, 6, 1910), H. Spencer Jones (Cape Annals, 10, pt. 8, 76, 1928) and -- the previous best -- R.F. Sanford (Astrophys. J., 89, 333, 1939). The work of Evans and Fekel provides a beautiful example of the power of occultation observations, in favourable circumstances, confirms Sanford's work, and represents a considerable improvement on it for the short-period binary. The long-period orbit, that of the K giant and the spectroscopic pair, is determined from both spectroscopic and occultation (and one speckle) observations. Therefore, the orbital inclination is known (84 deg) and the parallax can be accurately determined (0.0104"). The value of V0 for the short-period pair is variable. Since the masses and luminosities are well known, Evans and Fekel discuss the evolutionary status of the components. Two distant companions to the triple system are listed in I.D.S.: 6.2m at 205.3" and 9.0m at 226.6". System1224Orbit1End System1226Orbit1Begin Original observations made by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 4, 103, 1928). Luyten's recomputation is preferred because Plaskett fixed the value of T in his solution. The epoch is T0. Petrie(II) found Delta m=0.60. System1226Orbit1End System1227Orbit1Begin Pearce derived an orbital inclination of 64 deg from the mass-luminosity relation and predicted that eclipses would be found. Observations by S. Gaposchkin (Peremm. Zvezdy, 7, 38, 1949) and N.L. Magalashvili and Ya.I. Kumsishvili (Bulletin Abastumani Obs., No. 34, 3, 1966) appeared to confirm the prediction. E.G. Ebbighausen et al. (Publ. Astron. Soc. Pacific, 87, 923, 1975) suggested, however that the star is an ellipsoidal variable, with a range of light less than 0.1m. This has been confirmed by the analysis of their observations by G. Russo, L. Milano and C. Maceroni (Astron. Astrophys., 109, 368, 1982). They find an inclination of 50 deg and a fractional luminosity (in V) for the hotter component of 0.48. System1227Orbit1End System1228Orbit1Begin Although there has been much debate in the literature about V444 Cyg, rather surprisingly Munch's orbital elements remain the best ones determined. Earlier ones were given by O.C. Wilson (Astrophys. J., 91, 379, 1940) and E.S. Keeping (Publ. Dom. Astrophys. Obs., 7, 349, 1947) while a more recent set was published by K.S. Ganesh, M.K.V. Bappu and V. Natarajan et al. (Kodaikanal Bull. Series A, No. 184, 1967). The epoch is T0 for the star that has the O or B absorption spectrum (whose elements are given on the lower line); the orbit was assumed circular. All investigators agree that the value of K1 (W-R component) is close to 300 km/s, but estimates of K2 vary much more widely. Munch and Wilson are in agreement. Ganesh et al. find line-to-line differences for each of K1 and K2 -- but their spectrograms are of low dispersion. The value of V0 is, as often in W-R binaries, dependent on the lines measured; Munch gives +70 km/s, 40 km/s and +10 km/s for the N V emission, N IV emission and the absorption lines respectively. Despite the photometric work of A.M. Cherepashchuk (Peremm. Zvezdy, 16, 226, 1967) the discussion by G.E. Kron and K.C. Gordon (Astrophys. J., 97, 311, 1942 and 111, 454, 1950) is probably still the best. They found an inclination of 78 deg (confirmed by Cherepashchuk et al., see below) and a fractional luminosity of 0.83 for the star with the absorption spectrum. Their model of an extended atmosphere or disk surrounding the W-R star remains basic to most modern interpretations. Modern ultraviolet photometric observations have been published by A.M. Cherepashchuk, J.A. Eaton and Kh.F. Khaliullin (Astrophys. J., 281, 774, 1984). Their model was criticized by A.B. Underhill and R.P. Fahey (ibid., 313, 358, 1987). Infrared photometry has been published by L. Hartmann (ibid., 221, 193, 1978). V.G. Kornilov and A.M. Cherepashchuk (Pis. Astron. Zh., 5, 398, 1979) find a variable period that cannot be explained by a third body in the system; they discuss the rate of mass-loss from the W-R star. Variable polarization has been reported by O.S. Shulov (Astron. Tsirk. Kazan, No. 385, 5, 1966) and Yu.S. Efimov (Izv. Krym. Astrofiz. Obs., 37, 251, 1967). An attempt to detect radio emission from the star was unsuccessful (D.R. Florkowski and S.T. Gottesman, Inf. Bull. Var. Stars, No. 1101, 1976) System1228Orbit1End System1229Orbit1Begin This star is now recognized as belonging, or at least as related, to the class of cataclysmic variables. The light-curve shows that eclipses are superimposed on the irregular nova-like variations. The epoch is the time of primary minimum. The spectrum cannot be classified easily, but resembles that of a WN star. The fluorescent emission lines of O III are double. The brighter component of the system appears to be the less massive. R.H. Koch, M.J. Siah and M.N. Fanelli (I.A.U. Colloq. No. 53, p. 448, 1980) describe the IUE spectrum and find the period decreasing. R.H. Koch et al. (Astrophys. J., 306, 618, 1986) discuss the IUE spectra and the photometric observations more thoroughly, and offer three models. They find velocities measured from IUE spectra are much more positive than any measured from the ground. They suggest that the companion is a neutron star embedded in an accretion disk. G.A. Williams et al. (Mon. Not. Roy. Astron. Soc., 219, 809, 1986) published the results of photometric and spectroscopic observations during eclipse. They find evidence for a high-velocity wind and for the kind of rotational disturbance typical of cataclysmic variables. Herbig et al. note a 14.4m companion at 9.3", which is not listed in I.D.S. System1229Orbit1End System1230Orbit1Begin Although there has been no full orbital study since McDonald's work, D.M. Popper (Astrophys. J., 220, L11, 1978) states that the masses appear to require little revision. He prefers a spectral classification of O9.5 V to that of B0 V. The orbit should probably be taken as circular. Photoelectric observations have been published by C. Sezer et al. (Astron. Astrophys. Supp., 53, 363, 1983) and D.M. Popper and P.J. Dumont (Astron. J., 82, 216, 1977). The former find an orbital inclination of 78 deg and a fractional luminosity (in both B and V) of 0.54. The observations by Popper and Dumont were analyzed by D.M. Popper and P.B. Etzel (Astron. J., 86, 102, 1981) who pointed out the difficulty of deriving the ratio of the radii. Nevertheless their results (78 deg and 0.5) were similar. The system has also been discussed photometrically by M. Kitamura and Y. Nakamura (Ann. Tokyo Obs., 21, 229, 1986). The star is the brighter component of A.D.S. 13711: companion is 14.5m at 3.3". System1230Orbit1End System1231Orbit1Begin The epoch is the time of primary minimum; the orbit is assumed circular, an assumption in accordance with the light-curve. According to Popper, the metallic-line characteristics of the spectrum are well developed: the K line gives A7, the hydrogen lines F2. Several photometric observations and analyses have been reported: R.M. Williamon (Astron. J., 80, 976, 1975) re-analyzed by G. Giuricin, F. Mardirossian and M. Mezzetti (Astron. Astrophys. Supp., 39, 255, 1980), J. Tremko, J. Papousek and M. Vetesnik (Bull. Astron. Inst. Csl, 27, 125, 1976) and D.M. Popper and P.J. Dumont (Astron. J., 82, 216, 1977 -- analyzed by D.M. Popper and P.B. Etzel, ibid., 86, 102, 1981). All agree that the orbital inclination lies between 88 deg and 89 deg and the fractional luminosity (in V) of the brighter star lies in the range 0.51 to 0.55. System1231Orbit1End System1232Orbit1Begin Orbital elements based on a period of 1085 days were published by R. Lamontagne and A.F.J. Moffat (Astrophys. J., 277, 258, 1984) and criticized by P.S. Conti et al. (ibid., 282, 693, 1984) who made the unlikely suggestion that the two spectra arose from two stars in the same line of sight. The present elements, based on the period 7.9y+/-0.2y, are derived from heterogeneous observations over a long period of time. Velocities of the O-type star were derived from measures of the Balmer absorption-lines and those of the W-R component from measures of the C IV emission line at lambda 4650. These latter, especially, show a large scatter. The value of K on the upper line of the Catalogue refers to the O-type star. The attractive feature of this long-period, eccentric orbit is that the time of periastron passage is close to the times at which infrared outbursts of the star occur. System1232Orbit1End System1233Orbit1Begin Curchod and Hauck give the spectral types as A3 and F2, from the K line and metallic lines, respectively. Hube estimates A5 from the hydrogen lines. No secondary spectrum is visible. System1233Orbit1End System1234Orbit1Begin The epoch is T0. The original observations were by H.D. Curtis (Lick Obs. Bull., 4, 154, 1907). Luyten's solution is preferred because that by Curtis was graphical. Lucy & Sweeney, like Luyten, adopt a circular orbit. Two companions are listed in I.D.S.: B is 9.2m at 245.4" and C is 10.5m at 17.2" from B. System1234Orbit1End System1235Orbit1Begin Although new observations have been published by K.S. Ganesh and M.K.V. Bappu (Kodaikanal Bull. Series A, No. 185, 1968) Hiltner's orbital elements are retained because they are based on more spectrograms. Ganesh and Bappu have brought out more clearly than Hiltner did the differences between the various lines: for example there is a phase shift between the velocities derived from the line lambda 4058 N IV and those from the line lambda 4686 He II. Different values of V0 are required by lambda lambda 4686, 4058, and 4603 (N V). This was also found by Hiltner; the value given in the Catalogue is for lambda 4686 and agrees well with the value found from the same line by Ganesh and Bappu. On the other hand, the two values of K differ by 17 km/s (Ganesh and Bappu give K=147 km/s). In view of the uncertainties of measurement of this kind of spectrum, especially at the low dispersions employed, the disagreement is probably not very important. The epoch is an estimate of T0 made from Hiltner's data. Ganesh and Bappu give a zero phase of 2,434,719.77 which is the time at which the velocity derived from lambda 4686 equals the systemic velocity on the descending branch of the curve. They also differ from Hiltner in finding an appreciable eccentricity (e=0.12, omega=51 deg). Absorption lines of He I vary in phase with the emission lines, according to Hiltner, but with a large negative mean velocity. He attributes them to an expanding envelope surrounding the Wolf-Rayet star. System1235Orbit1End System1236Orbit1Begin This hitherto neglected bright spectroscopic binary has recently been the subject of two independent investigations. The other is by D.W. Willmarth (Publ. Astron. Soc. Pacific, 88, 86, 1976). He found almost the same orbital period as Hube did but his solution differed in some respects. Willmarth assumed a circular orbit and found K1=53.8 km/s and V0=1.1 km/s. Only the difference in K1 is at all important, but until it is resolved the elements can hardly be considered well determined. Hube had the greater number of observations, most of them at a higher dispersion than Willmarth's, and his solution is preferred. Hube also noted a systematic departure from the velocity curve about the expected time of conjunction of the two stars and pointed out that an eclipse might be observable. One was observed at the expected phase, apparently also independently, by W. Furtig (Inf. Bull. Var. Stars, No. 1071, 1975). A variation in brightness of at least 0.15m was found, but a complete light-curve has not yet been published. System1236Orbit1End System1237Orbit1Begin System1237Orbit1End System1238Orbit1Begin System1238Orbit1End System1239Orbit1Begin The minimum of the velocity-curve is not well defined. Bopp et al. state that the observations can be fitted to a pure sine curve of half the period -- but poorly. System1239Orbit1End System1240Orbit1Begin The orbit of this cataclysmic variable is assumed circular. The epoch is the time of superior conjunction of the emission-line source. System1240Orbit1End System1241Orbit1Begin The velocity-curve is well covered but the scatter of observations is rather large. Very similar elements are derived from these observations by Lucy & Sweeney. Reference: G.A.Shajn, Pulkovo Circ.,, No. 26-27; 75, 1939 System1241Orbit1End System1242Orbit1Begin The spectrum has been reported as showing double lines which were not fully resolved (W.W. Campbell and S. Albrecht, Lick Obs. Bull., 5, 174, 1910). This report was not confirmed by Abt, who found the lines broad but not double. He concluded that the secondary component is not visible. Abt classified the spectrum as A6, A8 and F5 IV from the K line, the hydrogen lines and the metallic lines, respectively. System1242Orbit1End System1243Orbit1Begin The observations by Bohannan and Conti supersede the lower-dispersion ones by O.C. Wilson and H.A. Abt (Astrophys. J., 114, 477, 1951). Both components display emission at lambda 4686, the stronger emission being associated with the O6 component. The coverage of the velocity-curve is poor, but there is little doubt that the elements derived by Bohannan and Conti are the more trustworthy, especially as they remove an apparent contradiction to the probable membership of the system in Cyg OB2. A circular orbit is assumed and the epoch is the time of primary minimum as found by D.S. Hall (Acta Astron., 24, 69, 1974) from his own UBV observations. J.-M. Vreux (Astron. Astrophys., 143, 209, 1985) has published a study of the variations in the structure of the H-alpha emission line. Hall's photometric observations have been re-analyzed by K.-C. Leung and D.P. Schneider (Astrophys. J., 224, 565, 1978) who find that the system is an early-type contact system with an orbital inclination of 68 deg and a fractional luminosity (in V) for the more massive star of 0.88. Hall noted a faint companion at 1.5" from the system. System1243Orbit1End System1244Orbit1Begin The K line shows a smaller amplitude because it is blended with an interstellar line. Lucy & Sweeney derive very similar elements from these observations. System1244Orbit1End System1245Orbit1Begin Imbert estimates the spectral type of the (invisible) secondary to be not much later than K5 V and he suggests that the system may display eclipses. These elements are confirmed by D.W. Latham et al. (Astron. J., 96, 567, 1988). System1245Orbit1End System1246Orbit1Begin The observations show systematic residuals from the velocity-curve, and there is some evidence of changes in the spectrum. Note the high eccentricity. System1246Orbit1End System1247Orbit1Begin These elements supersede those derived earlier by Shajn (Pulkovo Obs. Circ., No. 1, 17, 1932). Reference: G.A.Shajn, Pulkovo Circ.,, No. 8; 16, 1934 System1247Orbit1End System1248Orbit1Begin The period of 26.65y was assumed from the visual orbit computed by P. Couteau (J. Observateurs, 45, 39, 1962). The other elements were computed from new observations by Abt and Levy and those previously published by A.B. Underhill (Publ. Dom. Astrophys. Obs., 12, 159, 1963). The values of T, e, and omega differ from those found from the visual orbit and are, as Abt and Levy point out, uncertain because the velocity minimum has not yet been covered. The major semi-axis of the orbital pair is 0.475" and the inclination 63.6 deg. The components of the orbital pair (A.D.S. 14073) differ in brightness by about a magnitude. Three other companions listed in I.D.S. are considered optical by Abt and Levy. The earliest radial-velocity study of this system was by Y.C. Chang (Astrophys. J., 68, 319, 1928). System1248Orbit1End System1249Orbit1Begin These elements supersede those derived earlier by Harper (Publ. Dom. Astrophys. Obs., 1, 153, 1919) which were based on an incorrect value of the period. System1249Orbit1End System1250Orbit1Begin The secondary spectrum is seen in eclipse and was classified G5 by Struve. The solution of the light-curve requires the secondary to be a subgiant. Lucy & Sweeney confirm the orbital eccentricity, but the B, V light-curves by K. Walter (Astron. Nachr., 292, 145, 1970) indicate e cos omega=0. The light-curve shows evidence of gas streams, and its solution is correspondingly uncertain. Walter finds i=84 deg and that the fractional luminosity of the brighter star (in V) is 0.86. M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 273, 1980) obtained similar results from Walter's observations. A periodic effect in the residuals of times of minima may be caused by apsidal rotation in about 51y (M. Plavec, Bull. Astron. Inst. Csl, 11, 148, 1960). System1250Orbit1End System1251Orbit1Begin Harper (Publ. Dom. Astrophys. Obs., 6, 249, 1935) later revised the period to 205.2d. Lucy & Sweeney, adopting this new period, obtained very similar values for K1, V0 and a slightly larger value for e(0.138). The star is the brighter component of A.D.S. 14081: B is 11.0m at 32.0". System1251Orbit1End System1252Orbit1Begin The epoch is T0 for the primary component. From his photoelectric observations, M.W. Ovenden (Mon. Not. Roy. Astron. Soc., 114, 569, 1954) deduced that the values of the masses derived by Pearce might be seriously affected by the reflection effect. D.M. Popper (Astrophys. J. Supp., 3, 107, 1957) questioned whether the secondary spectrum is visible at all. Light-curves in B and V have been published by G. Mannino (Mem. Soc. Astron. Ital., 34, 191, 1963). The magnitudes given in the Catalogue are derived from his data but are subject to a zero-point error since he gave only an approximate magnitude for his comparison star. He derived i=63 deg and the fractional luminosity of the brighter star (in V) as 0.68. System1252Orbit1End System1253Orbit1Begin The value of K2 depends on only a few observations. The value of V0 is variable. This spectroscopic binary is the brighter component of a visual binary, Kuiper 99, with an orbital period of 39.4y and a major semi-axis of 0.8". The visual secondary is about 1 m fainter than the primary and probably of early M spectral type. Duquennoy finds that the two orbital planes are mutually nearly perpendicular. There are problems reconciling the two orbits with the mass-luminosity relation. Duquennoy derives values K=3.2 km/s, V0=40.9 km/s, for the velocity variation of the centre of mass of the close pair about that of the visual system; but they are based on observations at only three epochs covering about a quarter of the long-period orbit. System1253Orbit1End System1254Orbit1Begin The first orbital elements were determined by A.H. Joy (Astrophys. J., 120, 377, 1954) who derived a period of 0.7d. New observations by M.F. Walker (Sky Telesc., 29, 23, 1965) suggested a shorter period, and C. Payne-Gaposchkin (Astrophys. J., 158, 429, 1969) showed that Joy's observations were satisfied by a circular orbit with a period of 0.4116550d. Chincarini and Walker have improved the orbital elements for the absorption-line component (which they confirm to be K5 V as first suggested by J.A. Crawford and R.P. Kraft, Astrophys. J., 123, 44, 1956), given on the upper line. The V magnitude is an approximate average; there are fluctuations of up to two magnitudes in the brightness of the object. The epoch is the time of superior conjunction of the K-type star. The orbit should probably be regarded as circular, but measures of the emission lines (H, He I, Ca II) require e=0.16, omega=235 deg, V0=32 km/s. Thus the true value of K2 (derived from the emission lines) remains uncertain. The ultraviolet spectrum, as observed with IUE, is described by R.F. Jameson, A.R. King and M.R. Sherrington (Mon. Not. Roy. Astron. Soc., 191, 559, 1980). J. Patterson (Astrophys. J., 234, 978, 1979) has found a period of just over 33s in the light-variation of this star, which he explains with a model of an accreting magnetic white dwarf. System1254Orbit1End System1255Orbit1Begin The star has 9.8m companion at 48.3". System1255Orbit1End System1256Orbit1Begin Orbital elements were first published for this ex-nova (Nova Del 1967) by J.B. Hutchings (Astrophys. J., 232, 176, 1979) who found two possible periods near 0.17d and a third at 0.225d. The period found by Bruch appears to satisfy all the data. The orbit is assumed circular and the epoch is T0. The values given for K1 and V0 are derived from measures of the He II emission line at lambda 4686. The emission at H-beta gives 34 km/s and 15 km/s, respectively. The magnitude given is an approximate mean magnitude since the end of the outburst -- there is not much variation. Both Bruch and Hutchings estimate that the orbital inclination is just over 40 deg. System1256Orbit1End System1257Orbit1Begin Earlier studies of this system were published by K. Bracher (Publ. Astron. Soc. Pacific, 91, 827, 1980) and A.F.J. Moffat and W. Seggewiss (Astron. Astrophys., 86, 87, 1980). The observations by Drissen et al. permit a refinement of the period and this is the chief reason that their results are preferred. The elements given are derived from measures of the emission line of N IV at lambda 4058. Different values are obtained from measures of He II lambda 4686. Measures of the phase-dependent polarization of this star's light permit determination of the inclination of the orbital plane as approximately 67 deg. The star has an unusually high galactic latitude, for a W-R star, and is a runaway star. Similarities of the system with H.D. 226868 lead the authors to postulate that the unseen secondary component is a black hole. System1257Orbit1End System1258Orbit1Begin The epoch is T0 and the orbit is assumed circular. The period is variable. L. Binnendijk (Publ. Dom. Astrophys. Obs., 13, 27, 1967) published elements based on observations by R.M. Petrie, giving V0=10 km/s, K1=90 km/s and K2=220 km/s. New observations measured by the cross-correlation method, by G. Hill and D. Holmgren, are in press (Astron. Astrophys., 1989). Recent solutions of the light-curve have been published by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978 and Astron. Astrophys. Supp., 58, 261, 1984 -- based on new observations) and C. Cristescu, G. Oprescu and M.S. Suran (Inf. Bull. Var. Stars, No. 1686, 1979 -- also partly based on new observations). The orbital inclination appears to be close to 65 deg and the fractional luminosity (in V) of the brighter star is about 0.9. A long discussion of the light-curve was also published by I. Pustylnik and L. Sorgesepp (Publ. Tartu Astrophys. Obs., 43, 130, 1975) while I.B. Pustylnik and H. Einasto (Astrophys. Space Sci., 105, 259, 1984) use the system to illustrate their model of a binary immersed in a single gaseous envelope. Astrometric observations have revealed a visual companion, 2.7m fainter than the eclipsing pair, with an orbital period of 30.45y (J.L. Hershey, Astron. J., 80, 662, 1975). Hershey estimates masses of 1.1 MSol, 0.4 MSol (eclipsing pair) and 0.58 MSol (visual secondary). Light-time in the long-period orbit cannot account for all the observed variations of the short period. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System1258Orbit1End System1259Orbit1Begin The values of K2, and hence of the masses, are rather uncertain. System1259Orbit1End System1260Orbit1Begin The spectral type may be slightly earlier than K2 III, but certainly no earlier than K0 III. System1260Orbit1End System1261Orbit1Begin The epoch is T0 and the orbit is assumed circular. Earlier investigations were published by W.H. Christie (Astrophys. J., 78, 200, 1933), who believed there was a long-period variation (12.3y) not subsequently confirmed, and by H.A. Abt (Publ. Astron. Soc. Pacific, 66, 171, 1954). The spectrum is difficult to interpret because it contains shell lines as well as stellar lines (A.B. Underhill, Publ. Astron. Soc. Pacific, 66, 334, 1954) -- which may account for Abt's small value of K1. C. Aydin, M. Hack and N. Yilmaz (Astrophys. Space Sci., 53, 345, 1978) classify the shell as A9 Ia and the star as A5 I. They also obtained orbital elements that confirm Heiser's values, and were derived -- as his were -- from measures of the Mg II line at lambda 4481. Even this line has a shell component, however. They find evidence for stratification in the shell and, sometimes, for prominence-like eruptions. The ultraviolet spectrum is discussed by M. Hack, S. Engin and N. Yilmaz (Astron. Astrophys., 131, 147, 1984). They find that the secondary star is hotter than the primary and conclude that primary eclipse is caused by a cooler disk surrounding the secondary. Emission at H-gamma is discussed by P.M. Afanas'eva and V.L. Gorshkov (Astron. Tsirk., No. 1284, 1983). Apart from Heiser's own photometric observations (Astrophys. J., 135, 78, 1962), light-curves have been published and discussed by A. Fresa (Mem. Soc. Astron. Ital., 37, 607, 1966) and P. Kalv and I. Pustylnik (Publ. Tartu Astrophys. Obs., 43, 114, 1975). These have all been re-analyzed by Yan-Feng Li and Kam-Ching Leung (Astrophys. J., 313, 801, 1987) who find an orbital inclination close to 77 deg and a fractional luminosity for the primary (in V) of 0.71. They suggest that the system is an evolved early-type contact system. The interpretation of this complex binary remains uncertain. The star is the brightest member of A.D.S. 14314: B is of equal brightness at 0.1m, C is 13.7m at 2.3". System1261Orbit1End System1262Orbit1Begin The star's light has been suspected of variability. Reference: G.Shajn, Pulkovo Circ.,, No. 7; 16, 1933 System1262Orbit1End System1263Orbit1Begin This symbiotic object shows a periodicity of about 950 days in its light variation, which is apparently caused by eclipses. The magnitudes quoted, however, indicate the total range of variation during outbursts. Radial velocities measured from the emission lines show the same periodicity. The orbit is assumed circular and the epoch is the time of primary minimum. System1263Orbit1End System1264Orbit1Begin Abt and Levy offer these elements as improvements over those published by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961). The scatter of observations is still large, however, compared with the total range of variation in velocity. The spectral type is A4, F0 and F5 IV from the K line, hydrogen lines and metallic lines, respectively. System1264Orbit1End System1265Orbit1Begin Lucy & Sweeney adopt a circular orbit. System1265Orbit1End System1266Orbit1Begin Earlier studies of orbital elements have been published by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 213, 1920); R.O. Redman (Publ. Dom. Astrophys. Obs., 4, 341, 1931); and O. Struve et al. (Astrophys. J., 129, 59, 1959). The last named contained only estimates of some of the elements. Vitrichenko has combined 26 new observations with the older material. Apsidal rotation in a period of about 56 years is well established photometrically. Vitrichenko gives omega=90deg+0.06266degE, where E is to be measured from the value of T given in the Catalogue. He also considers the possible variation in V0 suggested by Redman and concludes there is no variation within the errors of observation. Despite the difficulties of measuring this spectrum, the spectroscopic elements now appear to be well determined. N.L. Magalashvili and Ya.I. Kumsishvili (Bulletin Abastumani Obs., No. 24, 13, 1959) find from photoelectric observations that the two stars are precisely equal in size and luminosity and that i=85.5 deg. Similar results are obtained from these observations by G. Giuricin, F. Mardirossian and M. Mezzetti (Astron. Astrophys. Supp., 39, 255, 1980) who give i=86.4 deg and a fractional luminosity at lambda 4200 of 0.54 for the brighter star. Petrie(II) found Delta m=0.07. The depths of eclipses are about 0.6m. System1266Orbit1End System1267Orbit1Begin Since these elements of this close visual pair are derived from radial-velocity observations at only one periastron passage, which showed the previously derived elements of the visual orbit -- including the period -- to be only approximate (P. Muller, J. Observateurs, 38, 58, 1955), they, too, can be only approximate. The spectral types given are inferred from the mean spectral type -- the stars are never resolved on the spectrograph slit since a=0.25". The elements given are not derived in any way from the visual observations, except that those serve to give the approximate period. Griffin estimates Delta m=1.1. The pair is the visual binary A.D.S. 14396. System1267Orbit1End System1268Orbit1Begin Earlier investigations were published by R.H. Baker (Publ. Allegheny Obs., 2, 35, 1910), J.A. Pearce (Publ. Am. Astron. Soc., 9, 268, 1939) and W.J. Luyten et al. (Publ. Yerkes Obs., 7, pt. IV, 31, 1939). The system displays apsidal motion and the value given for omega and T are appropriate for 1972. Hilditch estimates the apsidal period at 203y +/-4y. M.W. Ovenden (Mon. Not. Roy. Astron. Soc., 126, 77, 1963) found evidence for a dependence of K1+K2 on the ionization potential of the lines being measured. Ovenden ascribed this dependence to the reflection effect, but neither Hilditch nor M. Tapia and R.C. Smith (Mon. Not. Roy. Astron. Soc., 189, 551, 1979) could confirm his observations. Elements, similar to those presented here, have also been published by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 36, 241, 1978) but Hilditch's values, based on the more complete investigation of this system, are preferred. Determinations of K2 range from 113 km/s to 126 km/s. This may be primarily due to the blending of the lines of the two components. Hilditch took some pains to avoid this effect by omitting from his orbital solution the results of any measurements that gave a velocity separation of less than 100 km/s. Petrie(I) found Delta m=0.34. System1268Orbit1End System1269Orbit1Begin The spectrum shows component lines arising from a gaseous stream (A.D. Thackeray, Observatory, 85, 206, 1965) and the distorting effect of these on the stellar line profiles has been allowed for. Lucy & Sweeney confirm the orbital eccentricity, but neither photoelectric (BV) light-curves by S. Catalano and M. Rodono (Mem. Soc. Astron. Ital., 39, 617, 1968) nor a photographic one by N. Tashpulatov (Peremm. Zvezdy, 17, 76, 1969) show any appreciable displacement of the secondary minimum. Catalano and Rodono found that the eclipses were not total, as previously believed. They derived i=87.5 deg and the fractional luminosity of the primary star (in V) to be 0.91. Similar results were obtained from the same observations by B. Cester et al. (Astron. Astrophys. Supp., 36, 273, 1979). R.S. Polidan and M. Plavec (Bull. Am. Astron. Soc., 6, 465, 1974) report the detection of emission at H-alpha during primary eclipse. System1269Orbit1End System1270Orbit1Begin If each star has a mass of 2 MSol, the orbital inclination would be 23 deg. System1270Orbit1End System1271Orbit1Begin System1271Orbit1End System1272Orbit1Begin Lucy & Sweeney derive very similar orbital elements from these observations. System1272Orbit1End System1273Orbit1Begin These are approximate elements. A circular orbit was assumed although a small eccentricity may be indicated by the observations. The epoch is the time of primary minimum. A. Okazaki et al. (Publ. Astron. Soc. Pacific, 97, 62, 1985) have published BV observations. They find an orbital inclination of 70 deg and a fractional luminosity (in V) for the primary component of 0.95. They estimate the secondary star to be a K-type subgiant. System1273Orbit1End System1274Orbit1Begin This is a cataclysmic variable. The orbit is assumed circular and the epoch is the time of superior conjunction of the emission-line source. System1274Orbit1End System1275Orbit1Begin The velocity-curve is well covered but the scatter of the observations is large. Nevertheless, further analysis by C.L. Morbey and R.F. Griffin (Astrophys. J., 317, 343, 1987) confirms the period derived by Abt and Levy. The star is the brightest member of A.D.S. 14499. A 6.3m companion has an orbital period of 101.5y (G. Zeller, Ann. Univ. Sternw. Wien, 26, 114, 1965). Another companion, 7.26m at 10.5" has a common proper motion with the orbital pair. A third companion, 12.4m at 75", is listed in I.D.S. System1275Orbit1End System1276Orbit1Begin This is an RS CVn system. The spectral types, necessarily only approximate because of mutual contamination of the component spectra during the partial eclipses, are taken from S.A. Naftilan and E.F. Milone (Astron. J., 84, 1218, 1979). The epoch is the time of minimum as given by E.F. Milone et al. (ibid., 84, 417, 1979). The period is variable. The orbit is assumed circular, in accordance with the light-curve. The elements K1 and V0 are only approximately determined. The value of K2 is inferred from the adopted mass-ratio of 1.0. Naftilan and Milone find an orbital inclination of 82.5 deg. The luminosity-ratio is also close to unity. System1276Orbit1End System1277Orbit1Begin System1277Orbit1End System1278Orbit1Begin Hube estimates that the secondary component is at least 1.5m fainter than the primary and probably of mass about 3 MSol. He also estimates an orbital inclination of around 40 deg. System1278Orbit1End System1279Orbit1Begin System1279Orbit1End System1280Orbit1Begin The magnitude of the star varies irregularly by about 0.1m and the star is both a flare star and a BY Dra variable. The spectral type given is the mean for the two components that appear to differ in luminosity by about 0.6m, near H-alpha (which is seen in emission). The star belongs to a known visual binary for which a provisional orbit has been determined (S.L. Lippincott, Astron. J., 80, 831, 1975) with a major semi-axis of 0.73". The visual secondary is estimated to be some 2m fainter than the spectroscopic pair. System1280Orbit1End System1281Orbit1Begin System1281Orbit1End System1282Orbit1Begin New spectroscopic observations have been published by H.W. Duerbeck et al. (Mitt. Astron. Gesells., 55, 164, 1982), from which values of K1=139.2 km/s and K2=145 km/s have been derived. Few details have been given, however, and we prefer to retain the older investigation. Nevertheless, the agreement between the two is good enough to be encouraging. The orbit should probably be considered circular, as the light-curve would suggest. In addition to photometric observations published by Northcott and Bakos themselves, A. Abrami and B. Cester (Publ. Oss. Trieste, No. 320, 1963) and, more recently, N.M.K. Al Naimiy (Astron. Astrophys. Supp., 43, 85, 1981) have published light-curves and analyses. The last-named points out that the light-curve is variable and distorted and the system (which displays H and K emission in its spectrum) may belong to the RS CVn group. Nevertheless, the various authors agree on an orbital inclination close to 70 deg and a fractional luminosity for the brighter star (in V) of about 0.58 System1282Orbit1End System1283Orbit1Begin The orbit was assumed to be circular after a preliminary solution had shown that e is very small. The epoch is T0. The spectrum is composite but Griffin et al. were unable to measure reliably any features in the A-type spectrum. They estimate Delta m(pv)=1.6. They point out that there is sudegcient probability of observable eclipses to justify a search for them. System1283Orbit1End System1284Orbit1Begin The elements are preliminary and the orbit may be circular. System1284Orbit1End System1285Orbit1Begin The orbit is assumed circular and the epoch is T0. The elements are described as preliminary by Burki and Mayor themselves. System1285Orbit1End System1286Orbit1Begin Lucy & Sweeney derive similar elements from these observations. System1286Orbit1End System1287Orbit1Begin Although the observations are few, the elements seem fairly well defined. System1287Orbit1End System1288Orbit1Begin Orbital elements were first derived for this system by R.K. Young (Publ. Dom. Astrophys. Obs., 1, 319, 1921) but little confidence was placed in them, even by Young himself, because of the large scatter of individual measures despite the relatively good quality of the spectrum. Guthnick (in a series of papers cited by Gieseking and Seggewiss) suggested that both components of the spectroscopic binary might be pulsating variables. Gieseking and Seggewiss have at least partially resolved the the problem by deriving an approximate long-period orbit (V0 for the short-period pair is variable). The elements given for the short-period orbit are not very different from those originally derived by Young and later by Guthnick. The spectrum is said, by Gieseking and Seggewiss, to show enhanced lines of Si II. Only the spectrum of one component is visible. Both orbits are assumed circular and the epochs are T0 for each. C.T. Bolton (Inf. Bull. Var. Stars, No. 1322, 1977) also suspected a 150-day periodicity in a different set of velocity observations. The spectroscopic system is the brightest component of A.D.S. 14682. Component B is 7.8m at 3.4", while fainter components are at 57.7" and 74.1". System1288Orbit1End System1289Orbit1Begin Orbital elements were first derived for this system by R.K. Young (Publ. Dom. Astrophys. Obs., 1, 319, 1921) but little confidence was placed in them, even by Young himself, because of the large scatter of individual measures despite the relatively good quality of the spectrum. Guthnick (in a series of papers cited by Gieseking and Seggewiss) suggested that both components of the spectroscopic binary might be pulsating variables. Gieseking and Seggewiss have at least partially resolved the the problem by deriving an approximate long-period orbit (V0 for the short-period pair is variable). The elements given for the short-period orbit are not very different from those originally derived by Young and later by Guthnick. The spectrum is said, by Gieseking and Seggewiss, to show enhanced lines of Si II. Only the spectrum of one component is visible. Both orbits are assumed circular and the epochs are T0 for each. C.T. Bolton (Inf. Bull. Var. Stars, No. 1322, 1977) also suspected a 150-day periodicity in a different set of velocity observations. The spectroscopic system is the brightest component of A.D.S. 14682. Component B is 7.8m at 3.4", while fainter components are at 57.7" and 74.1". System1289Orbit1End System1290Orbit1Begin This is the binary A.D.S. 14773 whose visual orbit (P=5.7y) has long been known (W.J. Luyten and E.G. Ebbighausen, Publ. Minnesota Obs., 2, No. 1, 1934). There is also a distant companion to the system, discovered by F.G.W. Struve and recognized by him to be optical. A radial-velocity study was published by M.M. Dworetsky, D.M. Popper and D.S. Dearborn (Publ. Astron. Soc. Pacific, 83, 207, 1971) who also combined the spectroscopic and visual observations. Two of these authors subsequently further refined their work (D.M. Popper and M.M. Dworetsky, ibid., 90, 71, 1978). The results of these investigations are in substantial agreement with those of Hans et al., which are preferred here because of the more uniform coverage of the velocity-curve. There is little doubt that the properties of the system are now well known, except for a possible systematic error of a few tenths of a kilometre per second in V0. The origin of the spectral classes given is a bit obscure, since the two stars can never be resolved on the spectrograph slit. A mean class of F7 V is about right. Hans et al. find Delta m=0.1 in the photographic region. The period found by them is 5.7006y and the periastron passage was 1970.07. The orbital inclination is close to 98 deg and the parallax is 0.057". The elements given are derived by solving simultaneously for the visual and spectroscopic elements. The values of K1 and K2 are derived from the published values of K1+K2 and the mass-ratio. System1290Orbit1End System1291Orbit1Begin The orbital elements given here are derived from the same observations as D.J. Stickland (Mon. Not. Roy. Astron. Soc., 175, 473, 1976) used, but the velocities for Pike's study were measured by a P.D.S. microdensitometer, with a consequent improvement in their quality. An earlier orbit was published by A.J. Deutsch (Publ. Astron. Soc. Pacific, 66, 58, 1954). Stickland's value for the period has been retained, since Pike himself regards it as more accurate than his own value of 99.2d. The most obvious improvement made by Pike's study is that now the evolved star is seen to be the more massive, as expected. (The spectral classes are also taken from Stickland's work.) System1291Orbit1End System1292Orbit1Begin The brightest member of A.D.S. 14847: B is 9.5m at about 3" and C is 12.0m at 82". Two other 12.0m companions at separations of about 200" are probably optical. System1292Orbit1End System1293Orbit1Begin The star is involved in nebulosity and H-alpha is seen in emission. The velocity of the centre of mass of the triple system is the sum of the Catalogue values of V0 for both the long-period and short- period pairs in this triple system. The actual value of V0 for the short-period pair is, of course, variable. Re-observation of this system might lead to a better separation of the two sets of orbital elements. The triple is the brightest member of A.D.S. 14832: companions are 12.0m and 12.6m at 4.1" and 69.9". System1293Orbit1End System1294Orbit1Begin The star is involved in nebulosity and H-alpha is seen in emission. The velocity of the centre of mass of the triple system is the sum of the Catalogue values of V0 for both the long-period and short- period pairs in this triple system. The actual value of V0 for the short-period pair is, of course, variable. Re-observation of this system might lead to a better separation of the two sets of orbital elements. The triple is the brightest member of A.D.S. 14832: companions are 12.0m and 12.6m at 4.1" and 69.9". System1294Orbit1End System1295Orbit1Begin These very approximate elements barely sudegce to establish the binary nature of this O-type star associated with a ring nebula. No epoch is given and the orbit is assumed circular. Both K and V0 are estimates (the latter made from the published graph). System1295Orbit1End System1296Orbit1Begin This star is the visual binary A.D.S. 14893 consisting of two nearly equal components revolving with an orbital period formerly believed to be 12.20y (P. Baize, J. Observateurs, 42, 118, 1959). West showed in his 1976 paper that one of the components (probably the marginally fainter -- Delta m=0.04 -- estimated to be slightly later in type) is a spectroscopic binary with a variable systemic velocity. He predicted that the visual orbit would be found to be an eccentric one of half the proposed period. This was confirmed by observations during the 1979 periastron passage from which West and McAlister derived the period of 2200d or 6.023y. Only preliminary elements are yet available for the visual (long-period) pair. Some speckle interferometric observations enable an orbital inclination of 125.6 deg to be deduced for that pair. Observations of the spectrum of the spectroscopic secondary, made by F.C. Fekel, are also reported in the abstract by West and McAlister. Those observations lead to masses of 1.25 MSol, 1.23 MSol and 0.78 MSol for the visual primary and the two components of the spectroscopic pair, respectively. System1296Orbit1End System1297Orbit1Begin This star is the visual binary A.D.S. 14893 consisting of two nearly equal components revolving with an orbital period formerly believed to be 12.20y (P. Baize, J. Observateurs, 42, 118, 1959). West showed in his 1976 paper that one of the components (probably the marginally fainter -- Delta m=0.04 -- estimated to be slightly later in type) is a spectroscopic binary with a variable systemic velocity. He predicted that the visual orbit would be found to be an eccentric one of half the proposed period. This was confirmed by observations during the 1979 periastron passage from which West and McAlister derived the period of 2200d or 6.023y. Only preliminary elements are yet available for the visual (long-period) pair. Some speckle interferometric observations enable an orbital inclination of 125.6 deg to be deduced for that pair. Observations of the spectrum of the spectroscopic secondary, made by F.C. Fekel, are also reported in the abstract by West and McAlister. Those observations lead to masses of 1.25 MSol, 1.23 MSol and 0.78 MSol for the visual primary and the two components of the spectroscopic pair, respectively. System1297Orbit1End System1298Orbit1Begin Harper later revised the period to 20.342d (Publ. Dom. Astrophys. Obs., 6, 249, 1935). Petrie(II) found Delta m=0.93. System1298Orbit1End System1299Orbit1Begin Original observations by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 1, 113, 1919). Luyten's recomputation is preferred because Plaskett fixed the value of T in his solution. Luyten adopted the epoch T0. Lucy & Sweeney adopt a circular orbit. Fekel (private communication) has detected the secondary spectrum in the red. System1299Orbit1End System1300Orbit1Begin The orbit is assumed circular (in accordance with the light-curve) and the epoch is the time of primary minimum. The period is known to be variable. Several photometric studies have been published and the results are summarized, and new UBV observations presented, by R.A. Breinhorst and H.W. Duerbeck (J. Astrophys. Astron., 3, 219, 1982). The light-curve is distorted and somewhat variable. The orbital inclination lies in the range 75 deg to 80 deg and the primary component gives more than 0.9 of the total light (in B). Breinhorst and Duerbeck believe that the primary component fills the Roche lobe and that the invisible secondary is a G1 V star. System1300Orbit1End System1301Orbit1Begin The observations do not cover the velocity-curve uniformly because the orbital period is very close to three years. The star is the fainter member of A.D.S. 14909. The brighter member, 36" away is 1 Peg (V=4.08m). Proper motions, radial velocities and spectral classifications (combined with apparent magnitudes) all support the hypothesis that the visual double is a physically related pair of stars. There is also a component C, 12.1m at 75" from A. System1301Orbit1End System1302Orbit1Begin Old observations from Mount Wilson suggest that the period may be a few days shorter. System1302Orbit1End System1303Orbit1Begin This is a Cepheid variable that is also a spectroscopic binary. The star is cooler than is normal for a Cepheid of its pulsation period (2.4d). It is suggested that the invisible companion may be a compact object. System1303Orbit1End System1304Orbit1Begin Epoch is T0 for primary component. A circular orbit was assumed after a solution by Sterne's method had yielded e=0.022+/-0.027. Patten and McKellar found Delta m=0.31, by Petrie's method. This value was confirmed by Petrie(II). Star is brightest member of A.D.S. 14943; principal companion is 12.2m at 9.2". System1304Orbit1End System1305Orbit1Begin The mass-ratio (estimated at 0.35) depends on only a few measures of the weak secondary spectrum and is uncertain. The spectrum appears to be that of a rapidly rotating (approx 150 km/s) Am star -- the type A3 V is derived from the hydrogen lines. A brief report on IUE spectra of the system has been published by R. Koch, M.J. Siah and M.N. Fanelli (Inf. Bull. Var. Stars, No. 1579, 1979). Photometric observations have been published by Y. Kondo (Astron. J., 71, 54, 1966) and O. Bendinelli et al. (Mem. Soc. Astron. Ital., 38, 763, 1967). New analyses of these observations have been published by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978) and K.-C. Leung and D.P. Schneider (Astrophys. J., 222, 917, 1978). The components are in or near contact and the light-curve displays interaction effects, but all computers agree on an orbital inclination within a few degrees of 65 deg, while estimates of the fractional luminosity of the brighter star (in V) range from 0.77 to 0.89. System1305Orbit1End System1306Orbit1Begin Only approximate elements have been published for the orbit of this barium star, and even those have not been published with full detail (no values for T or omega), but are described as `preliminary'. E. Bohm-Vitense (Astrophys. J., 239, L79, 1980) finds evidence from IUE spectra that the companion is a white dwarf. V.M. Smith and D.L. Lambert (Publ. Astron. Soc. Pacific, 96, 226, 1984) discuss the abundance of niobium and rubidium in the atmosphere of this star. The spectroscopic binary is the brighter member of A.D.S. 14971: companion is 12.5m at 21.3". System1306Orbit1End System1307Orbit1Begin Epoch is T0. Harper later revised the period to 21.720d (Publ. Dom. Astrophys. Obs., 6, 249, 1935). Lucy & Sweeney also adopt a circular orbit and derive very similar elements with a period of 21.7246d. Curchod and Hauck give the spectral type as A5 and F0, from the K line and the metallic lines respectively. System1307Orbit1End System1308Orbit1Begin These orbital elements are based on the same observations as the original elements derived by G.A. Radford and R.F. Griffin (Observatory, 95, 187, 1975). The elements were revised when Bassett found a significant eccentricity was required by the observations. System1308Orbit1End System1309Orbit1Begin This is a high-velocity, metal-poor star and is therefore of considerable interest. A discussion of its metal abundance was published by R.C. Peterson (Astrophys. J., 235, 491, 1980). The epoch is T0 for the primary component (preferred to periastron because the orbital eccentricity is small and different for each component). The two values of V0 are almost identical. Both components show H and K emission, and the primary at least shows Balmer-line emission. The authors conclude that the system is midway, in character, between the RS CVn and the BY Dra variables. Both components rotate slowly (V rot=7 km/s). System1309Orbit1End System1310Orbit1Begin These elements are based on an analysis of an extensive series of radial-velocity measurements published by O. Struve et al. (Astrophys. J., 118, 39, 1953). It is difficult to separate any orbital component of velocity from the pulsations intrinsic to variable stars of its type, and in the present case the evidence for binary nature is not completely convincing. The scatter of observations is comparable with the amplitude of the derived velocity curve. The star is the brightest member of A.D.S. 15032: B is 8.0m at 13.6". System1310Orbit1End System1311Orbit1Begin The orbital elements are derived from measures of the emission line at H-beta, which is visible for only about half the cycle. The value of V0 is uncertain by +/-100 km/s omega The orbit is assumed circular and the epoch is the time of optical minimum as given by J.E. McClintock et al. (Astrophys. J., 258, 245, 1982). This time of minimum coincides, within the observational uncertainties, with the times of X-ray eclipse and inferior conjunction of the source of H-beta emission. Orbital elements have also been published by J.R. Thorstensen and P.A. Charles (Astrophys. J., 253, 756, 1982) who find a similar value of K1 (216 km/s) and a different (but equally uncertain) value of V0 (+120 km/s). System1311Orbit1End System1312Orbit1Begin The elements of this system are described as preliminary by Burki and Mayor themselves. The spectrum is composite and the star has long been suspected to be binary. System1312Orbit1End System1313Orbit1Begin Popper's observations agree fairly well with earlier ones by W.E. Harper (J. Roy. Astron. Soc. Can., 29, 411, 1935) although the period has been revised. Popper assumed a circular orbit and the epoch is the time of primary minimum. The spectral type is that corresponding to the colours. Although the spectra are similar, Popper finds that the hotter shows Am characteristics while the cooler one does not. A photoelectric light-curve has been published by A. Abrami (Mem. Soc. Astron. Ital., 37, 369, 1966) who found eclipses to be about 0.4m deep at lambda 4000. He could not obtain a solution without assuming `third light' of 0.093. He derived i=88 deg and found that the primary star contributes 0.58 of the stellar light. R.A. Botsula (Izv. Engelhardt Obs. Kazan, 47, 19, 1981) finds an orbital inclination of 87 deg and that the two stars are equal in luminosity. Popper reports a faint visual companion, about six magnitudes fainter than the eclipsing binary, distant approximately 12". System1313Orbit1End System1314Orbit1Begin The epoch is T0 and the orbit is assumed circular. The velocities are based on measures of the K lines only. Bartolini et al. find by Petrie's method that the ratio of luminosities is 0.8 (also from the K line). Their photoelectric (BV) light-curves show the effects of gas streams in the system, but they derive i=78.3 deg. The total range of variation (in V) is about 0.5m. The photometric light ratio is consistent with the spectroscopic one. Reference: C.Bartolini et al. , Asiago Contr.,, No. 168, 1965 System1314Orbit1End System1315Orbit1Begin A. Colacevich found P=1037 d, T=J.D. 2,317,506, omega=90 deg, e=0.25, K1=8.0 km/s, V0=+34.7 km/s (Publ. Astron. Soc. Pacific, 47, 87, 1935). There is little to choose between the two sets of elements. H.L. Alden (Astron. J., 48, 81, 1939) assumed Colacevich's spectroscopic elements, and derived the following astrometric elements: a=0.052", i=65 deg, omega=37 deg. System1315Orbit1End System1316Orbit1Begin Harper later revised the period to 12.216d (Publ. Dom. Astrophys. Obs., 6, 250, 1935). Petrie(II) found Delta m=0.67. System1316Orbit1End System1317Orbit1Begin System1317Orbit1End System1318Orbit1Begin The spectrum of the secondary component is seen during primary eclipse. Photoelectric light- curves (UBV) have been published and analyzed by M.M. Ammann, D.S. Hall and R.C. Tate (Acta Astron., 29, 259, 1979) and re-analyzed by L. Milano et al. (Astrophys. Space Sci., 82, 189, 1982). The orbital inclination is close to 86 deg and the fractional luminosity (in V) of the brighter star is 0.83. The period is variable (D.S. Hall and K.S. Woolley, Publ. Astron. Soc. Pacific, 85, 618, 1973) and the light-curve suggests that the spectroscopic eccentricity is spurious. A modern velocity-curve is desirable. System1318Orbit1End System1319Orbit1Begin Earlier investigations were published by P. Wellmann (Z. Astrophys., 32, 1, 1953) and G.A. Bakos (Publ. David Dunlap Obs., 2, 431, 1965). Improved elements published by D.M. Popper (Astrophys. J., 244, 541, 1981) have been themselves superseded by the discovery that the system is triple and V0 for the short-period pair is therefore variable. The first elements published for the long-period orbit in the system are given in the Catalogue. The spectrum of the third body has not been detected, but the star's mass is estimated to be between 0.3 MSol and 0.7 MSol. Popper (loc. cit.) quotes the spectral types of the primary of the eclipsing pair as approximately A2 from the K line and A5 from the hydrogen lines. The short-period orbit is assumed circular, in accordance with the light- curve, despite small eccentricities found by some earlier investigators; the epoch is the time of primary minimum. Several photometric studies have been published, including one in the paper by Lacy and Popper. This is preferred since only they were aware of the existence of the third body. They cite and quote the earlier studies and find an orbital inclination of 88.6 deg and a fractional luminosity (at lambda 4400) for the primary component of 0.92. The third light would have had little effect on those analyses made by modern methods. System1319Orbit1End System1320Orbit1Begin Earlier investigations were published by P. Wellmann (Z. Astrophys., 32, 1, 1953) and G.A. Bakos (Publ. David Dunlap Obs., 2, 431, 1965). Improved elements published by D.M. Popper (Astrophys. J., 244, 541, 1981) have been themselves superseded by the discovery that the system is triple and V0 for the short-period pair is therefore variable. The first elements published for the long-period orbit in the system are given in the Catalogue. The spectrum of the third body has not been detected, but the star's mass is estimated to be between 0.3 MSol and 0.7 MSol. Popper (loc. cit.) quotes the spectral types of the primary of the eclipsing pair as approximately A2 from the K line and A5 from the hydrogen lines. The short-period orbit is assumed circular, in accordance with the light- curve, despite small eccentricities found by some earlier investigators; the epoch is the time of primary minimum. Several photometric studies have been published, including one in the paper by Lacy and Popper. This is preferred since only they were aware of the existence of the third body. They cite and quote the earlier studies and find an orbital inclination of 88.6 deg and a fractional luminosity (at lambda 4400) for the primary component of 0.92. The third light would have had little effect on those analyses made by modern methods. System1320Orbit1End System1321Orbit1Begin Earlier investigations were published by J.S. Plaskett (Publ. Dom. Astrophys. Obs., 2, 269, 1923 and 4, 108, 1928) and W.C. Rufus (Publ. Michigan Obs., 6, 45, 1934). The system has presented difficulties in the past, even the period being difficult to determine precisely. Crampton and Redman have used velocities determined from measures of the He II lines only. Although their measures are few and K2 is highly uncertain, Crampton and Redman confirm the existence of a secondary spectrum, suspected by Rufus and also by P.S. Conti and W.R. Alschuler (Astrophys. J., 170, 325, 1971) who estimated Delta m=0.8. There is some evidence for a small range of variability in the light of the star. Crampton and Redman conclude that it is unlikely that this system is connected with the X-ray source Cep X-4. The star is the brightest component of A.D.S. 15184. A number of faint companions are listed in I.D.S. including a possibly suspect one of 13.3m at 1.6". There are also a 7.7m companion at 11.7" and one of 7.8m at 19.9". System1321Orbit1End System1322Orbit1Begin Earlier investigations were published by J. Lunt (Astrophys. J., 47, 134, 1918; Cape Annals, 10, pt. 6, 3F, 1921) and H.S. Jones (Cape Annals, 10, pt. 8, 81, 1928). Jones believed the systemic velocity varied, but his conclusion was contested by W.J. Luyten (Publ. Minnesota Obs., 2, 17, 1934). Sanford's elements largely confirm those derived by Jones, and Sanford also considered that V0 is probably variable. The mean error per plate is higher than would be expected for this type of spectrum. Except for this question of variation in V0, the elements seem to be well determined. System1322Orbit1End System1323Orbit1Begin Epoch is T0 for the primary component. Sanford reported that `the differences in spectral type and line intensity are negligible'. System1323Orbit1End System1324Orbit1Begin Epoch is T0. Circular orbit assumed. Original observations were published by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 324, 1926) who fixed the value of T in his solution. Luyten's recomputation in which a circular orbit was assumed has been preferred. The scatter of the observations is rather large, but Harper found no need to revise his elements (Publ. Dom. Astrophys. Obs., 6, 250, 1935). Petrie(II) found Delta m=0.32. The star is listed in I.D.S. and has a companion of nearly equal brightness at about 0.2". An orbit has been computed for the visual pair by G. Van Biesbroeck (Publ. Yerkes Obs., 9, pt. 2, 1960). The period is 24.40y. System1324Orbit1End System1325Orbit1Begin The epoch is T0 and a circular orbit was assumed. Lucy & Sweeney confirm the circular orbit and derive K1=11.2 km/s. System1325Orbit1End System1326Orbit1Begin The early work on this eruptive variable by A.H. Joy (Astrophys. J., 124, 317, 1956) and M.F. Walker and G. Chincarini (ibid., 154, 157, 1968), together with J. Smak's (Acta Astron., 19, 287, 1969) attempt to unify them, is now superseded by several more modern studies. We have chosen the one by E.L. Robinson, E.-H. Zhang and R.J. Stover, even though it is concerned primarily with the late-type component, because it seems to us the most thorough discussion available. It draws upon other recent work by R.J. Stover et al. (Astrophys. J., 240, 597, 1980), A.P. Cowley, D. Crampton and J.B. Hutchings (ibid., 241, 269, 1980), M.F. Walker (ibid., 248, 256, 1981) and F.V. Hessmann et al. (ibid., 286, 747, 1984) and attempts to reconcile differences between them. The orbit is assumed circular and the epoch is T0 for the K5 component. The value of K1 (for the white-dwarf component) is the mean of that found by Hessmann et al. and Stover et al. The value of K2 is that finally adopted by Robinson et al. The value of V0 is very uncertain, Robinson et al. quote figures found by other investigators, ranging from 1 km/s to 38 km/s. A value near the middle of this range seems the most probable. The system does not eclipse and the inclination of the orbit is not known, but Robinson et al. argue that it must be less than 60 deg. The requirement that the mass of the white dwarf does not exceed 1.4 MSol puts a lower limit of about 35 deg on the inclination. System1326Orbit1End System1327Orbit1Begin Tomkin's work supersedes the spectroscopic study by E.G. Ebbighausen (Astron. J., 71, 730, 1966) because of both the superior precision of the former's Reticon results and his success in detecting the secondary spectrum. Tomkin discusses at some length the relative merits of Ebbighausen's photometric solution (Astron. J., 71, 642, 1966) and the reanalysis of the same observations by M. Mezzetti et al. (Astron. Astrophys. Supp., 42, 15, 1980). All have been superseded by a new analysis by G. Hill and E.G. Ebbighausen (Astron. J., 89, 1256, 1984 -- from which paper the depth of eclipse in V has been estimated) who find an orbital inclination of 89 deg and a visual magnitude difference between the components of approximately 2.5m. The effective temperature they give for the secondary component is that of an early G-type star. The expected rate of apsidal motion is too slow to be detected spectroscopically for some time, but Hill and Ebbighausen derive, from eclipse times, an apsidal period of about 5,500 years -- which is roughly confirmed by A. Gimenez and T.E. Margrave (Astron. J., 90, 358, 1985). According to E.F. Guinan and F.P. Maloney (ibid., 90, 1519, 1985) this is in accord with the theory of general relativity. System1327Orbit1End System1328Orbit1Begin The orbital elements derived by R.F. Sanford (Astrophys. J., 53, 218, 1921) were based on a period of 3.74860d. R.W. Tanner (Publ. David Dunlap Obs., 1, 483, 1949) showed that the observations could be better satisfied by a circular orbit with a period of 3.23d. New observations by Fisk and Abt have confirmed the shorter period. The small orbital eccentricity perhaps should be ignored. System1328Orbit1End System1329Orbit1Begin There are new observations by H.A. Abt and S.G. Levy (Astrophys. J. Supp., 30, 273, 1976) that lead to rather different elements, especially K1 which they find to be 34.7 km/s. The system should be further observed to decide between the two sets. Possible interference by the spectrum of the visual companion is the cause of the uncertainty. The system is A.D.S. 15281 for which an orbit with a period of 11y.52 was computed and published by Luyten in the same paper as that cited in the Catalogue. The element V0, therefore is variable. Lucy & Sweeney adopt a circular orbit. Recently W.R. Beardsley and M.W. King (Publ. Astron. Soc. Pacific, 88, 200, 1976) have obtained separate spectra of the two stars in the visual pair (Delta m=0.3). They identified B as the presently known spectroscopic binary and found double lines in the spectrum of A. They believe the period of A to be 4.77d. D.J. Barlow and C.D. Scarfe (Publ. Astron. Soc. Pacific, 89, 857, 1977) have, however, questioned the claim that the visual primary is double and it appears likely that the system is only triple. It is still premature to give spectroscopic elements for the visual pair. There is also a 10.8m visual companion at 13.8". System1329Orbit1End System1330Orbit1Begin Several earlier attempts to obtain orbital elements, based on incorrect values for the period, are cited in the orbital study by A.P. Cowley, D. Crampton and J.B. Hutchings (Astrophys. J., 231, 539, 1979). The elements given here confirm those first derived in that study. The comparatively late optical spectrum permits rather better radial-velocity measures than are often possible for X-ray binaries. According to Crampton and Cowley, their results rule out the degenerate-dwarf model proposed by G. Branduardi et al. (Astrophys. J., 235, L153, 1980). Another discussion of models for the system will be found in J. Zio lkowski and B. Paczynski (Acta Astron., 30, 143, 1980). The spectrum varies and the spectral type given is only approximate. System1330Orbit1End System1331Orbit1Begin Earlier investigations were published by C.C. Crump (Astrophys. J., 54, 127, 1921 -- recomputed by Luyten and M. Stewart (J. Roy. Astron. Soc. Can., 52, 11, 1958). A few observations were also published by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961). The elements are well determined, except for some doubt about the cause of apparent variations in the value of K (Crump found K=65.7 km/s). Abt gives the spectral type as A6, F2 and F2 IV from the K line, hydrogen lines and metallic lines, respectively, but not all classifiers now agree that this is an Am star. Shallow eclipses have been detected, but analysis of the light-curve presents difficulties because of changes in the light-curve (F.B. Wood and G. Lampert, Publ. Astron. Soc. Pacific, 75, 281, 1963). Star is brightest member of A.D.S. 15314: B is 15.8m at 69.1", and C is 12.7m at 120". Lucy & Sweeney adopt a circular orbit. System1331Orbit1End System1332Orbit1Begin Taffara regarded these elements as provisional, and expressed some doubt about the value of the period. Similar elements were obtained from these observations by A. Krancj and L. Pigoni (Publ. Bologna Univ. Obs., 7, No. 17, 1960). System1332Orbit1End System1333Orbit1Begin The orbit is assumed circular and the epoch is T0. System1333Orbit1End System1334Orbit1Begin Petrie(I) also found Delta m=0.23. He estimated i=17 deg if the components conform to the mass-luminosity relation. System1334Orbit1End System1335Orbit1Begin The elements given in the Catalogue supersede those published by A.P. Cowley and R. Stencel (Astrophys. J., 184, 687, 1973) based on a somewhat longer value for the period. Since the Seventh Catalogue appeared, J.D. Fernie has redetermined the period photometrically, finding 816.5d (Publ. Astron. Soc. Pacific, 97, 653, 1985). The magnitudes given are estimated graphically from Fernie's paper and refer to the range at the time of his observations. Historically, of course, the range has been greater. The emission component of the spectrum of this symbiotic star is sometimes classified as a WN spectrum, but the hot star itself does not appear to be a typical Wolf-Rayet star. Emission lines give values of K2 ranging from 10 km/s to 30 km/s, but they do not move exactly out of phase with absorption lines in the spectrum of the M-type giant, and seem to require different periods. Hutchings, Cowley and Redman give an elliptical solution for the orbital elements as well as the circular one given in the Catalogue; there are no strong reasons for preferring one to the other, but the eccentricity may be spurious. The epoch is T0 for the M-type component. A detailed discussion of the spectrum and a possible model have been published by C.D. Keyes and M.J. Plavec (I.A.U. Symp. No. 88, p. 535, 1980). See also, C.M. Anderson and J.S. Gallagher (Bull. Am. Astron. Soc., 10, 410, 1978). A discussion of evidence for magnetic fields in the system was published by M.H. Slovak (Astrophys. J., 262, 282, 1982). System1335Orbit1End System1336Orbit1Begin McKellar and Patten found that a circular orbit with V0=15.33 km/s and K=30.71 km/s would fit the observations almost as well as the elements given in the Catalogue. Lucy & Sweeney did adopt a circular orbit. The star is the brighter component of A.D.S. 15366: B is 9.6m at 11.8" and has a proper motion similar to that of A. System1336Orbit1End System1337Orbit1Begin These elements are derived from observations made by Stickland and Weatherby and by G.C.L. Aikman (Publ. Dom. Astrophys. Obs., 14, 379, 1976). The star is another binary in the mercury-manganese group. System1337Orbit1End System1338Orbit1Begin Epoch is primary minimum. Earlier investigations have been published by O. Struve (Astrophys. J., 102, 74, 1945) and L.T. Slocum (Astrophys. J., 105, 350, 1947). The orbit of the secondary component is very well determined, but the velocities derived for the primary component do not represent Keplerian motion. The values of K1 and hence of the masses, are very uncertain. It is difficult to assign a quality to the orbit because of this difference in the behaviour of the two components. From their narrow-band photoelectric photometry, Hilton and McNamara conclude that eclipses are partial, thus invalidating earlier photometric solutions based on the assumption that eclipses are total. They estimate Delta m=1.1 and i=90 deg. Another photoelectric light-curve has been published by A. Fresa (Mem. Soc. Astron. Ital., 37, 539, 1966) who finds i=87 deg and the fractional luminosity of the primary star is 0.93. B. Cester et al. (Astron. Astrophys., 62, 291, 1978) re-analyzed Fresa's observations and confirmed his value for the inclination while finding a fractional luminosity of 0.83. System1338Orbit1End System1339Orbit1Begin The new work by Popper supersedes the earlier orbit by J.A. Pearce (Publ. Dom. Astrophys. Obs., 6, 74, 1938). Working at higher resolution, Popper has been able to show that the value derived for the period by Pearce was incorrect, and that Pearce also overestimated the amplitudes of the velocity variations. The new results conform much more closely to the mass-luminosity relation than did the old. An accurate difference of magnitude between the components is difficult to estimate. The star is the brightest member of A.D.S. 15405: B is 7.3m at 18.3", C is 13.2m at 55.2". System1339Orbit1End System1340Orbit1Begin Earlier investigations of this well-known system have been published by W.E. Harper (J. Roy. Astron. Soc. Can., 28, 173, 1934); S. Gaposchkin (Publ. Am. Astron. Soc., 9, 39, 1937); V. Goedicke (Publ. Michigan Obs., 8, 1, 1939); B.F. Peery (Astrophys. J., 144, 672, 1966); and K.O. Wright and J.B. Hutchings (Mon. Not. Roy. Astron. Soc., 155, 203, 1971). The elements given in the Catalogue are a refinement by Wright, who has now followed the system at high dispersion through a complete cycle, of the elements earlier published by Hutchings and Wright. The value of K2 is determined from measurements of the H-alpha emission. Wright has obtained a much lower value than Peery derived from the H-alpha emission, and therefore obtains more believable masses. The classification of the `B star' is problematical -- its spectrum could be as early as O8. An orbital inclination of 77 deg was derived by Hutchings and Wright from a consideration of observations made near primary eclipse. There is ample evidence (discussed in detail by Wright) for transfer of mass from the M supergiant to the hot star, and analysis of the light-curve itself is difficult. A combined photometric, spectroscopic and astrometric study by L.W. Frederick (Astron. J., 65, 628, 1960) gave P=20.34y, T=1951.2, omega=302 deg, e=0.5, a=0.03", and i=90.39 deg. However the spectroscopic and astrometric data are not entirely accordant. In an earlier paper, Wright (Vistas in Astron., 12, 147, 1970) gives Delta m(vis) approx 3.5. The star is a magnetic variable. Several photometric studies of the 1976-78 eclipse have been published (L. Baldinelli et al. Mem. Soc. Astron. Ital., 52, 275, 1981, M. Saito et al., Publ. Astron. Soc. Japan, 32, 163, 1980 and M. Nakagiri and Y. Yamashita, Ann. Tokyo Obs., 17, 147, 1979). Details of the UV spectrum have been published by R. Faraggiana (I.A.U. Symp. No. 88, p. 549, 1980) and a brief account by W. Hagen et al. (Bull. Am. Astron. Soc., 10, 620, 1978). Spectroscopic observations of the eclipse ingress were published by C. Mollenhoff and K. Schaifers (Astron. Astrophys., 64, 253, 1978). Several papers in Highlights in Astronomy, 7, 1986 concern systems of this general type; especially relevant to VV Cep is the paper by E.F. Guinan et al. on p. 211. The companion listed in I.D.S. is presumably the spectroscopic secondary. System1340Orbit1End System1341Orbit1Begin There is evidence of a shell spectrum on some of the spectrograms. Lucy & Sweeney adopt a circular orbit. System1341Orbit1End System1342Orbit1Begin By Petrie's method, Delta m=0.54: from the mass-luminosity relation the orbital inclination is 41 deg. There is no conclusive evidence for apsidal motion, but there is some evidence, from earlier Victoria observations, for changes in V0 and K1 and K2. The observations used to determine the elements given in the Catalogue are modern, high-dispersion observations concentrated in a ten-year interval. System1342Orbit1End System1343Orbit1Begin Elements were published for this system by H.A. Abt et al. (Astrophys. J., 161, 477, 1970), but further observations by Rogers showed that the period should be doubled and the range of variation considerably increased. See also the note for BD+52 3135. An entry with these coordinates appears in I.D.S. but the magnitudes given do not tally with that of this system. System1343Orbit1End System1344Orbit1Begin The new observations by Hill and Hutchings have shown that this system is not as easy to interpret as appeared from the earlier work of J.A. Pearce (J. Roy. Astron. Soc. Can., 29, 411, 1935). Hill and Hutchings assumed a circular orbit, in accordance with the UBV light-curves of D.S. Hall and R.H. Hardie (Publ. Astron. Soc. Pacific, 81, 754, 1969), and fixed the epoch T0 in their solution by reference to the observed time of minimum light. They were unable to detect the secondary spectrum directly, but they could see its effect on the line profiles of the hydrogen lines. By analysis of these profiles they derived a mass-ratio (primary.secondary) of 1.81 (compare Pearce's 1.18), individual masses of 4.4 MSol and 2.5 MSol, and Delta m(bol)=2.2. The asymmetries in the line profiles and a conspicuous rotation effect during primary eclipse which were both noted by Hill and Hutchings, may help to explain the appreciable eccentricity (0.12) found by Pearce. The scatter of observations about the velocity curve is fairly large. Several modern analyses have been made of the photoelectric observations by Hall and Hardie and M.I. Lavrov (Bull. Engelhardt Obs., No. 38, 1965). The most recent is by A.P. Linnell and J. Kallrath (Astrophys. J., 316, 754, 1987) who considered several previously published sets of observations and found an orbital inclination close to 83 deg and a fractional luminosity of 0.84 (in B and V) for the primary star. They give computed spectral types of B3 and B7 and find both stars to be close to the main sequence. B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) from a study of the observations by Hall and Hardie find an inclination of 85 deg and a fractional luminosity in V of 0.92. S. Soderhjelm (Astron. Astrophys., 66, 161, 1978) finds that there is no unique solution of the light-curve and argues that the system is semi-detached. From light-curve synthesis, Hill and Hutchings (Astrophys. Space Sci., 20, 123, 1973) find i=86 deg and that the ratio of luminosities (at lambda 5500) is 3.6. System1344Orbit1End System1345Orbit1Begin Popper assumed a circular orbit and the epoch is the time of primary minimum. His results agree quite well with those of R.F. Sanford (Astrophys. J., 79, 95, 1934) despite the difficulties that both investigators encountered in measuring the secondary spectrum. The velocities of the secondary component show considerable scatter and the spectral type is estimated from the colours. R.C. Barnes et al. (Publ. Astron. Soc. Pacific, 80, 69, 1968) published UBV observations, and, on the assumption that primary eclipse is a transit, derived an orbital inclination of 87 deg and a fractional luminosity (in V) for the primary star of 0.73. A.P. Linnell (Astrophys. Space Sci., 22, 13, 1973) assumed primary eclipse to be an occultation and derived, from the same observations, 87 deg and 0.68 respectively. The observations have been analyzed a third time by B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978) who claim to show decisively that the cooler, fainter star is also the smaller and derive 87 deg and 0.73. Similar figures were obtained by R.A. Botsula (Izv. Kazan Obs., 47, 19, 1981). System1345Orbit1End System1346Orbit1Begin The orbit was assumed circular, and the epoch is the time of primary minimum as redetermined by Paffhausen and Seggewiss. The velocities show a pronounced rotation effect during primary eclipse. No light-curve has yet been published. The star is the brighter component of A.D.S. 15562: B at 3.7" is nearly as bright and is estimated to be of spectral type G2 V. There is also an 11.7m component at 43". System1346Orbit1End System1347Orbit1Begin The present observations do not cover the velocity-curve as well as the older observations by A.H. Joy (Astrophys. J., 74, 101, 1931), being concentrated in one half. The uncertainties ascribed to K1 and K2 are comparable in the two solutions, but we suspect that the slightly lower values found for these two elements by Huenemoerder and Barden are the more nearly correct. The orbit is assumed circular and the epoch is the time of primary minimum. Huenemoerder and Barden also discuss the UV spectrum of this RS CVn system. Modern photometry (E.F. Milone, Astron. J., 73, 708, 1968, D.S. Hall, Inf. Bull. Var. Stars, No. 259, 1968) has shown the light-curve to be complex and variable. Milone has published a preliminary solution of the V light-curve (Astron. J., 82, 998, 1977), finding an inclination of 89 deg and a fractional luminosity of 0.59 for the larger component. He has also published the results of infrared photometry (E.F. Milone, Astrophys. J. Supp., 31, 93, 1976). Variations in the H and K emission have been noted by J.C. Droppo and E.F. Milone (Inf. Bull. Var. Stars, No. 1130, 1976), while D.P. Huenemoerder has studied the H-alpha profile and concluded that it provides evidence for the presence of intermittent gas streams in the system. J.A. Eaton and D.S. Hall (Astrophys. J., 227, 907, 1979) have applied the starspot model to this system. D.M. Gibson (Bull. Am. Astron. Soc., 11, 651, 1979) has observed soft X-ray flares. System1347Orbit1End System1348Orbit1Begin Hilditch's observations complement and confirm those of R.M. Petrie (Publ. Dom. Astrophys. Obs., 12, 111, 1962). The new orbital elements do not differ significantly from those obtained by Petrie. The secondary spectrum is similar to the primary, but the appearance of lambda 4686 He II in the two spectra leads Hilditch to conclude that the secondary star is of a different luminosity class from the primary. Petrie had found Delta m=0.48 and that the two stars apparently did not obey the mass-luminosity relation. Hilditch confirms this result in that he finds the secondary star to be overluminous for its mass. He deduces that mass has been transferred between the components. The star's light has long been suspected of variability and recent observations (N.K. Rao, Publ. Astron. Soc. Pacific, 84, 563, 1972; G. Hill et al., Publ. Dom. Astrophys. Obs., 15, 1, 1976) show that it is an ellipsoidal variable. System1348Orbit1End System1349Orbit1Begin These elements are similar to those derived by R.B. Jones and A.H. Farnsworth (Lick Obs. Bull., 16, 46, 1932) but are preferred because they have a longer time base and have been computed without the need to fix T or omega. The epoch is T0, and the eccentricity should probably be assumed to be zero. Abt and Levy give spectral types of A3, A8 and A4 from the K line, hydrogen lines and metallic lines, respectively. System1349Orbit1End System1350Orbit1Begin The binary nature of this star was suspected by H.A. Abt (Astrophys. J. Supp., 6, 37, 1961) who classified the primary spectrum as A2, F0, F5 IV from the K line, the hydrogen lines, and the metallic lines respectively. Vickers and Scarfe were unable to classify the secondary spectrum precisely, but deduce that it lies within the range F2 III-IV to F5 III-IV. They estimate Delta m(photographic) to be 0.55. An unpublished measurement by speckle interferometry reported by H.A. McAlister had enabled Vickers and Scarfe to derive i=47 deg and hence individual masses of 2.2 MSol and 0.8 MSol for the spectroscopic pair. The secondary is thus undermassive for its luminosity and this presents an evolutionary problem that is discussed by Vickers and Scarfe. For more up-to-date results of speckle interferometry see H.A. McAlister et al. (Astrophys. J. Supp., 54, 251, 1984). The spectroscopic pair is the brightest member of A.D.S. 15600: B is 6.5m at 7.5" and has a common proper motion with A. The 12.7m companion at 97" is probably optical. System1350Orbit1End System1351Orbit1Begin The new observations complement and confirm earlier ones by R.J. Northcott (Publ. David Dunlap Obs., 1, 369, 1947). The spectrum of the star shows very strong H and K emission. The velocities derived from the emission lines agree closely with those from the absorption lines. The width of the emission lines leads to an estimate MV=+0.8. The very small eccentricity probably should be ignored. (Lucy & Sweeney derived a circular orbit from Northcott's observations). The system shows light variations in a period of 25.3d -- slightly different from the orbital period (C. Blanco and S. Catalano, Astron. Astrophys., 4, 482, 1970). The shape of the light-curve is variable. System1351Orbit1End System1352Orbit1Begin Epoch is T0 for the primary component: circular orbit assumed. Star is component B of A.D.S. 15571: A is 7.1m at 13.7" and has the same proper motion as and similar velocity to B. There is also C at 145" from A. No information is given about the relative intensities of the component spectra. System1352Orbit1End System1353Orbit1Begin An earlier study of this system was published by R.K. Young (Publ. Dom. Astrophys. Obs., 1, 193, 1920) who assumed a circular orbit. Van Albada and Klomp discuss new observations from McDonald Observatory and the Hale Observatories. They also recompute the Victoria orbit with their revised value of the period. There are differences between the three sets of elements some of which appear to be significant, and which may, as van Albada and Klomp suggest, be the result of an unresolved secondary spectrum. System1353Orbit1End System1354Orbit1Begin The new elements are preferred to all earlier investigations because Fekel and Tomkin succeeded in measuring the lines of the secondary spectrum, first detected by G.H. Herbig (Astrophys. J., 141, 595, 1965). Most investigations of the orbit of the primary (H.A. Abt and S.G. Levy, Astrophys. J. Supp., 30, 273, 1976, R.M. Petrie and E. Phibbs, Publ. Dom. Astrophys. Obs., 8, 225, 1949, H.D. Curtis, Lick Obs. Bull., 2, 169, 1904 -- recomputed by Luyten, and W. Zurhellen, Astron. Nachr., 177, 321, 1908) agree with each other and with the new results. The exception is the work of G.R. Miczaika (Z. Astrophys., 29, 108, 1951). The orbit is assumed circular and the epoch is T0 for the primary component. Fekel and Tomkin estimate Delta m(in the red region) to be 1.60m and suggest a spectral type of G5 V or later. An 11.4m companion at 104", listed in I.D.S., is probably optical. System1354Orbit1End System1355Orbit1Begin The epoch is T0 for the primary component and the orbit is assumed circular. The elements are similar to those found earlier by W.E. Harper (J. Roy. Astron. Soc. Can., 27, 146, 1933). Sanford found that the relative intensities of the two spectra varied throughout the cycle. He also noted the emission at the H and K lines. As one of the brighter members of the RS CVn class, the system has naturally attracted much attention: it was the first star, in modern times, for which spots were proposed to explain variations and distortions in the light-curve (G.E. Kron, Publ. Astron. Soc. Pacific, 59, 261, 1947). It is known as a radio source (D.M. Gibson and R.M. Hjellming, ibid., 86, 652, 1974). Spectral variations at H and K and at H-alpha have been studied by S.A. Naftilan and G.C.L. Aikman (Astron. J., 86, 766, 1981) and H.L. Nations and L.W. Ramsey (ibid., 85, 1086, 1980) respectively, as well as by M.B. Babayev (Peremm. Zvezdy, 19, 377, 1974 and 20, 207, 1975), D.P. Huenemoerder and L.W. Ramsey (Astron. J., 89, 549, 1984) and P.S. Goraya and S.K. Srivastava (Inf. Bull. Var. Stars, No. 2579, 1984). The results of IUE observations of the spectrum are published by M. Rodono et al. (Astron. Astrophys., 176, 267, 1987). Several light-curves and photometric analyses have been published (R.K. Srivastava, Astrophys. Space Sci., 78, 123, 1981, Acta Astron., 34, 291, 1984; A.C. Theokas, Astrophys. Space Sci., 52, 213, 1977, E.-H. Lee, K.-Y. Chen and I.-S. Nha Astron. J., 91, 1438, 1986). The best is still probably that by C.R. Chambliss (Publ. Astron. Soc. Pacific, 88, 762, 1986) who found an orbital inclination of 86 deg and a fractional luminosity (in yellow light), for the brighter, star of 0.59. He also proposed spectral types of G2 IV and K0 IV for the two stars. System1355Orbit1End System1356Orbit1Begin The star is considered by Griffin probably to be a dwarf. System1356Orbit1End System1357Orbit1Begin These orbital elements are based on few observations and are described as `preliminary' by Andersen and Nordstrom themselves. The spectral type is from the H.D. Catalogue. The small eccentricity is believed to be real, but the epoch is the time at which an eclipse of one of the two nearly equal components would be expected if the orbital inclination were high enough. Eclipses are unlikely and E.H. Olsen (Astrophys. J. Supp., 54, 55, 1983) found no evidence for variable light. System1357Orbit1End System1358Orbit1Begin There is some uncertainty about the spectral type and luminosity class. Those given in the Catalogue are from the paper by Nadal et al. System1358Orbit1End System1359Orbit1Begin The elements of the Wolf-Rayet star (upper line) are based on measures of the N IV lambda 4058 line and are subject to revision when it becomes possible to measure He II lambda 4686. The coverage of the velocity-curve is not good. The orbit is assumed circular and the epoch is the time of inferior conjunction of the W-R star. (The times found from the two components are slightly but probably not significantly different -- 0.03d). Massey and Conti estimate that the orbital inclination is not much greater than 50 deg. N.A. Lipunova and A.M. Cherepashchuk (Astron. Zh., 59, 73, 1982) have published BV R light-curves and also estimate an inclination of about 53 deg. System1359Orbit1End System1360Orbit1Begin This is one of a group of binaries in the Perseus arm investigated by Abt et al. To allow for possible distortion of the spectrum, radial-velocity measurements were made with an oscilloscope device by setting on the mid-points of the line wings, rather than on the cores. In the only case in which an independent investigation has been made (H.D. 235679) very different orbital elements were derived by the other investigator. That system, however, was a low-amplitude one with the longest period in the group. See also notes for HD 235679, BD+54 2726, BD+43 2837, HD 235807, HD 212827, BD+53 2885, HD 239967, BD+54 2790, BD+55 2770 and HD 240068. System1360Orbit1End System1361Orbit1Begin The period was found from a discussion of times of minimum light and differs slightly from earlier published values. A photoelectric light-curve by S. Cristaldi and K. Walter (Astron. Nachr., 287, 103, 1963) gives i=76.7deg and a fractional luminosity of the primary star (at lambda 4500) of 0.93. System1361Orbit1End System1362Orbit1Begin Epoch is T0 for the late-type component and the orbit was assumed circular. The upper line in the Catalogue refers to the early-type component. Kraft states that the luminosity class of the G-star changes during the cycle. System1362Orbit1End System1363Orbit1Begin Only two cycles of orbital motion are covered by the period. An astrometric orbit has been derived by H.L. Alden (Astron. J., 47, 185, 1939). He assumed Jones' spectroscopic elements and found a=0.049", i=113 deg, and omega=76 deg. System1363Orbit1End System1364Orbit1Begin Lucy & Sweeney adopt a circular orbit. The star is not listed by Curchod and Hauck. System1364Orbit1End System1365Orbit1Begin The spectrum of the optical counterpart of this X-ray source is typical of a cataclysmic binary. The magnitude is given only approximately and is subject to variations in a period of about 21 m as well as in the orbital period of between four and five hours. The first estimate of the orbital period was just over four hours (J. Patterson and J.E. Steiner, Astrophys. J., 264, L61, 1983). Shafter and Targon still have insufficient observations to choose between this and the longer value given in the Catalogue, but seem to favour the latter. The orbit is assumed circular; no epoch is given. Patterson and Steiner give an orbital `minimum' of J.D. 2,444,782.879 but do not make clear what phase this is. Shafter and Targon regard the time of inferior conjunction of the emission-line source as zero phase, but give no date for it. System1365Orbit1End System1366Orbit1Begin See note for BD+52 3135. System1366Orbit1End System1367Orbit1Begin See note for BD+52 3135. System1367Orbit1End System1368Orbit1Begin Preliminary orbital elements were derived from heterogeneous observations. The orbit is assumed circular and the epoch appears to be the time of minimum radial velocity. The spectrum is that of a mercury-manganese star. System1368Orbit1End System1369Orbit1Begin Massey's observations and results supersede earlier work by W.A. Hiltner (Astrophys. J., 101, 356, 1945), K. Bracher (Publ. Astron. Soc. Pacific, 80, 165, 1968) and K.S. Ganesh and M.K.V. Bappu (Kodaikanal Bull., Series. A, No. 185, 1968). The orbital elements for the Wolf-Rayet component (upper line) are derived from the N IV emission line lambda 4058. The orbit is assumed circular and the epoch is the time of primary minimum (the first evidence for eclipses was found by R.M. Hjellming and W.A. Hiltner (Astrophys. J., 137, 1080, 1963). It is not yet possible to derive an orbital inclination. Massey finds evidence for a second periodicity in the absorption lines of the O-type spectrum and proposes that the entire system is multiple, a second binary in the system having at least one O-type component. He suggests as orbital elements for this pair: P=3.4698d, T (inferior conj.)=J.D. 2,443,689.59, e=0, K1=66 km/s and V0=55 km/s. The mean error of a single observation is 58 km/s. It seems premature to include these elements in the Catalogue. J.B. Hutchings and P. Massey (Publ. Astron. Soc. Pacific, 95, 151, 1983) have published observations and radial-velocity measurements of the ultraviolet spectrum. Spectroscopic and photometric observations have also been published by K. Annuk and T. Nugis (Publ. Tartu Astrophys. Obs., 49, 84, 1982)). System1369Orbit1End System1370Orbit1Begin Hilditch's values of the orbital elements are based on new observations combined with old ones by R.H. Baker (Publ. Allegheny Obs., 1, 93, 1909) and by W.J. Luyten et al. (Publ. Yerkes Obs., 7, pt. IV, 251, 1939). Luyten also recomputed the elements from Baker's observations. Petrie(I) found Delta m=1.03. According to Hilditch at least one of the components is probably somewhat evolved from the zero-age main sequence. Both components obey the mass-luminosity relation, however, and there is no evidence of any variation in the light of the system. The system is the brighter component of A.D.S. 15862: B is 10.9m at 48.2". System1370Orbit1End System1371Orbit1Begin See note for BD+52 3135. Abt et al. use the designation BD+54 2745 interchangeably with the H.D.E. number given in the Catalogue. System1371Orbit1End System1372Orbit1Begin The spectral types appear to be derived from photometry (Kh. F. Khaliullin and V.S. Kozureva, Astrophys. Space Sci., 120, 9, 1986). The magnitudes given are also taken from that work. The star of later spectral type is the brighter and the more massive, according to Imbert. Analysis of the photoelectric light-curve gives an orbital inclination of 88.7 deg and a visual magnitude difference, between the components, of 0.23m. System1372Orbit1End System1373Orbit1Begin See note for BD+52 3135. This low-amplitude binary should be checked. System1373Orbit1End System1374Orbit1Begin See note for BD+52 3135. System1374Orbit1End System1375Orbit1Begin See note for BD+52 3135. The scatter of observations is an appreciable fraction of the amplitude. System1375Orbit1End System1376Orbit1Begin It is difficult to assess these elements, since the numerical values of the observations are not given. The star does exhibit a composite spectrum. The spectral types given are Hendry's own, except that she indicates the A8 classification is uncertain. The Bright Star Catalogue gives M0 II + B8 V. The period proposed is 41.95y. System1376Orbit1End System1377Orbit1Begin Lucy & Sweeney adopt a circular orbit. A 9.7m companion at 63.9" is listed in I.D.S. System1377Orbit1End System1378Orbit1Begin The orbital elements, described by Beardsley as preliminary, are derived from annual mean velocities obtained at several different observatories. System1378Orbit1End System1379Orbit1Begin Griffin deduces the luminosity class from the small proper motion. System1379Orbit1End System1380Orbit1Begin See note for BD+52 3135. System1380Orbit1End System1381Orbit1Begin Epoch is T0 : circular orbit assumed. No analysis of the light-curve appears to have been made. A close, faint companion is mentioned in the Finding List, but is not listed in I.D.S. System1381Orbit1End System1382Orbit1Begin There are now three sets of observations of this system. The other two are by W.E. Harper (Publ. Dom. Astrophys. Obs., 6, 203, 1933) and V.A. Albitzky (Pulkovo Obs. Circ., No. 8, 1934). In addition, Luyten recomputed elements from the results of both these investigations and Lucy & Sweeney have computed a circular orbit for the system. Although Bolton and Geffken retain a small eccentricity, the epoch given is T0. The values given for K1 by Harper and by Bolton and Geffken differed by nearly 6 km/s. The new value agrees very closely with Albitzky's. The reason for Harper's lower value is unclear. Despite the very small eccentricity, there is some evidence for apsidal motion in a period of 260y. Values of omega are bound to be poorly determined, however, and values at only two epochs are insufficient to enable a conclusion to be drawn. System1382Orbit1End System1383Orbit1Begin The results obtained by Popper certainly supersede those of J. Sahade and C.U. Cesco (Astrophys. J., 102, 128, 1945), which included appreciably smaller velocity amplitudes. The new values of K1 and K2, however, are well determined. The orbit is assumed circular and the epoch is the time of primary minimum. The spectral classifications are taken from Sahade and Cesco, and that for the secondary depends partly on photometric evidence. Popper gives a mean spectral type of A3, a visual magnitude difference of 0.19 and log T eff of 3.948 and 3.911. Photometric observations have been published by E.G. Ebbighausen, G. Penegor and P. Straton (Publ. Astron. Soc. Pacific, 87, 795, 1975) and C.D. Kandpal and J.B. Srivastava (Bull. Astron. Inst. Csl, 21, 345, 1970). The former were re-analyzed by Popper who, in addition to the results already quoted, found an orbital inclination close to 85 deg, and by B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978), who found similar results. The system has also been discussed by M. Kitamura and Y. Nakamura (Ann. Tokyo Obs., 21, 229, 1986). System1383Orbit1End System1384Orbit1Begin Glazunova gives orbital elements derived from measures of lines of hydrogen, helium and `light elements'. In the Catalogue we have given the last-named. The epoch appears to be a time of minimum. L.V. Glazunova and V.G. Karetnikov (Astron. Zh., 62, 938, 1985) have published another study of this star, based on the same material, and give spectral types of B1.5 II-III and B1.1 III-V. The light-curve suggests that the spectroscopic eccentricity is spurious and this is in accord with the evidence for gas- streaming found by Glazunova and Karetnikov. V. Harvig (Publ. Tartu Astrophys. Obs., 48, 177, 1981) published two-colour photoelectric observations of this system which were re-analyzed by G. Giuricin, F. Mardirossian and M. Mezzetti (Mon. Not. Roy. Astron. Soc., 211, 39, 1984). They found it difficult to obtain photometric elements and concluded that the less luminous star is the more massive. They drew attention to some discordance in the literature about the luminosity class of the primary component and assigned an effective temperature corresponding to a middle or late B-type to the secondary. They derive an orbital inclination of 90 deg and a fractional luminosity (in V) for the primary component of 0.85. System1384Orbit1End System1385Orbit1Begin See note for BD+52 3135. This is the preceding star of a pair. System1385Orbit1End System1386Orbit1Begin The spectroscopic observations are few in number and concentrated at the two nodes. The orbit is assumed circular, in accordance with the light-curve. The epoch is the time of primary minimum. Photometric measurements are published in the same paper and the spectral types appear to be at least partly based on them. The orbital inclination is found to be close to 86 deg and the visual magnitude difference between the components is about 1.5m. System1386Orbit1End System1387Orbit1Begin The original determination of orbital elements was by S.N. Hill (Publ. Dom. Astrophys. Obs., 3, 358, 1926) who found P=10.9114d. The period was revised by van Albada and Klomp in the light of two new series of observations from the McDonald Observatory and one from Mount Wilson. They also computed the new elements which are given here. Somewhat different elements are obtained from the newer observations, and those from the Victoria spectrograms are preferred because those spectrograms are the only ones on which the secondary spectrum can be resolved. The velocity-curves derived from the other observations show asymmetries that can be ascribed to an unresolved secondary spectrum. Hill gave K2=129.4 km/s, and van Albada and Klomp derived m2/m1=0.69 (implying a similar value). In view of the determination by Petrie(II) Delta m=2.74, however, the value of K2 is probably only approximately known. System1387Orbit1End System1388Orbit1Begin Several studies of this system have been published since the Seventh Catalogue and that by Stickland et al. seems to us the most thorough, both spectroscopically and photometrically. Also important are the work of K.-C. Leung, A.F.J. Moffat and W. Seggewiss (Astrophys. J., 265, 961, 1983) and B.S. Shylaja (J. Astrophys. Astron., 7, 171, 1986); while more restricted studies have been published by V.S. Niemela (I.A.U. Symp. No. 88, p. 177, 1980) and T. Kartasheva and L.I. Shnezhko (Bulletin Abastumani Obs., No. 58, 25, 1985). D.B. McLaughlin (Publ. Astron. Soc. Pacific, 53, 328, 1941) saw absorption features in the spectrum that he ascribed to an early-type companion. In the first orbital study published, W.A. Hiltner (Astrophys. J., 99, 273, 1944) was unable to confirm the existence of these features -- in agreement with the new findings of Stickland et al. Leung et al. did see violet-displaced absorption features, but found them to vary in phase with the emission lines, thus ruling out the possibility of their origin in the secondary star. Although the orbital elements found by both Stickland et al. and Leung et al. appear to be fairly well-determined, agreement between them is only rough. There are the usual (for a W-R star) line-to-line differences; the elements given here are derived from measures of the N IV emission line at lambda 4058. Leung et al. give K1=310 km/s and V0=60 km/s +/-5 km/s for the same line. The differences, though larger than one would like, are not significant -- a somewhat discouraging reflection on the status of our knowledge of these systems. The orbit is assumed circular and the epoch is the time of primary minimum. Although Stickland et al. have obtained multicolour photoelectric measurements, variations and distortions in the light-curve indicate that it is premature to attempt a detailed photometric analysis. An infrared excess in the light of the system has been detected by J.A. Hackwell et al. (Astrophys. J., 192, 383, 1974). The system probably belongs to the Cep OB1 association. System1388Orbit1End System1389Orbit1Begin The epoch is T0 for the primary component. Spectral type is approximate. From mass-luminosity relation, Delta m=0.69. No measures have been made, but appearance of spectra suggests a smaller Delta m. Herbig and Moorhead searched for eclipses, but no eclipse as deep as 0.02m was found. System is brighter member of a visual binary. The companion 11.44m at 23.5" is considered by Herbig and Moorhead to be physically connected with the spectroscopic pair. System1389Orbit1End System1390Orbit1Begin This is A.D.S. 16138 with a known orbit of period 30 y (D.L. Harris III, Astron. J., 52, 151, 1947) and periastron at 1979.8. The elements given for the long-period orbit are derived from this visual orbit except, of course, for V0, K1 and K2, which still depend on rather few spectroscopic observations. The two visual components are nearly equal, but component B is a spectroscopic binary and Duquennoy estimates, from two marginal detections of its secondary, that the spectral types are as given in the Catalogue. The inclination of the long-period orbit is about 85 deg. The less massive component of the visual pair is found to be the brighter, and even the short-period pair should be resolvable by speckle interferometry. The value of V0 for the short-period pair is, of course, variable. System1390Orbit1End System1391Orbit1Begin This is A.D.S. 16138 with a known orbit of period 30 y (D.L. Harris III, Astron. J., 52, 151, 1947) and periastron at 1979.8. The elements given for the long-period orbit are derived from this visual orbit except, of course, for V0, K1 and K2, which still depend on rather few spectroscopic observations. The two visual components are nearly equal, but component B is a spectroscopic binary and Duquennoy estimates, from two marginal detections of its secondary, that the spectral types are as given in the Catalogue. The inclination of the long-period orbit is about 85 deg. The less massive component of the visual pair is found to be the brighter, and even the short-period pair should be resolvable by speckle interferometry. The value of V0 for the short-period pair is, of course, variable. System1391Orbit1End System1392Orbit1Begin The new observations are in substantial agreement with older ones analyzed by A. McKellar (Publ. Dom. Astrophys. Obs., 6, 369, 1937). There is little to choose between the two sets of elements. The values of e and omega differ somewhat, but e is so small that this is probably not significant. Indeed, Lucy & Sweeney adopt a circular orbit. The star is the brighter member of A.D.S. 16143: B is 10.8m at 15.5". System1392Orbit1End System1393Orbit1Begin The observations by Bond et al. supersede those obtained by R.F. Sanford (Astrophys. J., 74, 209, 1931), which were more affected by blending of the spectral lines of the two components. Of the two sets of orbital elements given by Bond et al., we have adopted that based entirely on Lick Observatory spectrograms. The two components have nearly equal spectra and masses. Bond et al. recommend a search for eclipses. System1393Orbit1End System1394Orbit1Begin The spectra of the two components are of equal intensity in the combined light of the system. Imbert therefore deduced that the period is double that derived by S. Gaposchkin (Ann. Harv. Coll. Obs., 113, No. 2, 1953) from a photographic light-curve. From the depths of the two equal eclipses (as given by Gaposchkin for the `primary' minimum), Imbert estimates i=86.2 deg. System1394Orbit1End System1395Orbit1Begin This is a visual binary (A.D.S. 16173) whose components are not resolved on the slit-head (a=0.3"). The spectral types given are estimated from the observed combined colours, the probable magnitude difference and the parallax and are not direct M-K classifications. The period and time of periastron passage were determined by P. Baize (J. Observateurs, 40, 17, 1957), from the visual observations, to be 20.93y and 1983.86 respectively. Since the spectroscopic observations suggest that the periastron passage occurred about 0.3y early, either or both of these figures should be modified. The elements omega and e are also taken from Baize's visual orbit and may be only preliminary. The value given for K1 is in fact a value of K1+K2 and this should be remembered in interpreting the mass-function. The mass-ratio is estimated to be 0.8. The value of V0 is only a rough estimate from measures of the combined spectrum at phases when its components are unresolved. Visual estimates of the difference in the magnitudes of the two components range widely about a mean of roughly 0.5m. Spectrophotometry suggests that the difference may be closer to 1.0m. The stars definitely lie above the main-sequence. There is also an 11.6m companion at 70", which seems likely to be optical. System1395Orbit1End System1396Orbit1Begin The spectral type is that given by H.L. Johnson and W.W. Morgan, as quoted by P. van de Kamp and J.E. Damkoehler (Astron. J., 62, 393, 1957) who have derived a photocentric orbit. The Bright Star Catalogue gives the spectral type as G2 II-III + F0 V. Van de Kamp and Damkoehler find a=0.022" and i=82 deg. The system is the brightest component of A.D.S. 16211: four other components are listed in I.D.S. The light of the star has been suspected of variability. System1396Orbit1End System1397Orbit1Begin The secondary spectrum is seen at primary minimum. The elements are approximate and V0 may be affected by guiding errors. A V light-curve was published by C.D. Kandpal and J.B. Srivastava (Bull. Astron. Inst. Csl, 18, 265, 1967) who found an orbital inclination of 88.5 deg and a fractional luminosity of 0.93 for the primary component. Koch et al. pointed out that this implied unusual properties for a secondary component of the observed spectral type. A new analysis of the light-curve by B. Cester et al. (Astron. Astrophys. Supp., 33, 91, 1978) yields similar results to the original one. The star is the brightest member of A.D.S. 16252: companions are 10.2m at 3.5" and 10.3m at 20.6". System1397Orbit1End System1398Orbit1Begin The epoch is the time of primary minimum. A circular orbit was assumed although the light-curve indicates e=0.039 and apsidal motion in a period of 42.3y is well established (I. Semeniuk, Acta Astron., 17, 223, 1967). The orbital elements are derived from measures of metallic lines, including the K line, since the hydrogen lines of the two component spectra are strongly blended with each other. Even so, some large residuals remain. Semeniuk (loc. cit.) analyzed her two-colour photoelectric observations, which were also discussed by M. Mezzetti et al. (Astron. Astrophys. Supp., 42, 15, 1980). The light-curve was further studied by R.A. Botsula (Izv. Engelhardt Obs. Kazan, 47, 19, 1981) and M. Kitamura and Y. Nakamura (Ann. Tokyo Obs., 21, 229, 1986). The most recent discussion, however, is of new UBV observations by R.E. Wilson and E.J. Woodward (Astrophys. Space Sci., 89, 5, 1983). Their results for the orbital inclination (85 deg) and fractional luminosity in V of the primary (0.53) are similar to Semeniuk's, but they draw attention to distortions and possible variations in the light-curve. System1398Orbit1End System1399Orbit1Begin Pearce estimated i=62 deg from the mass-luminosity relation and predicted that the system would show eclipses. G. Hill et al. (Publ. Dom. Astrophys. Obs., 15, 1, 1976) found some light variation, and their conclusion that the star is an ellipsoidal variable has been confirmed by more complete observations by H.C. Lines et al. (Inf. Bull. Var. Stars, No. 2932, 1986). They also find that the eccentricity is close to zero (<=0.05), in contrast with the spectroscopic result. A new orbital study is desirable. A brief account of a polarimetric, photometric and spectrophotometric study of the system has been published by M.F. Corcoran (Bull. Am. Astron. Soc., 19, 714, 1987). Spectrograms obtained with IUE show evidence of mass-loss from the system. Petrie(II) found Delta m=0.28. The star is a member of N.G.C. 7380. System1399Orbit1End System1400Orbit1Begin See note for BD+52 3135. The scatter of observations about the velocity-curve is large. This is the last binary of the group in the Perseus arm investigated by Abt et al.. System1400Orbit1End System1401Orbit1Begin Although the new discussion by Bell, Hilditch and Adamson certainly supersedes the older one by J.A. Pearce (J. Roy. Astron. Soc. Can., 29, 413, 1935), the observations are few and their scatter still fairly large. The orbit is assumed circular, in accordance with the light-curve, and the epoch is the time of primary minimum. The value of K2 is uncertain: that given excludes one poor observation whose inclusion would lead to K2=291 km/s. Discordant spectral classifications have been made and types of O8 + O9 are possible and, in some respects, lead to a more consistent picture of the system. Stromgren photometry by Bell, Hilditch and Adamson also supersedes the previous best available work by C.M. Huffer and O.J. Eggen (Astrophys. J., 106, 313, 1947). The orbital inclination is close to 69 deg and the visual magnitudes of the two components differ by about 0.3m. System1401Orbit1End System1402Orbit1Begin The epoch is T0 and a circular orbit was assumed. Lucy & Sweeney also adopted a circular orbit. Harper adopted an arbitrary T, a quarter of a period before T0. A misprint in his original value was corrected in a later paper (Publ. Dom. Astrophys. Obs., 6, 251, 1935) in which he also revised P to 24.649d. System1402Orbit1End System1403Orbit1Begin The epoch appears to be the time of superior conjunction of the primary star. The spectrum of the primary shows mercury and manganese lines, that of the secondary shows mercury lines. Except for the period, the elements of the orbit of the secondary star were derived independently of those of the primary. The small disagreements in e, omega, and V0 are not significant. System1403Orbit1End System1404Orbit1Begin This star belongs to the Sr-Cr family of Ap stars. Detailed analysis of its spectrum has been published by S.J. Adelman (Astrophys. J., 183, 95, 1973, Astrophys. J. Supp., 26, 1, 1973). Floquet discusses the 17.22d variation in terms of the oblique-rotator model. The orbital elements are only approximate and depend only on measures of the K line. It is not quite clear what is taken as the epoch, but it appears to be related to the rotational period rather than the orbital. System1404Orbit1End System1405Orbit1Begin The spectral types are those assigned by A.B. Wyse and quoted by Struve: modern sources suggest a somewhat later type (G5 to G8). The epoch is T0 and the orbit is assumed circular. An error for the values given for the minimum masses was corrected by Struve in a later paper (Astrophys. J., 116, 81, 1952). He also reported changes in the relative intensities of the two components during the orbital period. Like those of many W UMa systems, the light-curve is variable, and rather differing solutions have been published. A useful summary discussion was presented by B.B. Bookmyer (Astron. J., 70, 415, 1965). Several new studies have been published, many based on new observations: P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978 and Astron. Astrophys. Supp., 67, 365, 1987), K.-C. Leung, D.-S. Zhai and R-X Zhang (Publ. Astron. Soc. Pacific, 96, 634, 1984), L. Binnendijk (ibid., 646, 1984), and J.A. Eaton (Acta Astron., 36, 79, 1986). Most investigators find an orbital inclination close to 80 deg and nearly equal luminosities for the two components in V, but a range of values has been published, especially for the relative luminosity. The IUE spectrum has been studied by S.M. Rucinski et al. (Mon. Not. Roy. Astron. Soc., 208, 309, 1984) but no modern spectroscopic orbit is available: one is much needed. The system is an X-ray source (R.G. Cruddace and A.K. Dupree, Astrophys. J., 277, 263, 1984). System1405Orbit1End System1406Orbit1Begin Abt and Levy give the spectral type as A2, A8, F2 from the K line, hydrogen lines and metallic lines respectively. The maximum of the velocity-curve is not covered by the observations and therefore the elements are uncertain. The star is the brightest member of A.D.S. 16345. The companion B (7.8, F6 V) revolves in an orbit about the primary with a period of 104.5y and a major semi-axis of 0.65". The companion C (10.7m at 28.0") is optical, according to Abt and Levy. System1406Orbit1End System1407Orbit1Begin This is the first of a group of systems in the association Cep OB 3 studied by Garmany. The elements of this system are only approximate. The observations show a fairly large scatter about the velocity-curve. System1407Orbit1End System1408Orbit1Begin This is a binary system containing a degenerate star and exhibiting slow X-ray pulsations. The epoch is T0 and the orbit is assumed circular. The elements given are derived from measures of the emission peaks of He II -- which give the most self-consistent results. The scatter of observations is very large, however. System1408Orbit1End System1409Orbit1Begin Fitch's observations supersede the earlier work of O. Struve and N.T. Brobrovnikoff (Astrophys. J., 62, 139, 1925) and O. Struve et al. (Astrophys. J., 116, 81, 1952). The results of these investigations are in substantial agreement and it now seems well established that this beta CMa variable (primary pulsation period 0.17d) is also a spectroscopic binary. The star is now known to be an eclipsing variable (depth of eclipse about 0.04m). M. Jerzykiewicz (Inf. Bull. Var. Stars, No. 1552, 1979) estimates an orbital inclination near 84 deg and a mass-ratio not much over 0.1 The star is also the brighter component of A.D.S. 16381: B is 11.5m at 55.9". System1409Orbit1End System1410Orbit1Begin This is another of the binaries in Cep OB 3 (see note for HD 216711). Only the period is really known. Some plates show two spectra and the approximate value of K is derived from the isolated measures of the secondary spectrum. On most plates both spectra are blended. No value was given for the epoch. System1410Orbit1End System1411Orbit1Begin The secondary spectrum is described as `considerably weaker than the primary'. The light-curve suggests that the orbit is circular. Eclipses were discovered and the period determined by W. Strohmeier, R. Knigge and H. Ott (Veroff. Remeis-Sternw. Bamberg, 5, No. 13, 1962). Photographic light-curves in two colours were obtained by I.I. Bondarenko and J.I. Tokareva (Peremm. Zvezd. Pril., 2, 171, 1975) and analyzed both by them and by G. Giuricin, F. Mardirossian and M. Mezzetti (Astron. Astrophys. Supp., 49, 89, 1982). Photoelectric UBV light-curves have been published and analyzed by C. Bartolini, A. Bonifazi and L. Milano (Astron. Astrophys. Supp., 55, 403, 1984). They find an orbital inclination close to 77 deg and a fractional luminosity (in V) for the brighter component of 0.75. System1411Orbit1End System1412Orbit1Begin The discussion by Heard and Fernie is more detailed than the original one by Heard alone (in I.A.U. Symp. No. 30, p. 219, 1967) although the elements derived are the same. The only worrying feature is the large unexplained difference found for the two values of V0. Heard and Fernie found Delta m appox 1.0 at lambda 4500 by Petrie's method. Although they looked for eclipses, they were unable to detect them. Several independent investigators were successful somewhat later, however (N.K. Rao, Publ. Astron. Soc. Pacific, 84, 563, 1972; K. Madore and J.R. Percy, ibid., 85, 319, 1973; C.D. Scarfe and D.J. Barlow J. Roy. Astron. Soc. Can., 68, 96, 1974). J.D. Fernie (Astrophys. J., 183, 583, 1973) estimates a minimum value of i=77 deg, and a probable value of about 85 deg. Further photometric information has been published by C.D. Scarfe (J. Roy. Astron. Soc. Can., 73, 258, 1979). System1412Orbit1End System1413Orbit1Begin This is another binary member of the association Cep OB 3 (see note for HD 216711). The eccentricity is described by Garmany as probably spurious, an effect of gas streams within the system. This would be consistent with the large scatter of observations, although the value of omega is not in the quadrant usually associated with that kind of distortion of the velocity-curve. System1413Orbit1End System1414Orbit1Begin This is another binary in the Cep OB 3 association (see note for HD 216711). Garmany believes the orbital eccentricity derived for this system to be spurious also. The scatter of the observations about the velocity-curve is relatively small, however. System1414Orbit1End System1415Orbit1Begin Although the secondary spectrum may arise from a shell, the binary nature of this star is attested by speckle interferometry (H.A. McAlister and F.C. Fekel, Astrophys. J. Supp., 43, 327, 1980 and other references given by Pastori et al.). Two completely different sets of orbital elements have been published. Neither is completely convincing, but the short period combined with a high eccentricity (and the giant classification for the primary) required by M. Singh (Inf. Bull. Var. Stars, No. 2284, 1983, Astrophys. Space Sci., 100, 13, 1984) seems to us implausible, while the 23.5y period proposed by Pastori et al. fits what we know about the system (see also J. Horn et al. I.A.U. Symp. No. 98, p. 315, 1982). System1415Orbit1End System1416Orbit1Begin An earlier investigation was published by W. Buscombe and P.M. Morris (Mon. Not. Roy. Astron. Soc., 123, 183, 1961) who noted that early Cape observations deviated from their velocity-curve. Bopp et al. have shown that the period is only half that found by Buscombe and Morris, and have thus improved the orbital elements. There is still evidence of systematic difference between velocities obtained at different observatories, however. System1416Orbit1End System1417Orbit1Begin This is another of the binaries in the Cep OB 3 association investigated by Garmany who points out that the secondary spectrum is seen on some spectrograms and that therefore measures on others may be affected by blending. See also note for HD 216711. System1417Orbit1End System1418Orbit1Begin This is another binary in the Cep OB 3 association (see note for HD 216711). Although the observations define the velocity-curve fairly well, they show appreciable scatter at some phases. System1418Orbit1End System1419Orbit1Begin Elements for this system were first derived by R.M. Petrie (Publ. Dom. Astrophys. Obs., 7, 305, 1947) who also derived Delta m=0.3. Popper's observations lead to somewhat higher values of K1 and K2 than Petrie found. The epoch is the time of primary minimum. Popper adopted the small eccentricity found photometrically (I.-S. Nha, Astron. J., 80, 232, 1975) and the apsidal period of about 39 y that Nha also determined -- omega=9.39deg(t-1949.5). Two recent discussions of the light-curve were published by S. Soderhjelm (Astron. Astrophys. Supp., 25, 151, 1976) and B. Cester et al. (ibid., 33, 91, 1978). Soderhjelm found an orbital inclination close to 82 deg and a visual magnitude difference between the components of 0.23m -- figures confirmed by Cester et al. Nha mentions a companion, about 5m fainter than the eclipsing pair, and separated by 20". It is not listed in I.D.S. The system is a member of Cep OB 3. System1419Orbit1End System1420Orbit1Begin Orbital elements were first published by V.A. Albitzky (Izv. Krym. Astrofiz. Obs., 4, 78, 1949). R. Bouigue and J.-L. Chapuis (Ann. Obs. Toulouse, 23, 37, 1955) improved his elements, but pointed out that the observations could be satisfied nearly as well by a period of 1.83748d. The new observations by Thomson and Bolton remove this possibility, lead to a slight revision of Albitzky's value for the period, confirm his value of K1, and indicate that the orbit is more nearly circular. The epoch is T0. System1420Orbit1End System1421Orbit1Begin This is the fifth radio pulsar known to be in a binary system. Neither magnitude nor spectral type are available. The quantity K1 is inferred from the measured a sin i of 32.6905 light-seconds (approx. 9.8E6 km). The value of V0, of course, cannot be determined. Both components are believed to be collapsed objects. The high eccentricity should enable apsidal motion to be readily detected and the total mass of the system to be determined. System1421Orbit1End System1422Orbit1Begin This is the last binary in the Cep OB 3 association studied by Garmany (See note for HD 216711). The observations show an appreciable scatter about the velocity-curve. System1422Orbit1End System1423Orbit1Begin The first determination of orbital elements was by R.K. Young (Publ. Dom. Astrophys. Obs., 1, 239, 1920). Further determinations were made by R.M. Petrie (Publ. Dom. Astrophys. Obs., 10, 459, 1959), O. Struve et al. (Astrophys. J., 129, 314, 1959), and R.M. Petrie and J.K. Petrie (Publ. Dom. Astrophys. Obs., 13, 111, 1967). R.M. Petrie pointed out the apparent rotation of the line of apsides, and he and J.K. Petrie give a value of 156 y for the apsidal period. Extensive recomputations and some new observations are published by van Albada and Klomp, and the set of elements accepted for inclusion in the Catalogue is derived from their 1954 McDonald series. There are some differences in V0 between the different series which probably are not significant, and some between values of K1 which are more worrying. The extreme range of K1 is from 78 km/s to 100.5 km/s. If, however, these two extreme values are ignored (one from Victoria, the other from Mount Wilson) the remaining values are all between 86 km/s and 92 km/s. The secondary spectrum may be a contributory factor to this confusion. Petrie found Delta m=2.0 and estimated the mass-ratio to be 0.58; Struve et al. estimated the mass-ratio to be 0.43. The spectral type of the secondary is uncertain -- either B or A. According to van Albada and Klomp the evidence for apsidal motion depends heavily on Young's orbit. New observations in the next few years would be worthwhile. System1423Orbit1End System1424Orbit1Begin The elements given in the Catalogue are improvements of those found by S.L. Boothroyd (Publ. Dom. Astrophys. Obs., 1, 281, 1921) based on new observations. Petrie(II) found Delta m=2.14. System1424Orbit1End System1425Orbit1Begin The new elements obtained by Scarfe et al. supersede those derived by W.E. Harper (Publ. Dom. Astrophys. Obs., 3, 204, 1925; 6, 251, 1935) and the additional observations derived by H.A. Abt, N.B. Sanwal and S.G. Levy (Astrophys. J. Supp., 43, 549, 1980). The spectral type of the primary component may be a little later than G2 III. The invisible secondary cannot be a normal main-sequence star and Scarfe et al. advance arguments for supposing that it may be a short-period binary. The star is the brightest component of A.D.S. 16538, which has an orbital period of 150 y and a major semi-axis of 0.86" (there is also a component C: 12.2m at 58.6"). The systemic velocity of A is, of course, variable. Scarfe et al. show that the two available determinations of V0 fit well the orbital elements derived for the visual pair by either P. Muller (Bull. Astron. Paris, 16, 210 and 351, 1952) or G. van Biesbroeck (Publ. Yerkes Obs., 8, 371, 1954), if V0 (triple system) is 18.7 km/s and KA=1.9 km/s. Their conclusion is tentative, however, because the systematic correction needed between the two determinations of V0 in the 557 d orbit is uncertain. Speckle interferometry (H.A. McAlister and F.C. Fekel, Astrophys. J. Supp., 43, 327, 1980) yields results that do not agree with the presently adopted visual orbit. System1425Orbit1End System1426Orbit1Begin The elements given in the Catalogue supersede those published by J. Lunt (Cape Annals, 10, pt. 7, 9G, 1924). System1426Orbit1End System1427Orbit1Begin This system is a BY Dra variable. The two absorption components of the spectrum both have very closely the same strength, although there is a suspicion of variability of one of them with phase. Both components show central emission at H and K. There is no evidence for any difference between the velocities derived from the absorption lines and those from the emission lines. The system is the fainter member of A.D.S. 16557: A is 6.6m at 15.4" and spectral type G5. System1427Orbit1End System1428Orbit1Begin The epoch is the time of minimum. The small eccentricity is confirmed by the photometric observations and apsidal motion with a period of approximately 90 years has been detected (A. Gimenez and T.E. Margrave, Astron. J., 87, 1233, 1982). The element omega varied from 187 deg to 247 deg in the interval of spectroscopic observation. Popper has analyzed two-colour photoelectric observations (approximately BV) made by C. Ibanoglu (Astron. Astrophys., 35, 483, 1974) and derives an orbital inclination close to 85 deg and a fractional luminosity (in V) for the brighter star of 0.51. System1428Orbit1End System1429Orbit1Begin The secondary spectrum was seen on only five spectrograms, so the values of K2, m1sin^3i and m2sin^3i are very uncertain. A modern spectroscopic study is highly desirable. The earliest attempts to analyze the light-curve (K.C. Gordon, Astron. J., 60, 422, 1955) encountered difficulties and the night-to-night variations, asymmetric eclipses and variable period were all confirmed by C.A. Dean (Publ. Astron. Soc. Pacific, 86, 912, 1974). The system, now recognized as one of the RS CVn group has continued to attract the attention of photometrists. New observations or studies have been reported by L. Milano, G. Russo and S. Mancuso (Astron. Astrophys., 103, 57, 1981), S. Mancuso et al. (in Photometric and Spectroscopic Binary Systems, p. 313, 1981), B. Cester et al. (Astron. Astrophys. Supp., 32, 351, 1978), S. Mancuso, L. Milano and G. Russo (ibid., 36, 415, 1979) and S. Mancuso et al. (Astrophys. Space Sci., 66, 475, 1979). Values for the orbital inclination and the fractional luminosity of the primary star are partly model dependent, but most authors find about 87 deg and between 0.8 and 0.9 (in V) respectively. System1429Orbit1End System1430Orbit1Begin The epoch is T0 for the primary star and a circular orbit is assumed. Different observers do not agree about the photometric elements, and the light-curve of this W UMa system is variable: F. Hinderer (J. Observateurs, 43, 161, 1960) postulated a luminous cloud in the system. More recent photometric studies are by P.V. Rigternik (Astron. Astrophys. Supp., 12, 313, 1973), P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978), S.A. Bell, R.W. Hilditch and D.J. King (Mon. Not. Roy. Astron. Soc., 208, 123, 1984), S.J. Lafta and J.F. Grainger (ibid., 127, 153, 1986) and H. Rovithis-Livaniou and P. Rovithis (Astron. Nachr., 307, 17, 1986). Values derived for the orbital inclination range from 74 deg to 87 deg, and for the fractional luminosity of the primary star in V, from 0.65 to 0.77. System1430Orbit1End System1431Orbit1Begin This star is A.D.S. 16591 and the long period (29.5y) is taken from the visual orbit by P. Baize (J. Observateurs, 38, 37, 1955). Also adopted from this orbit was the eccentricity (0.40), but the time of periastron passage (1982.7) has been adjusted with the help of the spectroscopic observations. The spectral type given for the secondary component of the close pair is an estimate only: the spectrum has not been seen, and the star is estimated to be more than four magnitudes fainter than its primary. The two components of the visual pair differ by about 0.3m in V. The orbital inclination of the visual pair is 112 deg. The value of V0 for the short-period pair is variable. System1431Orbit1End System1432Orbit1Begin This star is A.D.S. 16591 and the long period (29.5y) is taken from the visual orbit by P. Baize (J. Observateurs, 38, 37, 1955). Also adopted from this orbit was the eccentricity (0.40), but the time of periastron passage (1982.7) has been adjusted with the help of the spectroscopic observations. The spectral type given for the secondary component of the close pair is an estimate only: the spectrum has not been seen, and the star is estimated to be more than four magnitudes fainter than its primary. The two components of the visual pair differ by about 0.3m in V. The orbital inclination of the visual pair is 112 deg. The value of V0 for the short-period pair is variable. System1432Orbit1End System1433Orbit1Begin The discussion by S. Jakate et al. is a revision and improvement of earlier results published by two of the same authors (G.A. Bakos and J.F. Heard, Astron. J., 63, 302, 1958). The system displays many of the features associated with the RS CVn group -- variable period and light-curve, an asymmetric light-curve and H and K emission. The last of these is stable (E.J. Weiler, Mon. Not. Roy. Astron. Soc., 182, 77, 1978) but the same author found H-alpha emission to vary -- a conclusion confirmed by H.L. Nations and L.W. Ramsey (Astron. J., 85, 1086, 1980) and, even more strongly, by B.W. Bopp (ibid., 86, 771, 1981). The variations of the light-curve make its solution for photometric elements difficult. J.A. Eaton and D.S. Hall (Astrophys. J., 227, 907, 1979) introduce starspots to explain the phenomena. Other solutions are offered by J.A. Eaton et al. (Astrophys. Space Sci., 82, 289, 1982) and Z. Tunca (ibid., 105, 23, 1984). The orbital inclination appears to lie between 76 deg and 78 deg and the fractional luminosity of the cooler star (in V) between 0.72 and 0.75. System1433Orbit1End System1434Orbit1Begin A long history of puzzlement over the nature of this star has been described by Griffin and by S.B. Howell and B.W. Bopp (Publ. Astron. Soc. Pacific, 97, 72, 1985) and need not be repeated here. The orbit is assumed circular and the epoch is T0 for the `primary' component. This primary is the star whose spectrum shows the strongest trace on the spectrometer record; it appears to be marginally less massive, although the mass-ratio cannot be distinguished from unity when the observational uncertainties are taken into account. S.B. Howell et al. (Publ. Astron. Soc. Pacific, 98, 777, 1986) find the light of the star to vary by about 0.1m in V throughout the orbital period. They regard the system as an RS CVn binary with the primary rotating synchronously. System1434Orbit1End System1435Orbit1Begin The orbit was assumed circular after a preliminary solution showed that the eccentricity (less than 0.02) was smaller than its own eccentricity. The epoch is T0 for the primary star. The difference in the values of V0 for the two components is unexplained; presumably the value found from the primary spectrum is the more reliable. Eclipses have been detected. System1435Orbit1End System1436Orbit1Begin A more detailed paper by Ouhrabka cited by G. Scholz, E. Gerth and K.P. Panov (Astron. Nachr., 306, 329, 1985) is not available in Victoria. Scholz et al. discuss the possibility of a short-period (0.1d) periodicity in the light variation of the star. System1436Orbit1End System1437Orbit1Begin The first orbital elements were derived by R.K. Young (Publ. Dom. Astrophys. Obs., 4, 83, 1917) whose results were recomputed by Luyten. Elements have also been derived by A. Young (Publ. Astron. Soc. Pacific, 86, 63, 1974). All three orbits are based on spectrograms of moderate dispersion, but Cester's is based on the most observations and his show the least scatter. Recently, M. Kitamura, Y. Nakamura and A. Yamasaki (Ann. Tokyo Obs. 2nd. Ser., 19, 361, 1983) have published orbital elements derived from observations fewer in number than Cester's, but of higher dispersions. They (probably correctly) assume a circular orbit and derive K1=70.3 km/s and V0=7.6 km/s -- both results agreeing with Cester's within the uncertainties. Thus A. Young's suggestion of a third body to account for his deviant value of V0 now seems less plausible. The photoelectric observations obtained by C.M. Huffer (Publ. Washburn Obs., 15, 117, 1928) are superseded by UBV observations obtained by M. Kitamura et al. (Tokyo Astron. Bull, 2nd Ser., No. 266, 3021, 1982) and analyzed in the Ann. Tokyo Obs. paper cited above. The orbital inclination is found to be 65 deg and the fractional luminosity (in V) of the primary component lies between 0.74 and 0.78. There is evidence for variation in the metallicity of the primary component during eclipse, indicating a non-uniform distribution of absorption, in the lines of metals, over the surface of the star. Reference: B.Cester, Trieste Contr.,, No. 287, 1959 System1437Orbit1End System1438Orbit1Begin The epoch is T0. Sarma notes that the probable error of a single velocity (1.2 km/s) is large for spectrograms of this type of star obtained with the Mills spectrograph, and he suggests some additional cause of velocity variation may be acting. Lucy & Sweeney adopt a circular orbit. The star is the brighter member of A.D.S. 16672: B is 7.5m at 13.0" and shares the proper motion of A. System1438Orbit1End System1439Orbit1Begin The star is the brighter member of A.D.S. 16681; companion is 11.9m at 17.5". Griffin regards it as probably a physical companion and estimates that it is probably a late F or early G main-sequence star. System1439Orbit1End System1440Orbit1Begin Slightly different values of P and T are found from measures of each component. Gies and Bolton find Delta m=0.61, by Petrie's method. The star may be slightly variable. System1440Orbit1End System1441Orbit1Begin System1441Orbit1End System1442Orbit1Begin Martin, Jones and Smith give an elliptical orbital solution as well as a circular one. The eccentricity appears to be formally significant and the observations are represented better by an eccentric orbit, but it seems unlikely that the orbit of a dwarf nova would be other than circular, and the circular solution is given in the Catalogue. The value of K2 is not much affected (note it is K2), the orbital elements refer to the red-dwarf secondary. The epoch is the time of primary minimum. Martin, Jones and Smith also publish the results of infrared photometry. Other photometric observations have been published by V.B. Goranskij et al. Inf. Bull. Var. Stars, No. 2653, 1985), by J. Wood and C.S. Crawford (Mon. Not. Roy. Astron. Soc., 222, 645, 1986) who find the orbital inclination to lie between 81 deg and 90 deg, and by P. Szkody and M. Mateo (Astron. J., 92, 483, 1986). System1442Orbit1End System1443Orbit1Begin The system is of interest because both components appear to be metal deficient, although its space velocity is small. The F8 spectral type is derived from the hydrogen lines. The K line, and lines of Fe I and Fe II indicate a spectral type of F5, while the lines of Ca I and Sr II indicate F4. Both components have similar spectra and are closely similar in luminosity. The small orbital eccentricity probably should be ignored. System1443Orbit1End System1444Orbit1Begin The period of this cataclysmic variable is still uncertain and different emission lines give different orbital elements. The elements given in the Catalogue are derived from measures of the bases of the hydrogen emission lines. The epoch is T0. System1444Orbit1End System1445Orbit1Begin New orbital elements have been derived by M. Gaida and W. Seggewiss (Acta Astron., 31, 231, 1981); they agree reasonably well with those obtained by Gorza and Heard (except that the newer value of the eccentricity is somewhat smaller) and there are few grounds for preferring one set of elements to the other. The observations by Gorza and Heard cover the velocity-curve a little more uniformly. On the other hand, the work of Gaida and Seggewiss reduces the plausibility of both the relatively rapid apsidal motion suggested by R.M. Petrie (Astron. J., 51, 22, 1946 and Astronomical Techniques ed. W.A. Hiltner, Chicago University Press, 1962, p. 569), and the third body suggested by A.H. Batten (J. Roy. Astron. Soc. Can., 55, 120, 1961). Earlier spectroscopic observations were published by R.H. Baker (Publ. Allegheny Obs., 2, 28, 1910 -- rediscussed by Gaida and Seggewiss) and by W.J. Luyten, O. Struve and W.W. Morgan (Publ. Yerkes Obs., 7, pt. 4, 39, 1939). Although a slow revolution of the line of apsides is possible (period about 1,000 years), most spectroscopic observations give values of omega close to the photometric ones found by J. Stebbins (Astrophys. J., 54, 81, 1921), C.M. Huffer and G.W. Collins II (Astrophys. J. Supp., 7, 351, 1962) and S. Catalano and M. Rodono (Astron. J., 76, 557, 1971). Six- colour photometry by K.C. Gordon and G.E. Kron (Astrophys. Space Sci., 23, 403, 1973) leads to an estimate for the spectral type of the secondary of between A5 and A7. However, Koch et al. suggest A1. Huffer and Collins find an orbital inclination of 90 deg and a fractional luminosity (in yellow light) for the primary of 0.9. The system is the brightest component of A.D.S. 16795: the closest companion is 9.3m at 1.1". Six others are listed in I.D.S. System1445Orbit1End System1446Orbit1Begin The secondary spectrum is visible during partial eclipse. Lucy & Sweeney derive similar elements from these observations. K. Walter (Astrophys. Space Sci., 24, 189, 1973) has published photoelectric (BV) light-curves, and the V magnitudes given in the Catalogue. He finds that observations obtained immediately after each eclipse show a larger scatter than do those at other phases. Because of this, and because it is difficult to tell whether the primary eclipse is total or partial, a definitive solution of the light-curve is impossible. It appears that i is close to 87 deg and the brighter component contributes about 0.86 of the total light (in V). Similar results were obtained from the same observations by M. Mezzetti et al. (Astron. Astrophys. Supp., 39, 265, 1980). System1446Orbit1End System1447Orbit1Begin The duplicity of this star was first announced by G. Cayrel de Strobel (Astrophys. Letters, 1, 173, 1968) who commented that one spectrum is stronger and contains sharper lines then the other. The results of photometry on the Stromgren system suggest that the two components are metal deficient. This may, however, be an appearance caused by gas streams within the system. There is some evidence of systematic departures from the computed velocity-curve of velocities determined from the spectrum that shows more diffuse lines. System1447Orbit1End System1448Orbit1Begin According to Griffin, the radial-velocity traces indicate that the star is a giant. System1448Orbit1End System1449Orbit1Begin Similar elements have been computed from the same observations both by Luyten and by Lucy & Sweeney. Two faint and distant companions are listed in I.D.S. System1449Orbit1End System1450Orbit1Begin Earlier investigations were published by K. Burns (Lick Obs. Bull., 4, 87, 1906), E.L. Martin (Mem. Soc. Astron. Ital., 4, N.S. 93, 1927 -- a paper not available in Victoria, the elements are based on Ottawa observations) and J.A. Pearce (Publ. Am. Astron. Soc., 10, 312, 1943 -- confirmed by L. Gratton, Astrophys. J., 111, 31, 1950). Lucy & Sweeney adopt a circular orbit. Although its period is long, the system is now widely regarded as one of the RS CVn group. The H and K emission is variable (J.A. Eilek and G.A.H. Walker, Publ. Astron. Soc. Pacific, 88, 137, 1976) although the variation is not correlated with the orbital period. Several studies of the also variable UV spectrum have been published (J.L. Linsky et al., Nature, 275, 389, 1978, S.L. Baliunas and A.K. Dupree, Astrophys. J., 227, 870, 1979 and R. Glebocki et al., Acta Astron., 36, 369, 1986). Radio emission has been detected (G.T. Bath and G. Wallerstein, Publ. Astron. Soc. Pacific, 88, 759, 1976). A claim by M.S. Giampapa and L. Golub (Astrophys. J., 268, L121, 1983) to have detected a magnetic field has not been confirmed (G.W. Marcy and D.H. Bruning, ibid., 281, 286, 1984). The light of the star varies by about 0.4m in photographic light. Three companions are listed in I.D.S.: the closest is 13.0m at 47.5". System1450Orbit1End System1451Orbit1Begin Circular and elliptical orbits were computed for this system. The eccentricity found was marginally significant, but the circular orbit is adopted since it seems physically the more probable. The epoch is T0. If the primary component has a normal mass for an A1 dwarf, the mass-ratio of the system is less than 0.1. System1451Orbit1End System1452Orbit1Begin Lucy & Sweeney adopt a circular orbit. A new excellent BV light-curve has been published and analyzed by A. Bonifazi and A. Guarnieri (Astron. Astrophys., 156, 38, 1986). It supersedes all previous photometric work and also indicates that the true orbit is circular. Bonifazi and Guarnieri find an orbital inclination of about 82 deg and a visual magnitude difference between the components of 3.06m. They estimate that the secondary is K2 IV star filling its Roche lobe. A new spectroscopic study to match this photometric work is highly desirable. System1452Orbit1End System1453Orbit1Begin The binary nature of the star was first recognized by J.F. Heard (Publ. David Dunlap Obs., 2, 142, 1956). The lines of H and K are seen in emission. The epoch is T0. Fekel (private communication) has detected the secondary spectrum in the red. System1453Orbit1End System1454Orbit1Begin The orbital elements are very uncertain, but the symbiotic nature of the spectrum (late-type Mira variable and high-excitation emission lines) and possible eclipses (L.A. Willson, P. Garnavich and J.A. Mattei, Inf. Bull. Var. Stars, No. 1961, 1981) suggest that the star is a binary. Wallerstein adopted a period of 44 years, deduced photometrically with a supposed eclipse in 1977, and deduced the other elements which, however, lead to one large residual. There is also a jet associated with the star. The eccentricity is small. The value of V0 may be affected by sytematic error. System1454Orbit1End System1455Orbit1Begin Lucy & Sweeney also adopt a circular orbit. The orbital elements may have been affected by blending of the two component spectra. The F-type spectrum (seen in eclipse) has a K line of unusual appearance and there is probably emission at H-alpha. The epoch is T0. From visual observations A.B. Wyse (Lick Obs. Bull., 17, 37, 1934) found i to be close to 90 deg and the ratio of the light of the two components about 0.56. There appears to be no photoelectric light-curve. System1455Orbit1End System1456Orbit1Begin The orbit is assumed circular and the epoch is the time of primary minimum. From BV observations by D.M. Popper and P.J. Dumont (Astron. J., 82, 216, 1977), D.M. Popper and P.B. Etzel (ibid., 86, 102, 1981) derived an orbital inclination close to 88 deg and a fractional luminosity for the brighter star (in V) of 0.59. System1456Orbit1End System1457Orbit1Begin Lu's observations cover only one node of the orbit and the elements are therefore provisional. The observations were sudegcient to show that the true period is approximately double that found photometrically (T. Berthold, Inf. Bull. Var. Stars, No. 2192, 1982). The orbit is assumed circular and the epoch is the time of primary minimum. The values of K are estimated from Lu's graph. System1457Orbit1End System1458Orbit1Begin The epoch is T0 and a circular orbit was assumed (and confirmed by Lucy & Sweeney). P.P. Parenago and B.V. Kukarkin (Veranderliche Sterne Nishni-Novgorod, 5, 287, 1940) published a photographic light-curve and found i=55 deg and the ratio of luminosities of the two components is 0.25. System1458Orbit1End System1459Orbit1Begin Epoch is apparently the time at which the primary component's velocity is equal to the systemic velocity and is decreasing. A circular orbit was assumed. Petrie(II) found Delta m=0.10. System is brighter member of A.D.S. 17062: B is 11.5m at 4.6". System1459Orbit1End System1460Orbit1Begin Epoch is apparently the time at which the primary component's velocity is equal to the systemic velocity and decreasing (i.e. it should coincide with primary minimum). Struve wrote that the spectral type was `B8 in full light and perhaps A0 at mid-eclipse'. The K line is interstellar. Photoelectric UBV light-curves have been published by J.B. Srivastava and C.D. Kandpal (Astrophys. Space Sci., 66, 143, 1979). They derive an orbital inclination close to 76 deg and a fractional luminosity (in V) for the primary star of 0.8. System1460Orbit1End System1461Orbit1Begin Radford and Griffin describe the spectral type as late K or early M and luminosity class II or III. System1461Orbit1End System1462Orbit1Begin The elements obtained by Vogt are based partly on new high-dispersion observations and partly on the older ones. Except for the poorly determined longitude of periastron, Vogt's values agree well with those found by I. Halliday (J. Roy. Astron. Soc. Can., 46, 103, 1952) and R.F. Sanford (Astrophys. J., 53, 221, 1921). Variation of the system's light in a period close to the orbital period was first discovered by P.F. Chugainov (Izv. Krym. Astrofiz. Obs., 54, 89, 1976), see also S.M. Rucinski (Publ. Astron. Soc. Pacific, 89, 280, 1977). The star is now widely regarded as a non-eclipsing RS CVn system. Vogt's paper contains a thorough spectroscopic and photometric study. He also discusses (Astrophys. J., 240, 567, 1980) the evidence for a magnetic field. F.M. Walter et al. (ibid., 236, 212, 1980) discovered the X-ray flux from this system. Variations in the H-alpha emission are discussed by B.W. Bopp and P.V. Noah (Publ. Astron. Soc. Pacific, 92, 333, 1980) and H.L. Nations and L.W. Ramsey (Astron. J., 85, 1086, 1988). Observations with IUE are discussed by A. Udalski and S.M. Rucinski (Acta Astron., 32, 315, 1982) and M. Rodono et al. (Astron. Astrophys., 176, 267, 1987). System1462Orbit1End System1463Orbit1Begin The new observations supersede those of S. Archer and M.W. Feast (Mon. Notes Astron. Soc. South Africa, 17, 9, 1958). The spectral types are based partly on computations from the light-curve. The small eccentricity appears to be significant and is consistent with the light-curve. The epoch is T0 for the primary component. Primary minimum is at J.D. 2,443,698.513. Haefner, Skillen and de Groot also present UBV light-curves. They find an orbital inclination close to 80 deg and a visual-magnitude difference between the components of 2.17m. System1463Orbit1End System1464Orbit1Begin Although the star is believed to be an occultation double (D.W. Dunham et al., Astron. J., 78, 482, 1973) it seems unlikely that the spectroscopic secondary can be the star thus detected. Griffin considers the star to be a giant, because of the deep dips in his radial-velocity traces. System1464Orbit1End System1465Orbit1Begin The new orbital elements by Hill and Fisher supersede those derived by R.F. Sanford (Astrophys. J., 83, 121, 1936) and by R.K. Young (Publ. Dom. Obs., 3, 373, 1916). The spectral classification for the secondary is based on a comparison of equivalent widths in the spectra of the two components. Hill and Fisher estimate the difference of visual magnitude between the two components to be 2.2m. There is some evidence for apsidal motion with a period of about 400 years. Only an incomplete light-curve is available (C.R. Lynds, Astrophys. J., 130, 599, 1959). The orbital inclination is estimated to be around 60 deg. The star belongs to the group Cas OB9. System1465Orbit1End System1466Orbit1Begin The new observations by Imbert confirm and supersede the older observations by W.E. Harper (Publ. Dom. Astrophys. Obs., 2, 263, 1923) and his subsequent revision of the elements (Publ. Dom. Astrophys. Obs., 6, 252, 1935). The two spectra are apparently closely similar: their classification as G8 Ib in Kennedy's catalogue appears to be a mistake. Petrie(II) found Delta m=0.14. System1466Orbit1End System1467Orbit1Begin Lu's study of this W UMa system by cross-correlation methods represents a considerable improvement over the only previous spectroscopic investigation by O. Struve et al. (Astrophys. J., 111, 658, 1950). The orbit is assumed circular, in accordance with the light-curve, and the epoch is T0 for the primary (more massive component). Lu estimates the magnitude difference between the stars as 0.42m in the blue region. The spectral classifications given are his. Many photometric studies have been published. The best are probably the new UBV observations by D.-S. Zhai, K.-C. Leung and R.-X. Zhang (Astron. Astrophys. Supp., 57, 487, 1984) and the rediscussion by G. Russo et al. (ibid., 47, 211, 1982) of observations by L. Binnendijk (Astron. J., 65, 88, 1960) which agree on an orbital inclination of about 75 deg and a fractional luminosity (in V) for the brighter component between 0.6 and 0.7. Other studies have been published by P.G. Niarchos (Astrophys. Space Sci., 58, 301, 1978), S.J. Lafta and J.F. Grainger (ibid., 121, 61, 1986) and L. Binnendijk (Publ. Astron. Soc. Pacific, 96, 646, 1984). System1467Orbit1End System1468Orbit1Begin P=26.27y, T=1910.11, i=50 deg. Together with the values of e and omega these were assumed by Underhill from the visual orbit by R.G. Hall (Astron. J., 54, 102, 1949). Radial velocities were also published by O. Struve and V. Zebergs (Astrophys. J., 130, 134, 1959) who found V0=35.7 km/s. Assuming a parallax of 0.080", Underhill found the masses to be 0.77 MSol and 0.85 MSol. The system is A.D.S. 17175. The spectroscopic pair has a major semi-axis of 0.83" and Delta m=3.04. Two other companions are listed in I.D.S. but both are probably optical. System1468Orbit1End System1469Orbit1Begin The epoch is T0. Hiltner et al. tried a solution for the orbital elements with e=0.12 and omega=178 deg, but concluded that the circular orbit fitted the observations nearly as well. Lucy & Sweeney also adopt a circular orbit. The secondary spectrum is seen only during primary eclipse. M. Ammann and K. Walter (Astron. Astrophys., 24, 131, 1973) have published photoelectric (BV) light-curves. The V magnitudes given in the Catalogue are approximate and derived from their data. Their method of solution which leads them to hypothesize a hot spot on the surface of the primary is controversial. It yields i=87 deg and a fractional luminosity (in V) of 0.8 for the primary component, with an assumed third light of 0.05. System1469Orbit1End System815Orbit2Begin Despite the rather long period (about 80 years), there are radial velocities of both components back to 1904. This is a simultaneous visual-spectroscopic orbit which yielded to a tiny upward revision of the mass of the two components (Pourbaix, Dec. 2000). System815Orbit2End System4Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System4Orbit2End System1470Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1470Orbit1End System50Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System50Orbit2End System1471Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1471Orbit1End System98Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System98Orbit2End System111Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System111Orbit2End System117Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). There is a strong correlation between the inclination, the argument of the periastron and the periastron time. Additional precise radial velocities are welcome. System117Orbit2End System1472Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1472Orbit1End System135Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System135Orbit2End System136Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System136Orbit2End System154Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). The orbit perfectly recovers the date of the eclipse observed by R.F. Griffin et al. (1994, IAPPP Comm. 57, 31). Although the precision on the masses is already better than 4%, additional precise radial velocities are still very welcome. System154Orbit2End System232Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System232Orbit2End System1473Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1473Orbit1End System306Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System306Orbit2End System366Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System366Orbit2End System478Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System478Orbit2End System559Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System559Orbit2End System1474Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1474Orbit1End System690Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System690Orbit2End System764Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System764Orbit2End System1475Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1475Orbit1End System842Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System842Orbit2End System969Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System969Orbit2End System1476Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1476Orbit1End System1022Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1022Orbit2End System1058Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1058Orbit2End System1073Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). The uncertainty on V0 prevents from deriving precise masses. System1073Orbit2End System1162Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1162Orbit2End System1168Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1168Orbit2End System1477Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). Although the visual and spectroscopic data can both yield a 4.9-year orbit, the radial velocities of this Line-Width Spectroscopic Binary (Duquennoy & Mayor, 1991, A&A, 248, 485) might be questionable. System1477Orbit1End System1478Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1478Orbit1End System1211Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1211Orbit2End System2460Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System2460Orbit1End System1290Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1290Orbit2End System1291Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1291Orbit2End System1350Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1350Orbit2End System1479Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1479Orbit1End System1480Orbit1Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1480Orbit1End System1432Orbit2Begin Simultaneous adjustment of the visual and spectroscopic data (VB-SB2 system). System1432Orbit2End System1481Orbit1Begin AB is a visual binary with a period of 93 yr. The spectral type of the physical tertiary C is estimated as K0V from its photometry (V=10.21, B-V=0.86), it is the spectroscopic binary. Minimum mass of Cb is 0.18 M_sun. System1481Orbit1End System1482Orbit1Begin The 15 radial velocities of Bonsack (1981 PASP 93 756) were used jointly with our data to derive the orbit. The small eccentricity is significant. The spectroscopic secondary is likely to be massive (>1.0 M_sun) and can be a white dwarf. The visual secondary B is physical, RV=0.8 km/s. System1482Orbit1End System1483Orbit1Begin The spectroscopic binary Cab is a physical tertiary to the visual binary AB with an orbital period of 78.5 yr. The lines of Cb were detected marginally; the spectral type of Cb is estimated as K5V. The estimated separation of Cab is around 0.015 arcsec. System1483Orbit1End System1484Orbit1Begin The component C is physical to the A, which is also a spectroscopic binary. The mass of Cb is tentatively estimated as 0.3 M_sun. The C component contains a very hot white dwarf and is an X-ray source (Hodgikin et al. 1993, MNRAS 263, 229). It is not clear whether the white dwarf can be identified with Cb or constitutes yet another body of this multiple system. System1484Orbit1End System1485Orbit1Begin The component A is a spectroscopic binary, while the physical components BC are a visual binary with a period of 50 yr. The radial velocities of Beavers & Eitter (1986, ApJS 62, 147) were used to refine the period of Aab. The spectral types of Aa and Ab are estimated as F5V and G5V, their V-magnitudes as 6.86 and 9.14. System1485Orbit1End System1486Orbit1Begin The wide visual pair AB is physical, RV(B)=-6.59 +- 0.13 km/s. System1486Orbit1End System1487Orbit1Begin The estimated spectral types of Aa and Ab are M1V and M2V, their V-magnitudes 10.02 and 10.57. The separation of Aab must be 0.051 arcsec, it is resolvable with speckle interferometry. The component B is physical. System1487Orbit1End System1488Orbit1Begin Code 203: the data from H.A. Abt & D.W. Willmarth, ApJS 94, 677, 1994 with +1.3 km/s shift. The rest of data are from Cambridge coravel. System1488Orbit1End System1489Orbit1Begin The codes of RV observations: 201 OHP coravel, rejected observation 202 OHP coravel, half weight 203 H.A. Abt & D.W. Willmarth, ApJS 94, 677, 1994 218 F. & M. Spite, A&A 25, 325, 1973. Zero-weighted. 302 Cambridge coravel 303 OHP coravel All code numbers above 500 are blends, zero-weighted, and the velocites are printed between the columns for the primary and secondary. 578 H.A. Abt & S.G. Levy, ApJS 30, 273, 1976. 592 W.E. Harper, PDOA 6, 149, 1934. 703 W.W. Campbell & J.H. Moore, PLO 16, 306, 1928. 704 W.I. Beavers & J.J. Eitter, ApJS 62, 147, 1986. 705 OHP coravel, unresolved blend 718 As 218 720 W.S. Adams & A.H. Joy, ApJ 57, 149, 1923; H.A. Abt, ApJS 26, 385, 1973. System1489Orbit1End System1471Orbit2Begin Combined spectroscopic-visual solution. Magnitude difference in V is estimated as 1.23. System1471Orbit2End System1480Orbit2Begin Combined visual-spectroscopic orbit, but the spectroscopic data are yet poor. Center-of-mass velocity was fixed, as found from the blended lines (a+b). System1480Orbit2End System1490Orbit1Begin COR: data from CORAVEL at Haute Provence, otherwise - data from RVM. Additional 28 velocities were published by Latham et al. (1996 AJ 96 567), they match the new oarit with a zero-point correction of -0.6 km/s. This orbit refers to the visual secondary of ADS 2757, the primary has average radial velocity of 50.18 +- 0.11 km/s. System1490Orbit1End System1491Orbit1Begin COR: data from CORAVEL at Haute Provence, otherwise - data from RVM. System1491Orbit1End System1492Orbit1Begin COR: data from CORAVEL at Haute Provence, otherwise - data from RVM, corrected by -0.4 km/s. System1492Orbit1End System1493Orbit1Begin Three blended dips belonging to the visual primary A and the spectroscopic components Ba and Bb are observed. The dips are splitted with fixed parameters. System1493Orbit1End System1494Orbit1Begin Combined spectroscopic-visual orbit. Component 'b' are the center-of-mass velocities of Bab for individual seasons, component 'a' are the seasonal means for the visual primary A. System1494Orbit1End System1495Orbit1Begin Primary component of this fain visual binary is the spectroscopic system, the secondary at 4" is optical, radial velocity around -10 km/s. System1495Orbit1End System1496Orbit1Begin The orbit refers to the visual secondary B. Its photometry: V=11.74, B-V=0.75. The primary A at 9" is optical, its radial velocity is -33 km/s. System1496Orbit1End System1497Orbit1Begin Typographic error in the K1 is corrected here. It is assumed that the spectroscopic sub-system is related to the visual primary. Radial velocities in 1990 are corrected by +3.6 km/s to account for the motion in the visual orbit, hence the center-of-mass velocity of Aab refers to the period 1991-1993. System1497Orbit1End System1498Orbit1Begin Radial velocities of Aa are corrected for the motion in the AB orbit by adding -0.9, -0.7, -0.6, 0 km/s for the seasons of 1989, 1990, 1991, and 1992, respectively. The tentative values for the spectroscopic elements of the 30.5-yr isual orbit AB are found: K1=1.5 +- 0.2, K2=3.5 +- 0.4, V0=0.42 km/s. System1498Orbit1End System1499Orbit1Begin Additional 9 velocities measured at Mount Wilson (Abt, 1970, ApJS 19 387) were used with a correction of -1.5 km/s (code MtW). System1499Orbit1End System1500Orbit1Begin Circular orbit. Code COR: data from the CORAVEL at Haute Provence. System1500Orbit1End System1501Orbit1Begin The system has been resolved by speckle interferometry and now has a visual orbit as well. System1501Orbit1End System1032Orbit2Begin Old data of Boothroyd (1922 Publ. DAO 1 246) do not improve even the period, hence were not used for orbit computing. System1032Orbit2End System1502Orbit1Begin Combined spectroscopic-interferometric orbit. COR marks data from OHP Coravel, other data are from RVM, corrected by +0.20 km/s. Endnotes End Systems2Orbit1Begin The component C is physical to the visual binary AB with known orbit, the system is hence at least quadruple. Spectral types of Ca and Cb are derived from the system model, based on absolute magnitudes and equivalent widths of the correlation dips. Eccentricity is small, but significant. Systems2Orbit1End Systems3Orbit1Begin Component B is physical to A, which is itself a known double-lined binary. Difficult observations (mixed with the light from A at 10.6"). Systems3Orbit1End Systems4Orbit1Begin Component C is optical to the close visual pair AB. The spectral types of Ca and Cb are derived from system model, based on photometry and equivalent widths of the correlation dips. Systems4Orbit1End Systems5Orbit1Begin The component B is physical, C is optical. The system contains at least 5 components, because A is a close visual binary Cou 2084 and a double-lined spectroscopic binary. Systems5Orbit1End Systems6Orbit1Begin Component B is only at 3.4" from the bright primary A, hence observations were difficult. The spectral types of Ba and Bb are derived from system model, based on photometry and equivalent widths of the correlation dips. Systems6Orbit1End Systems7Orbit1Begin The spectroscop9c sub-system belongs to the primary of the visual binary ADS 16111 with an orbital period of 49 yr. Radial velocities were corrected for the motion in the visual orbit by adding +1.8, 0, and -1.3 km/s for the seasons of 1995, 1996, and 1997, respectively. Few measurements of the broad correlation dip of the component B lead to tentative estimate of the spectroscopic elements of the visual 49-yr orbit: K1=8.8, K2=11.2, V0=-4.2 km/s. The distant component D is physical. Systems7Orbit1End Systems8Orbit1Begin Despite the fact that the visual pair AB has only 2.5" separation, some observations were resolved. Plusses mark the velocities derived from the unresolved correlation profiles of A+B; asterisks mark the velocities derived by splitting the double dips in unresolved profiles when the velocities of A and B differed by more than 15 km/s. The spectral types of Aa and Ab are derived from the system model. The mean radial velocity of the component B is -22.74 +- 0.16 km/s. Systems8Orbit1End Systems9Orbit1Begin The whole system ADS 9731 is at least sextuple. The spectral types of Aa and Ab are derived from the system model. Systems9Orbit1End Systems10Orbit1Begin The orbit of Dab is based on a small number of observations when D and C (separated by 1.6") were resolved. Larger number of unresolved observations of CD is available and it confirms the orbital period. Spectral type of Da is estimated from the system model. Systems10Orbit1End Systems11Orbit1Begin The visual secondary B is physical to A, radial velocity of A is constant. Observations were difficult (A is 8.5" from B). Spectral types of Ba and Bb are estimated from the system model, based on the minimum masses and the parameters of the correlation dip. Code COR marks 2 observations at the OHP Coravel. Systems11Orbit1End Systems12Orbit1Begin Data from Latham et al. (1988 AJ 96 567) are marked as 'L' and used to improve the orbit together with new observations (same zero point), which show the system to be double-lined. The spectral types of Aa and Ab are estimated from the system model. Systems12Orbit1End Systems13Orbit1Begin The components Ca and Cb are identical. Cab is physical to the visual pair AB (= HD 8624), the whole system is thus at least quadruple. Systems13Orbit1End Systems14Orbit1Begin The spectroscopic system is the western component B, while the equally bright visual component A at 4.6" (HR 2485 = HD 48767) is physical and has a constant radial velocity 0f 7.9 +- 0.2 km/s. The component C is optical. Systems14Orbit1End Systems15Orbit1Begin Only one observation of the secondary dip is used to determine K2. The spectral types of Ba and Bb are estimated from the system model, based on correlation dip parameters. The visual component A at 6.1" is physical, its radial velocity is -16.1 +- 0.1 km/s. Systems15Orbit1End Systems16Orbit1Begin The visual secondary is optical, its radial velocity is -15.5 +- 0.2 km/s, correlation dip has a high contrast. Systems16Orbit1End Systems17Orbit1Begin The small eccentricity is significant. The visual components A and B are physical, both are evolved and above Main Sequence. The radial velocity of B is constant at -51.8 +- 0.2 km/s. Systems17Orbit1End Systems18Orbit1Begin The three visual components A, B, C are likely physical. The orbit refers to the blended lines of AB, hence the real K1 is larger. There are reasons to believe that the spectroscopic system is related to the component A. Systems18Orbit1End Systems19Orbit1Begin Combined spectroscopic-interferometric orbit of HR 7272A = CHARA 84. Most of the observations were obtained with the OHP Coravel, the remaining data (marked 'Camb') are from the Cambridge Coravel. The individual velocities of the components are found by splitting the heavily blended correlation dips with assumed dip parameters, hence the amplitudes K1 and K2 are model-dependent. Additional observations from RVM instrument are available, but were not splitted and not used in orbit computation. The spectral types and magnitudes of Aa and Ab are from the system model. The visual component B is physical and has a constant radial velocity of -40.5 km/s. Systems19Orbit1End Systems20Orbit1Begin Combined spectroscopic-interferometric orbit. Blended correlation dips were split with fixed parameters of individual components, hence the amplitudes K1 and K2 are model-dependent. Systems20Orbit1End System1502Orbit1End System1503Orbit1Begin The component C is physical to the visual binary AB with known orbit, the system is hence at least quadruple. Spectral types of Ca and Cb are derived from the system model, based on absolute magnitudes and equivalent widths of the correlation dips. Eccentricity is small, but significant. System1503Orbit1End System1504Orbit1Begin Component B is physical to A, which is itself a known double-lined binary. Difficult observations (mixed with the light from A at 10.6"). System1504Orbit1End System1505Orbit1Begin Component C is optical to the close visual pair AB. The spectral types of Ca and Cb are derived from system model, based on photometry and equivalent widths of the correlation dips. System1505Orbit1End System1506Orbit1Begin The component B is physical, C is optical. The system contains at least 5 components, because A is a close visual binary Cou 2084 and a double-lined spectroscopic binary. System1506Orbit1End System1507Orbit1Begin Component B is only at 3.4" from the bright primary A, hence observations were difficult. The spectral types of Ba and Bb are derived from system model, based on photometry and equivalent widths of the correlation dips. System1507Orbit1End System1508Orbit1Begin The spectroscop9c sub-system belongs to the primary of the visual binary ADS 16111 with an orbital period of 49 yr. Radial velocities were corrected for the motion in the visual orbit by adding +1.8, 0, and -1.3 km/s for the seasons of 1995, 1996, and 1997, respectively. Few measurements of the broad correlation dip of the component B lead to tentative estimate of the spectroscopic elements of the visual 49-yr orbit: K1=8.8, K2=11.2, V0=-4.2 km/s. The distant component D is physical. System1508Orbit1End System1509Orbit1Begin Despite the fact that the visual pair AB has only 2.5" separation, some observations were resolved. Plusses mark the velocities derived from the unresolved correlation profiles of A+B; asterisks mark the velocities derived by splitting the double dips in unresolved profiles when the velocities of A and B differed by more than 15 km/s. The spectral types of Aa and Ab are derived from the system model. The mean radial velocity of the component B is -22.74 +- 0.16 km/s. System1509Orbit1End System1510Orbit1Begin The whole system ADS 9731 is at least sextuple. The spectral types of Aa and Ab are derived from the system model. System1510Orbit1End System1511Orbit1Begin The orbit of Dab is based on a small number of observations when D and C (separated by 1.6") were resolved. Larger number of unresolved observations of CD is available and it confirms the orbital period. Spectral type of Da is estimated from the system model. System1511Orbit1End System1512Orbit1Begin The visual secondary B is physical to A, radial velocity of A is constant. Observations were difficult (A is 8.5" from B). Spectral types of Ba and Bb are estimated from the system model, based on the minimum masses and the parameters of the correlation dip. Code COR marks 2 observations at the OHP Coravel. System1512Orbit1End System1513Orbit1Begin Data from Latham et al. (1988 AJ 96 567) are marked as 'L' and used to improve the orbit together with new observations (same zero point), which show the system to be double-lined. The spectral types of Aa and Ab are estimated from the system model. System1513Orbit1End System1514Orbit1Begin The components Ca and Cb are identical. Cab is physical to the visual pair AB (= HD 8624), the whole system is thus at least quadruple. System1514Orbit1End System1515Orbit1Begin The spectroscopic system is the western component B, while the equally bright visual component A at 4.6" (HR 2485 = HD 48767) is physical and has a constant radial velocity 0f 7.9 +- 0.2 km/s. The component C is optical. System1515Orbit1End System1516Orbit1Begin Only one observation of the secondary dip is used to determine K2. The spectral types of Ba and Bb are estimated from the system model, based on correlation dip parameters. The visual component A at 6.1" is physical, its radial velocity is -16.1 +- 0.1 km/s. System1516Orbit1End System1517Orbit1Begin The visual secondary is optical, its radial velocity is -15.5 +- 0.2 km/s, correlation dip has a high contrast. System1517Orbit1End System1518Orbit1Begin The small eccentricity is significant. The visual components A and B are physical, both are evolved and above Main Sequence. The radial velocity of B is constant at -51.8 +- 0.2 km/s. System1518Orbit1End System1519Orbit1Begin The three visual components A, B, C are likely physical. The orbit refers to the blended lines of AB, hence the real K1 is larger. There are reasons to believe that the spectroscopic system is related to the component A. System1519Orbit1End System1520Orbit1Begin Combined spectroscopic-interferometric orbit of HR 7272A = CHARA 84. Most of the observations were obtained with the OHP Coravel, the remaining data (marked 'Camb') are from the Cambridge Coravel. The individual velocities of the components are found by splitting the heavily blended correlation dips with assumed dip parameters, hence the amplitudes K1 and K2 are model-dependent. Additional observations from RVM instrument are available, but were not splitted and not used in orbit computation. The spectral types and magnitudes of Aa and Ab are from the system model. The visual component B is physical and has a constant radial velocity of -40.5 km/s. System1520Orbit1End System1521Orbit1Begin Combined spectroscopic-interferometric orbit. Blended correlation dips were split with fixed parameters of individual components, hence the amplitudes K1 and K2 are model-dependent. System1521Orbit1End System1522Orbit1Begin The orbit is derived from the partially resolved observations of the visual component B separated from A by 1.5". It confirms the orbit of Griffin (1999 Observatory 119 27), which is of better quality. System1522Orbit1End System1523Orbit1Begin The physical visual primary component A is itself a double-lined binary. System1523Orbit1End System1524Orbit1Begin The visual secondary component B is a spectroscopic triple system, with two visible components in a short-period orbit and an invisible (but massive) tertiary on an 8-yr orbit. The radial velocities reflect motions in both long- and short-period orbits. Spectral types of Ba and Bb are derived from the system model (photometry, dip parameters). System1524Orbit1End System1525Orbit1Begin This 8-yr orbit of the long-period sub-system in ADS 3161 B is preliminary. Radial velocities listed for this orbit are in fact either residuals to the short-period orbit (only data with errors less than 0.5 km/s are retained) or the velocities corresponding to the blended dips of Ba and Bb (marked as component a+b). System1525Orbit1End System1526Orbit1Begin Both components A and B of ADS 3243 have fast axial rotation which explains the low accuracy of the radial velocities. The component B is physical and has a constant radial velocity of -43.3 +- 0.4 km/s. The component A is above the Main Sequence, it must be evolved. System1526Orbit1End System1527Orbit1Begin The component B is physical to A = 88 Tau which, in turn, contains a close visual system CHARA 18 and at least one spectroscopic binary. Three observations marked 'COR' are from the OHP Coravel. System1527Orbit1End System1528Orbit1Begin The orbit is only preliminary, eccentricity and longitude of periastron are fixed. Data of Struve & Zebergs (1959 AJ 64 219) are used with a correction of -1.8 km/s (marked 'Struve'). The visual secondary B = HD 139460 at 11.8" is physical and has a constant radial velocity of 1.2 +- 0.1 km/s. System1528Orbit1End System1529Orbit1Begin The visual components AB separated by 2.6" were difficult to resolve. The radial velocity of A is constant, -31.7 +- 0.4 km/s. The distant component C listed in ADS is optical and is itself a double-lined binary with yet unknown orbit. System1529Orbit1End System1530Orbit1Begin The system ADS 12145 is at least quintuple. The spectroscopic orbit refers to the component C, which forms together with the primary A a close visual system with period of 63 yr. The blended dips of A and Ca were separated by fitting two Gaussians. The radial velocity of A is constant, 26.1 +- 0.1 km/s. The component B, at 4.5" to the south of AC, has a slowly changing radial velocity (orbital period more than 9 yr). The spectral type of Ca is estimated from the model of the system. System1530Orbit1End System1531Orbit1Begin Large orbital uncertainties due to incomplete phase coverage. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1531Orbit1End System1532Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1532Orbit1End System1533Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1533Orbit1End System1534Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1534Orbit1End System1535Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1535Orbit1End System1536Orbit1Begin Large orbital uncertainties due to incomplete phase coverage. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1536Orbit1End System799Orbit2Begin Other references in text. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System799Orbit2End System820Orbit2Begin Other references in text. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System820Orbit2End System1537Orbit1Begin The eccentricity was fixed to e=0.54 (Latham et al. 1989) since not enough points were available to constrain the eccentricity. Other references in text. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1537Orbit1End System1538Orbit1Begin System1538Orbit1End System1539Orbit1Begin The fit is poor since as insufficient velocities are available to constrain the orbital period to better than a factor of 2. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1539Orbit1End System1540Orbit1Begin Large orbital uncertainties due to incomplete phase coverage. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1540Orbit1End System1541Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1541Orbit1End System1542Orbit1Begin Other references in text. The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1542Orbit1End System1543Orbit1Begin The 3 m/s precision is achieved thanks to relative velocities: a high resolution spectrum of the very same star is used as a reference template and the displacements measured according to that spectrum. The listed RV are nevertheless absolute (see publication for details). System1543Orbit1End System945Orbit2Begin System945Orbit2End System1544Orbit1Begin System1544Orbit1End System1545Orbit1Begin System1545Orbit1End System1546Orbit1Begin System1546Orbit1End System1547Orbit1Begin System1547Orbit1End System884Orbit2Begin System884Orbit2End System1548Orbit1Begin System1548Orbit1End System1549Orbit1Begin System1549Orbit1End System1550Orbit1Begin In the paper, the two T0 differ by nearly half a period. The two systemic velocities are also different System1550Orbit1End System1551Orbit1Begin System1551Orbit1End System1552Orbit1Begin System1552Orbit1End System1553Orbit1Begin System1553Orbit1End System1554Orbit1Begin The orbits published for that star in Van Eck et al. (2000, A&AS 145, 51) and Udry et al. (1998, A&A 131, 25) should be considered as identical. System1554Orbit1End System1554Orbit2Begin The orbits published for that star in Van Eck et al. (2000, A&AS 145, 51) and Udry et al. (1998, A&A 131, 25) should be considered as identical. System1554Orbit2End System1555Orbit1Begin System1555Orbit1End System1556Orbit1Begin System1556Orbit1End System1557Orbit1Begin System1557Orbit1End System1558Orbit1Begin System1558Orbit1End System1559Orbit1Begin The nearby K star PPM 91177 (BD+21 255p) is as well a spectroscopic binary System1559Orbit1End System1560Orbit1Begin System1560Orbit1End System1561Orbit1Begin System1561Orbit1End System1562Orbit1Begin System1562Orbit1End System1563Orbit1Begin System1563Orbit1End System1564Orbit1Begin System1564Orbit1End System1565Orbit1Begin System1565Orbit1End System1566Orbit1Begin System1566Orbit1End System1567Orbit1Begin System1567Orbit1End System1568Orbit1Begin System1568Orbit1End System1569Orbit1Begin System1569Orbit1End System1570Orbit1Begin System1570Orbit1End System1571Orbit1Begin System1571Orbit1End System1572Orbit1Begin System1572Orbit1End System1573Orbit1Begin System1573Orbit1End System1574Orbit1Begin System1574Orbit1End System1575Orbit1Begin System1575Orbit1End System1576Orbit1Begin System1576Orbit1End System1577Orbit1Begin System1577Orbit1End System1578Orbit1Begin System1578Orbit1End System1579Orbit1Begin System1579Orbit1End System1580Orbit1Begin System1580Orbit1End System1581Orbit1Begin System1581Orbit1End System1582Orbit1Begin System1582Orbit1End System1583Orbit1Begin System1583Orbit1End System1584Orbit1Begin System1584Orbit1End System1585Orbit1Begin System1585Orbit1End System1586Orbit1Begin System1586Orbit1End System1587Orbit1Begin System1587Orbit1End System1588Orbit1Begin System1588Orbit1End System1589Orbit1Begin System1589Orbit1End System1590Orbit1Begin System1590Orbit1End System1591Orbit1Begin System1591Orbit1End System1592Orbit1Begin System1592Orbit1End System1593Orbit1Begin System1593Orbit1End System1594Orbit1Begin System1594Orbit1End System1595Orbit1Begin A triple hierarchical system System1595Orbit1End System1596Orbit1Begin A triple hierarchical system System1596Orbit1End System1597Orbit1Begin System1597Orbit1End System1598Orbit1Begin System1598Orbit1End System1599Orbit1Begin System1599Orbit1End System1600Orbit1Begin System1600Orbit1End System1601Orbit1Begin System1601Orbit1End System407Orbit2Begin Possibly an eclipsing binary System407Orbit2End System1602Orbit1Begin System1602Orbit1End System1603Orbit1Begin System1603Orbit1End System1604Orbit1Begin System1604Orbit1End System1605Orbit1Begin System1605Orbit1End System1606Orbit1Begin System1606Orbit1End System1607Orbit1Begin The star was incorrectly labelled BD+21 255a in Jorissen & Mayor (1992, A&A 260, 115) System1607Orbit1End System1608Orbit1Begin System1608Orbit1End System1609Orbit1Begin System1609Orbit1End System1610Orbit1Begin System1610Orbit1End System1611Orbit1Begin System1611Orbit1End System1612Orbit1Begin System1612Orbit1End System1613Orbit1Begin System1613Orbit1End System1614Orbit1Begin An eclipsing binary, also symbiotic System1614Orbit1End System1615Orbit1Begin System1615Orbit1End System1616Orbit1Begin System1616Orbit1End System1617Orbit1Begin Possibly an ellipsoidal variable System1617Orbit1End System1618Orbit1Begin System1618Orbit1End System1619Orbit1Begin System1619Orbit1End System1620Orbit1Begin System1620Orbit1End System1621Orbit1Begin System1621Orbit1End System815Orbit3Begin Despite the rather long period (about 80 years), there are radial velocities of both components back to 1904. The time interval covered with very precise radial velocities is about 12 years. The simultaneous spectroscopic- visual orbit accounts for the convective blueshift and the gravitational redshift. System815Orbit3End System1622Orbit1Begin System1622Orbit1End System1623Orbit1Begin System1623Orbit1End System1624Orbit1Begin System1624Orbit1End System1625Orbit1Begin System1625Orbit1End System1626Orbit1Begin System1626Orbit1End System1627Orbit1Begin System1627Orbit1End System1628Orbit1Begin System1628Orbit1End System262Orbit2Begin System262Orbit2End System1629Orbit1Begin System1629Orbit1End System340Orbit2Begin System340Orbit2End System1630Orbit1Begin System1630Orbit1End System1631Orbit1Begin System1631Orbit1End System1632Orbit1Begin System1632Orbit1End System1633Orbit1Begin System1633Orbit1End System1634Orbit1Begin System1634Orbit1End System1635Orbit1Begin System1635Orbit1End System1636Orbit1Begin System1636Orbit1End System1637Orbit1Begin System1637Orbit1End System1638Orbit1Begin System1638Orbit1End System1469Orbit2Begin Eclipsing binary. The orbit is for the hot component. System1469Orbit2End System1639Orbit1Begin Eclipsing binary. The orbit is for the cool component. System1639Orbit1End System1640Orbit1Begin Eclipsing binary. The primary is the hot component. System1640Orbit1End System525Orbit2Begin Eclisping binary. The primary is the hot component. The periastron epoch is wrongly listed as 7582.981 in the paper. System525Orbit2End System1641Orbit1Begin Eclipsing binary. The orbit is for the cool component. System1641Orbit1End System490Orbit2Begin Eclipsing binary. The orbit is for the cool component. The period is wrongly listed as 96.967d is the paper. System490Orbit2End System1642Orbit1Begin Eclipsing binary. The orbit is for the cool component. System1642Orbit1End System1643Orbit1Begin Eclisping binary. The primary is the hot component. System1643Orbit1End System1017Orbit2Begin Eclisping binary. The primary is the hot component. System1017Orbit2End System1644Orbit1Begin Eclisping binary. The primary is the hot component. System1644Orbit1End System315Orbit2Begin Eclisping binary. The primary is the hot component. System315Orbit2End System1645Orbit1Begin Eclisping binary. The primary is the hot component. System1645Orbit1End System1646Orbit1Begin System1646Orbit1End System1647Orbit1Begin System1647Orbit1End System1648Orbit1Begin System1648Orbit1End System1649Orbit1Begin System1649Orbit1End System1650Orbit1Begin System1650Orbit1End System1651Orbit1Begin System1651Orbit1End System884Orbit3Begin System884Orbit3End System1652Orbit1Begin System1652Orbit1End System1653Orbit1Begin System1653Orbit1End System1654Orbit1Begin 13 RV obtained when the two sets of lines were not resolved are not listed on SB9 here although they are in Griffin's paper. System1654Orbit1End System1655Orbit1Begin System1655Orbit1End System1656Orbit1Begin System1656Orbit1End System1657Orbit1Begin System1657Orbit1End System1658Orbit1Begin System1658Orbit1End System1659Orbit1Begin System1659Orbit1End System1660Orbit1Begin System1660Orbit1End System1661Orbit1Begin System1661Orbit1End System1662Orbit1Begin System1662Orbit1End System1663Orbit1Begin 24 Aqr is a triple system. Although radial velocities of component B are given in the paper, no new orbit is derived for that system owing to its long orbital period (about 50 years) with respect to the time interval covered by the CORAVEL data available so far. System1663Orbit1End System1664Orbit1Begin System1664Orbit1End System1665Orbit1Begin System1665Orbit1End System1666Orbit1Begin System1666Orbit1End System1667Orbit1Begin System1667Orbit1End System1668Orbit1Begin System1668Orbit1End System1669Orbit1Begin System1669Orbit1End System1670Orbit1Begin System1670Orbit1End System1671Orbit1Begin System1671Orbit1End System1672Orbit1Begin System1672Orbit1End System1673Orbit1Begin System1673Orbit1End System1674Orbit1Begin System1674Orbit1End System1675Orbit1Begin System1675Orbit1End System1676Orbit1Begin System1676Orbit1End System1677Orbit1Begin System1677Orbit1End System1678Orbit1Begin System1678Orbit1End System1679Orbit1Begin System1679Orbit1End System276Orbit2Begin System276Orbit2End System1680Orbit1Begin System1680Orbit1End System1681Orbit1Begin System1681Orbit1End System1682Orbit1Begin System1682Orbit1End System1683Orbit1Begin System1683Orbit1End System1684Orbit1Begin System1684Orbit1End System1685Orbit1Begin System1685Orbit1End System1686Orbit1Begin System1686Orbit1End System1687Orbit1Begin System1687Orbit1End System1688Orbit1Begin System1688Orbit1End System1689Orbit1Begin System1689Orbit1End System1690Orbit1Begin System1690Orbit1End System1691Orbit1Begin System1691Orbit1End System1692Orbit1Begin System1692Orbit1End System1693Orbit1Begin System1693Orbit1End System1694Orbit1Begin System1694Orbit1End System1695Orbit1Begin System1695Orbit1End System1696Orbit1Begin System1696Orbit1End System1697Orbit1Begin System1697Orbit1End System908Orbit2Begin System908Orbit2End System1698Orbit1Begin The amplitude of the secondary listed in the paper is clearly wrong. It was updated to 17.01 km/s (instead of 167.01 km/s) System1698Orbit1End System1699Orbit1Begin System1699Orbit1End System1700Orbit1Begin System1700Orbit1End System1701Orbit1Begin System1701Orbit1End System1702Orbit1Begin System1702Orbit1End System1703Orbit1Begin System1703Orbit1End System1704Orbit1Begin System1704Orbit1End System1705Orbit1Begin System1705Orbit1End System1706Orbit1Begin System1706Orbit1End System1707Orbit1Begin System1707Orbit1End System1708Orbit1Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=33.3 km/s System1708Orbit1End System1709Orbit1Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=14.9 km/s System1709Orbit1End System1692Orbit2Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=11.5 km/s. Adopting a primary mass of 0.92 Mo and the Hipparcos orbital inclination of 73.9 deg yields a secondary mass of 0.45 Mo. System1692Orbit2End System1710Orbit1Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=9.0 km/s. System1710Orbit1End System1711Orbit1Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=8.1 km/s. System1711Orbit1End System1712Orbit1Begin The velocities are on the native CfA system; add 0.14 km/s to convert to an absolute system defined by minor planet observations. The velocities were recomputed in October 2002 with nzpass=2, and the orbits were resolved. No floor error is included in the velocity errors. vsini=11.6 km/s. System1712Orbit1End System1713Orbit1Begin System1713Orbit1End System351Orbit2Begin System351Orbit2End System61Orbit2Begin System61Orbit2End System934Orbit2Begin System934Orbit2End System1714Orbit1Begin System1714Orbit1End System1715Orbit1Begin System1715Orbit1End System1716Orbit1Begin System1716Orbit1End System1717Orbit1Begin System1717Orbit1End System1718Orbit1Begin System1718Orbit1End System1719Orbit1Begin System1719Orbit1End System1720Orbit1Begin System1720Orbit1End System1721Orbit1Begin System1721Orbit1End System1722Orbit1Begin System1722Orbit1End System1723Orbit1Begin System1723Orbit1End System1724Orbit1Begin System1724Orbit1End System1725Orbit1Begin Abstract: We report on the discovery of a speckle binary companion to the O7 V((f)) star 15~Monocerotis. A study of published radial velocities in conjunction with new measurements from KPNO and IUE suggests that the star is also a spectroscopic binary with a period of 25 years and a large eccentricity. Thus, 15 Mon is the first O star to bridge the gap between the spectroscopic and visual separation regimes. We have used the star's membership in the cluster NGC 2264 together with the cluster distance to derive masses of 34 and 19 solar masses for the primary and secondary, respectively. Several of the He- line profiles display a broad shallow component which we associate with the secondary, and we estimate the secondary's classification to be O9.5 Vn. The new orbit leads to several important predictions that can be tested over the next few years. System1725Orbit1End System49Orbit2Begin Abstract: The star HR 266 is thought to be a quadruple system of `Hierarchy 3'. The short--period binary, with components Ba and Bb, has a period of 4.241148+/-0.000008 days. The close pair orbits an unseen companion, Bc, with a period of 1769+/-10 days. This companion has been detected independently by spectroscopic and speckle observations. The long--period or visual orbit of this triple and component A has a period of 83.10+/-0.20 years. The speckle detection of Bc as a submotion in the long--period orbit represents the first detection of a ``speckle astrometric" system. Two possible models of the system's components are considered. The preferred model assumes that Bb is an A1V star with a mass of 2.25 solar masses. Then, Ba has a mass of 3.4+/-0.8 solar masses and a spectral type of B9IV. Component A is a B7IV star with an assumed mass of 5 solar masses. From the mass of Bb, the inclination of the short--period orbit is 54deg+/-5deg. Since the long--period orbit has an inclination of 54.9deg+/-1.1deg and the intermediate--period orbit appears to have an inclination of roughly 55deg+/-5deg, all three orbits may be coplanar. Component Bc has a minimum mass of 2.4 solar masses that increases to 2.8 solar masses if the intermediate--period orbit is coplanar. Such a value suggests that the Bc component's absorption features might be seen in our spectra, but this is not the case. Either Bc is a rapidly--rotating single star, similar to A, or Bc is actually a pair of late--type, lower--mass stars. The estimated distance to the system is 184 pc. System49Orbit2End System1726Orbit1Begin Abstract: The star HR 266 is thought to be a quadruple system of `Hierarchy 3'. The short--period binary, with components Ba and Bb, has a period of 4.241148+/-0.000008 days. The close pair orbits an unseen companion, Bc, with a period of 1769+/-10 days. This companion has been detected independently by spectroscopic and speckle observations. The long--period or visual orbit of this triple and component A has a period of 83.10+/-0.20 years. The speckle detection of Bc as a submotion in the long--period orbit represents the first detection of a ``speckle astrometric" system. Two possible models of the system's components are considered. The preferred model assumes that Bb is an A1V star with a mass of 2.25 solar masses. Then, Ba has a mass of 3.4+/-0.8 solar masses and a spectral type of B9IV. Component A is a B7IV star with an assumed mass of 5 solar masses. From the mass of Bb, the inclination of the short--period orbit is 54deg+/-5deg. Since the long--period orbit has an inclination of 54.9deg+/-1.1deg and the intermediate--period orbit appears to have an inclination of roughly 55deg+/-5deg, all three orbits may be coplanar. Component Bc has a minimum mass of 2.4 solar masses that increases to 2.8 solar masses if the intermediate--period orbit is coplanar. Such a value suggests that the Bc component's absorption features might be seen in our spectra, but this is not the case. Either Bc is a rapidly--rotating single star, similar to A, or Bc is actually a pair of late--type, lower--mass stars. The estimated distance to the system is 184 pc. System1726Orbit1End System718Orbit2Begin Abstract: Eta Virginis is a bright (V = 3.89) triple system of composite spectral type A2IV that has been observed for over a dozen years with both spectroscopy and speckle interferometry. Analysis of the speckle observations results in a long period of 13.1 years. This period is also detected in residuals from the spectroscopic observations of the 71.7919-day short-period orbit. Elements of the long-period orbit were determined separately using the observations of both techniques. The more accurate elements from the speckle solution have been assumed in a simultaneous spectroscopic determination of the short- and long-period orbital elements. The magnitude difference of the speckle components suggests that lines of the third star should be visible in the spectrum. In our blue and red spectra only the Mg II line at 4481 angstroms appears to show a third component, however, and it is a very broad and weak feature. The equatorial rotational velocities of the short-period pair are quite low, about 8 km/s each. System718Orbit2End System1727Orbit1Begin Abstract: Eta Virginis is a bright (V = 3.89) triple system of composite spectral type A2IV that has been observed for over a dozen years with both spectroscopy and speckle interferometry. Analysis of the speckle observations results in a long period of 13.1 years. This period is also detected in residuals from the spectroscopic observations of the 71.7919-day short-period orbit. Elements of the long-period orbit were determined separately using the observations of both techniques. The more accurate elements from the speckle solution have been assumed in a simultaneous spectroscopic determination of the short- and long-period orbital elements. The magnitude difference of the speckle components suggests that lines of the third star should be visible in the spectrum. In our blue and red spectra only the Mg II line at 4481 angstroms appears to show a third component, however, and it is a very broad and weak feature. The equatorial rotational velocities of the short-period pair are quite low, about 8 km/s each. System1727Orbit1End System559Orbit3Begin Quadruple system. Abstract: Visual, interferometric, and spectroscopic observations are presented for the nearby solar-type binary Fin 347 Aa. In a new solution combining both astrometric and spectroscopic data the orbital period is found to be 987.9 days or 2.7048 years, the semimajor axis 2.42 au or 0.116", the eccentricity 0.429, and the inclination 124.31deg. The masses and luminosities for this pair of G8V stars are 1.015+/-0.038 solar mass, 0.933+/-0.039 solar mass, 0.64+/-0.06 solar luminosity, and 0.62+/-0.06 solar luminosity, respectively. The orbital parallax of 0.0480"+/-0.0011" gives a distance of 20.84+/-0.47 pc. The small formal errors on all orbital elements leads to small errors for the masses and luminosities. The stars are found to be slightly over-massive and under-luminous for their spectral classifications. System559Orbit3End System1729Orbit1Begin Abstract: HD 202908 = ADS 14839 is a spectroscopic-visual triple system consisting of three solar-type stars. Eighteen years of spectroscopic observations including coverage of the recent periastron of 1987 January plus visual and speckle observations, the latter covering roughly the same interval as the radial velocities, have been used to obtain a simultaneous three-dimensional orbital solution. The short-period pair, Aa and Ab, has an orbital period of 3.9660465 days and a small but real eccentricity of 0.003. The visual pair, A and B, has an orbital period of 78.5 yr, and an eccentricity of 0.865. The solution yields masses for all three stars with uncertainties of about 2%, and the distance to the system with an uncertainty of 1.3%. Spectroscopic luninosity ratios, combined with the above distance, yield absolute magnitudes with uncertainties of about 0.1 mag. Thus the system provides three well-determined points on the mass-luminosity relationship. The inclinations of the short- and long-period orbits differ by 29deg, making the orbits non-coplanar. System1729Orbit1End System1730Orbit1Begin Abstract: HD 202908 = ADS 14839 is a spectroscopic-visual triple system consisting of three solar-type stars. Eighteen years of spectroscopic observations including coverage of the recent periastron of 1987 January plus visual and speckle observations, the latter covering roughly the same interval as the radial velocities, have been used to obtain a simultaneous three-dimensional orbital solution. The short-period pair, Aa and Ab, has an orbital period of 3.9660465 days and a small but real eccentricity of 0.003. The visual pair, A and B, has an orbital period of 78.5 yr, and an eccentricity of 0.865. The solution yields masses for all three stars with uncertainties of about 2%, and the distance to the system with an uncertainty of 1.3%. Spectroscopic luninosity ratios, combined with the above distance, yield absolute magnitudes with uncertainties of about 0.1 mag. Thus the system provides three well-determined points on the mass-luminosity relationship. The inclinations of the short- and long-period orbits differ by 29deg, making the orbits non-coplanar. System1730Orbit1End System1731Orbit1Begin Abstract: HR 6469 consists of an evolved G star and a close pair of stars, believed to be on the main sequence, the brighter of which is an early F star. Shallow eclipses have been detected in the close pair (Boyd et al. 1985), and the components of the wide system have been resolved over most of the orbit by speckle interferometry (McAlister & Hartkopf 1988). This paper presents radial velocities, obtained at the David Dunlap, McDonald, Kitt Peak and Dominion Astrophysical Observatories, for the G star and the primary of the close pair, along with solutions for elements of both the long- and short-period orbits, from those radial velocities and the speckle data, some of which have not previously been published. New spectrophotometry permits revisions of both the evolved star's spectral classification and the rotational velocity of the primary of the close pair, but not detection of the spectrum of the third component. These results, in combination with those from the light-curve solution of Van Hamme et al. (1993), enable us to determine the masses, radii and luminosities of all three stars, and to discuss the evolutionary state of the system. System1731Orbit1End System1732Orbit1Begin Abstract: HR 6469 consists of an evolved G star and a close pair of stars, believed to be on the main sequence, the brighter of which is an early F star. Shallow eclipses have been detected in the close pair (Boyd et al. 1985), and the components of the wide system have been resolved over most of the orbit by speckle interferometry (McAlister & Hartkopf 1988). This paper presents radial velocities, obtained at the David Dunlap, McDonald, Kitt Peak and Dominion Astrophysical Observatories, for the G star and the primary of the close pair, along with solutions for elements of both the long- and short-period orbits, from those radial velocities and the speckle data, some of which have not previously been published. New spectrophotometry permits revisions of both the evolved star's spectral classification and the rotational velocity of the primary of the close pair, but not detection of the spectrum of the third component. These results, in combination with those from the light-curve solution of Van Hamme et al. (1993), enable us to determine the masses, radii and luminosities of all three stars, and to discuss the evolutionary state of the system. System1732Orbit1End System1476Orbit2Begin Abstract: Interferometric, spectroscopic, astrometric, and photometric observations are presented for the nearby solar-type binary HR 6697. The system consists of a G0-2V primary and a K2-5V secondary. From a combined solution of the speckle and spectroscopic data the orbital period is 881 days or 2.41 years, the semimajor axis is 2.1 au, the eccentricity is 0.42, and the inclination is 68deg. The masses and luminosities are 1.16+/-0.12 solar masses, 0.77+/-0.05 sol. mass, 1.61+/-0.15 solar luminosity, and 0.17+/-0.05 solar luminosity. Two independent determinations of the parallax, a trigonometric parallax of 0.0379"+/-0.0030" and an orbital parallax of 0.0375"+/-0.0014", are in excellent agreement and give a mean distance of 26.6+/-0.9 pc. The system appears to be metal rich relative to the sun, and space motions do not identify it with any moving group. System1476Orbit2End System580Orbit2Begin Abstract: We present a three-dimensional solution for the orbit of the double star Omicron Leonis, based on new photoelectric radial velocity data mainly from the Observatoire de Haute-Provence and on interferometric data obtained with the Navy Prototype Optical Interferometer, the Mark III Stellar Interferometer, and the Palomar Testbed Interferometer. Omicron Leo's primary is a giant of type F9 and the secondary is an A5m dwarf, for which we derive masses of 2.12+/-0.01 solar masses and 1.87+/-0.01 solar masses , respectively. The distance to the binary is determined to be 41.4+/-0.1 pc. Combining the distance with the measured apparent magnitudes and color differences between the components yields luminosities of 39.4+/-2.4 solar luminosities and 15.4+/-1.0 solar luminosities for primary and secondary, respectively. Data from the Palomar Testbed Interferometer taken at 2.2 microns are used to constrain the photometry in the infrared. System580Orbit2End System1733Orbit1Begin Abstract: The G8 III star chi Andromedae, regarded as a probable spectroscopic binary for more than 70 years past, shares with an unseen companion an orbit of long period (21 years), small amplitude (3 km/s ), and moderate eccentricity (0.37). The companion seems likely to be a G or K dwarf. System1733Orbit1End System1734Orbit1Begin Abstract: HD 148224 is shown to be a spectroscopic binary with a presently unique combination of long period (nearly ten years) and small radial-velocity amplitude (1.5 km/s ) System1734Orbit1End System1522Orbit2Begin System1522Orbit2End System1735Orbit1Begin Abstract: HR 6797 is a fifth-magnitude F-dwarf system that was not recognized as a spectroscopic binary until 1966, when for the first time its spectrum was observed with sufficient dispersion to be seen, on occasion, as closely double-lined. It is now shown to consist of slightly unequal components in a somewhat eccentric orbit with a period of very nearly 200 days. The orbital inclination is 33 deg; the maximum angular separation is expected to be 0.019". There is a faint visual companion 7" away, so the system is at least triple. System1735Orbit1End System1736Orbit1Begin Abstract: 6 Ursae Majoris is a bright (5.5 mag) star of a type (G6 III) ideally suited to radial-velocity measurement, and it shows velocity variations of more than 25 km/s ; it has been known as a spectroscopic binary for nearly 80 years, and yet its orbit has never been determined until now. The period is very close to 1900 days, and the orbit is of high eccentricity (0.7). The mass function suggests that the secondary could well be a main-sequence F star. System1736Orbit1End System1737Orbit1Begin Abstract: 62 Ursae Majoris is a somewhat unequal pair of sixth-magnitude F stars. Its duplicity was first detected with the Haute-Provence Coravel by Geneva observers, who proceeded to determine its orbit. Its binary nature was also recognized at McDonald Observatory and reported to the Cambridge observer, who established the orbit independently. Now alerted to our joint interest, we combine to publish the orbit, which is very well determined and has quite an extreme eccentricity of 0.853 and a period of 267.5 days. The pair has been resolved by speckle interferometry; the observations show the inclination to be near 90deg but do not quantify it sufficiently accurately to decide whether eclipses are likely --- none has been noticed, but they have not yet been specifically looked for. Both stars, but particularly the primary, appear to be somewhat above the main sequence and are probably near the threshold of their giant-branch evolution. Despite the very high orbital eccentricity, the axial rotations of the stars appear to be pseudo-synchronized. There is a distant visual companion whose radial velocity is, as expected, different from that of\break 62 UMa itself. System1737Orbit1End System1738Orbit1Begin Abstract: HD 97810 is a `Clube Selected Areas' binary system close to the north celestial pole. It has a very eccentric orbit (e~0.73) and a period of 1164 days. Indirect evidence suggests a spectral type of K1 III. The object has been catalogued and repeatedly measured as a very close, equal, visual binary, but the author cannot see how to reconcile such a system with the radial-velocity observations. System1738Orbit1End System667Orbit2Begin The radial velocities of this quadruple systems are corrected for the outer orbit (Gamma= -15.50 km/s, K=4.33 km/s, P=21857 d, T=MJD 49735, e=0.412, omega1=127.3 d) System667Orbit2End System668Orbit2Begin The radial velocities of this quadruple systems are corrected for the outer orbit (Gamma= -14.87 km/s, K=4.85 km/s, P=21857 d, T=MJD 49735, e=0.412, omega1=307.3 d) System668Orbit2End System1739Orbit1Begin System1739Orbit1End System1740Orbit1Begin System1740Orbit1End System1741Orbit1Begin System1741Orbit1End System1742Orbit1Begin System1742Orbit1End System1743Orbit1Begin System1743Orbit1End System1744Orbit1Begin System1744Orbit1End System1745Orbit1Begin Abstract: 44 Leonis Minoris is shown to consist of two almost equal stars of types close to F3 IV, in an orbit with a period of 28.5 days and quite a high eccentricity (0.55). System1745Orbit1End System1746Orbit1Begin Abstract: HR 6313, a sixth-magnitude K3 giant, is shown to be a spectroscopic binary with a somewhat eccentric orbit whose period is close to 5000 days. System1746Orbit1End System1747Orbit1Begin Abstract: HD 51565/6, which used to be considered to show a composite spectrum, is an Am system recently discovered (by ourselves, among others) to be a visual binary. The components' disparity in brightness is something like one magnitude. Two velocities can be measured from radial-velocity traces; they vary in different periods, about 6.8 and 4.5 days, and doubtless belong to the brighter and fainter visual components respectively, each of which is therefore revealed to be a single-lined binary system. Both orbits are close to being circular, but that of the primary, which is naturally the better determined, has an eccentricity that is significant: although it is only 0.027, it is twenty times its standard deviation. System1747Orbit1End System1748Orbit1Begin Abstract: HD 51565/6, which used to be considered to show a composite spectrum, is an Am system recently discovered (by ourselves, among others) to be a visual binary. The components' disparity in brightness is something like one magnitude. Two velocities can be measured from radial-velocity traces; they vary in different periods, about 6.8 and 4.5 days, and doubtless belong to the brighter and fainter visual components respectively, each of which is therefore revealed to be a single-lined binary system. Both orbits are close to being circular, but that of the primary, which is naturally the better determined, has an eccentricity that is significant: although it is only 0.027, it is twenty times its standard deviation. System1748Orbit1End System1749Orbit1Begin Abstract: HR 7000, a double-lined F-type spectroscopic binary, is shown to have an eccentric orbit with a period of 40 days. The components are probably main-sequence stars, with spectral types close to F4~V and F6~V and rotations much faster than synchronous. System1749Orbit1End System1750Orbit1Begin Abstract: HR 2918 is a double-lined spectroscopic binary consisting of an almost equal pair of stars, slightly earlier in type than the Sun, in a low-eccentricity orbit with a period of about 26 days. The minimum masses are about 1.1 solar mass, so eclipses are not improbable. The stars rotate slowly, but whether their rotations are related to the orbital period remains uncertain. System1750Orbit1End System1751Orbit1Begin Abstract: HD 150932, a late-type star about which almost nothing has previously been known, is shown to be a spectroscopic binary with a period of about 23 years. System1751Orbit1End System1752Orbit1Begin Abstract: HD 158209 is a triple system exhibiting two late-type spectra. The dominant component of the spectrum shows a substantial radial-velocity variation in a period of 22 days; in addition, the -velocity changes with a periodicity of 8 years. The very weak secondary component moves in anti-phase with the long-period variation of the primary, identifying it as a single star in the 'outer' orbit of the triple system. The primary is the only visible member of the 22-day binary sub-system that constitutes the other component in that orbit. There is evidence from the parallax, spectral classification, and proper motion that HD 158209 is a main-sequence system; it is not incontrovertible evidence, but taken together it is quite strong. Unfortunately we are unable to present a model in which all the components are on the main sequence, because the orbital elements demand minimum masses that are too large. It is difficult to avoid the conclusion that the primary is a subgiant, the other components being about G8 V and mid-K V. The forthcoming Hipparcos parallax should be very informative. System1752Orbit1End System1753Orbit1Begin Abstract: HD 158209 is a triple system exhibiting two late-type spectra. The dominant component of the spectrum shows a substantial radial-velocity variation in a period of 22 days; in addition, the -velocity changes with a periodicity of 8 years. The very weak secondary component moves in anti-phase with the long-period variation of the primary, identifying it as a single star in the 'outer' orbit of the triple system. The primary is the only visible member of the 22-day binary sub-system that constitutes the other component in that orbit. There is evidence from the parallax, spectral classification, and proper motion that HD 158209 is a main-sequence system; it is not incontrovertible evidence, but taken together it is quite strong. Unfortunately we are unable to present a model in which all the components are on the main sequence, because the orbital elements demand minimum masses that are too large. It is difficult to avoid the conclusion that the primary is a subgiant, the other components being about G8 V and mid-K V. The forthcoming Hipparcos parallax should be very informative. System1753Orbit1End System1754Orbit1Begin System1754Orbit1End System1755Orbit1Begin Abstract: HR 2236 is a sixth-magnitude object with the spectrum of a mid-F main- sequence star. It has been known for half a century to be a very close visual binary; it has a tolerably well established orbit with a period of about 30 years. Thirty years ago it was found to exhibit a double-lined spectrum, implying that the system is of higher multiplicity. It is now shown to be triple-lined, consisting of three components all of comparable luminosities and spectral types: the visual primary is itself a double-lined binary system with a circular orbit whose period is a little more than 2 days. The large amplitude of the velocity changes in the 2-day orbit permits the relative velocities of the visual pair to be measured accurately, so in due course the 30-year orbit, too, should become well determined in all three dimensions. System1755Orbit1End System1756Orbit1Begin Abstract: HR 6985 is a fifth-magnitude F-type star which has been known for ten years to be double-lined. It is now shown to consist of somewhat unequal components in a circular orbit with an unusually short period of slightly under 36 hours. The orbital inclination is only 8 degrees. System1756Orbit1End System1757Orbit1Begin System1757Orbit1End System1758Orbit1Begin Abstract: HD 483 is a double-lined spectroscopic binary system with an eccentric orbit whose period is 23.5 days. It has feature in the literature as a Hertzsprung-gap giant of spectral type G2III, but we think it has been misclassified and is really a pair of main-sequence stars of approximately solar type. The inclination if thought to be high, but there are no eclipses. System1758Orbit1End System1759Orbit1Begin Abstract: HD 99903 is shown to be a double-lined system with a 61-day orbit of modest eccentricity. The other astrophysical data on it, consisting only of its HD spectral type of K0 and its magnitudes on the International system, are consonant with its being a main-sequence pair, as is also suggested by its non-zero eccentricity and the undetectably small rotation of both components. The masses of the individual components are, however, considerably in excess of 1 M and furthermore they are very similar to one another despite the substantial disparity in the depths of the two dips on radial-velocity traces. It therefore seems inescapable that the system consists of a pair of evolved stars, but the writer cannot explain why tidal effects have neither circularized the orbit nor synchronized the rotations of the stars with the orbital period.Spectroscopic and photometric observations are evidently very desirable. System1759Orbit1End System1760Orbit1Begin This orbit is part of a combined spectroscopic-interferometric solution. System1760Orbit1End System1761Orbit1Begin This orbit is part of a combined spectroscopic-interferometric solution. System1761Orbit1End System1762Orbit1Begin This orbit is part of a combined spectroscopic-interferometric solution. System1762Orbit1End System1763Orbit1Begin The criteria of Lucy & Sweeney (1971) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity, thus, omega is undefined. System1763Orbit1End System1764Orbit1Begin The criteria of Lucy & Sweeney (1971) indicate that the eccentric-orbit solution is to be prefered. System1764Orbit1End System634Orbit2Begin Radial velocity orbit derived using the HeII 4686 line for the primary O3.5V component and the HeI 4471 line for the secondary O8V. O-C values from the orbital fit are given as radial velocity errors. The system shows evidence of apsidal motion with 185 +/- 16 years period. System634Orbit2End System634Orbit3Begin Radial velocity orbit obtained from the HeI 4471 line measured in both components.O-C values from the orbital fit are given as radial velocity errors. System634Orbit3End System634Orbit4Begin Radial velocities and orbit calculation from the HeII 4686 line measured in both components. O-C values from the orbital fit are given as radial velocity errors. System634Orbit4End System1765Orbit1Begin Eclipsing binary in SMC. T is the time for primary minimum. O-C values from the orbital fit are given as radial velocity errors. Orbital inclination: 57 +/- 3 degrees. Individual parameters are: M1 = 25 +/- 3, R1 = 10.1 +/- 0.4, M2 = 16 +/- 2, R2 = 8.4 +/- 0.3, solar units. System1765Orbit1End System1766Orbit1Begin Circular orbit assumed. T is the time of maximum radial velocity. System1766Orbit1End System1021Orbit2Begin O-C values from the orbital fit are given as radial velocity errors. System1021Orbit2End System1768Orbit1Begin System1768Orbit1End System1769Orbit1Begin Triple-lined system. Orbital parameters for the close pair,designed a+c in reference. T corresponds to the conjunction with the most massive star (component `a') being behind its companion. The systemic velocity for the secondary component is -3.2 +/- 5.9. Orbital solution computed only from data near quadratures (other are assigned 0.0 weight). O-C values from the fit are given in the error column. Orbital parameters for component b are given separately. System1769Orbit1End System1770Orbit1Begin Triple-lined system. Orbital parameters for component labeled as b in reference, making a triple system with the close pair a+c. O-C values from the orbtial fit given in the error column. An orbital period of 1340.5 days is also possible; the corresponding orbital parameters are given separately. System1770Orbit1End System1770Orbit2Begin Triple-lined system. Orbital parameters for component b, making a triple system with the close pair a+c. O-C values from the orbital fit given in the error column. An orbital period of 285.1 days is also possible; the corresponding orbital parameters are given separately. System1770Orbit2End System1771Orbit1Begin Orbital parameters derived from high resolution echelle-CCD spectra. O-C values from the orbital fit are given as radial velocity errors. The orbital period was derived considering a large database containing lower resolution observations not included in the orbital fit. System1771Orbit1End System1772Orbit1Begin Circular orbit assumed. Only observations near quadrature phases were used in the orbital calculation. T is the time of maximum radial velocity of the primary component. O-C from the orbital fit given as errors. System1772Orbit1End System1773Orbit1Begin Closest pair in quadruple system. Three sets of lines in the spectrum. Orbital parameters for the third component are given separately. O-C from the orbital fit quoted in the error column. System1773Orbit1End System1774Orbit1Begin Single lined binary in quadruple system. Triple lines in the spectrum. Orbital elements for the closest pair (a + b) are given separately. O-C from the orbital fit are quoted in the error column. System1774Orbit1End System1040Orbit2Begin Radial velocities and orbital elements for the O-type absorption line spectrum. The period was obtained by fitting the radial velocity variations of both the Wolf-Rayet emission lines and the O-type absorption lines. System1040Orbit2End System1775Orbit1Begin asini = 14740000 plus or minus 40000 km f(m) = 0.06146 plus or minus 0.00047 solar masses System1775Orbit1End System1776Orbit1Begin Double lined binary, but the authors are unable to measure secondary spectrum. Three previous observations by Neubauer (1932) included in the orbital calculation. System1776Orbit1End System1777Orbit1Begin O-C values from the orbital fit given as errors. System1777Orbit1End System1778Orbit1Begin O-C values from the orbital fit given as errors. System1778Orbit1End System1779Orbit1Begin O-C values from the orbital fit given as errors. System1779Orbit1End System1780Orbit1Begin O-C from the orbital fit given as errors. System1780Orbit1End System1781Orbit1Begin O-C values from the orbital fit given as errors. System1781Orbit1End System1782Orbit1Begin O-C values from the orbital fit given as errors. System1782Orbit1End System1783Orbit1Begin O-C from the orbital fit given as errors. System1783Orbit1End System631Orbit2Begin Radial velocities collected from the literature also used in the orbit calculation. No errors given. Internal standard deviation of a single observation is about 15 km/s. System631Orbit2End System1784Orbit1Begin Subsequent studies by Solivella & Niemela (1999RMxAC...8..145S) and Freyhammer et al. (2001A&A...369..561F) demonstrated the orbital period is indeed 1.47 days. The later also found this is an eclipsing system and performed a simultaneous radial velocity and light curve solution, determining physical parameters for the component stars. System1784Orbit1End System1769Orbit2Begin Later work by Rauw et al. (2001MNRAS.326.1149R) showed this is a triple system presenting also light variations. System1769Orbit2End System1785Orbit1Begin O-C values from the orbital fit given as errors. System1785Orbit1End System1786Orbit1Begin O-C values from the orbital fit given as errors. System1786Orbit1End System1787Orbit1Begin O-C values from the orbital fit given as errors. Circular orbit assumed. T is the time of maximum radial velocity. System1787Orbit1End System1788Orbit1Begin Circular orbit assumed. O-C values from the orbital fit given as errors. T is the time of maximum radial velocity. System1788Orbit1End System1789Orbit1Begin O-C values from the orbital fit given as errors. Circular orbit assumed. T is the time of maximum radial velocity. System1789Orbit1End System1790Orbit1Begin Circular orbit assumed. T is the time of maximum radial velocity. O-C values from the orbital fit given as errors. System1790Orbit1End System1791Orbit1Begin O-C values from the orbital fit given as errors. System1791Orbit1End System1792Orbit1Begin Circular orbit assumed. T is the time of maximum radial velocity. O-C values from the orbital fit given as errors. System1792Orbit1End System1793Orbit1Begin A previous orbit by Balona, L. A., 1987, South African Astron. Obs. Circ., 11, 1, resulted in a period of 15.05 days, which is one half the value of the correct period. His 36 SAAO radial velocities listed by the source B87 were given zero weight in the current orbital solution. Balona's velocity of HJD = 2444244.299 is not listed because the orbital velocity residual is quite large, suggesting that the velocity may be a missprint or belong to another star. asini = 4495000 +/- 45000 km f(m) = 0.00400 +/- 0.00012 solar masses System1793Orbit1End System1794Orbit1Begin The system is a symbiotic binary consisting of an M giant and a probable hot compact companion. Separate orbits were computed for the primary and secondary. Radial velocities of the primary were measured from absorption lines in the infrared. Radial velocities of the hot secondary star were determined from the ultraviolet emission lines measured by Gonzalez-Riestra et al. (1990, A&A, 237, 385). Thus, the semi-amplitude K2 is not from a double-lined orbital solution but rather from an independent orbit computed with the ultraviolet velocities. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 70000000 +/- 260000 km f(m) = 0.0239 +/- 0.0026 solar masses System1794Orbit1End System1263Orbit2Begin The system is a symbiotic binary consisting of an M giant and a probable hot compact companion. Radial velocities were measured from absorption lines in the infrared. The orbital period was adopted from Schild & Schmid (1997, A&A, 324, 606). The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 103300000 +/- 3400000 km f(m) = 0.0481 +/- 0.0047 solar masses System1263Orbit2End System1795Orbit1Begin The system is a symbiotic binary consisting of an M giant and a probable hot compact companion. Radial velocities were measured from absorption lines in the infrared. The criteria of Lucy and Sweeney (1971, AJ, 76, 644) indicate that the eccentric-orbit solution is to be preferred, but the results are relatively close to the dividing lines of both tests. asini = 16330000 +/- 740000 km f(m) = 0.00086 +/- 0.00012 solar masses System1795Orbit1End System1796Orbit1Begin Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. a1sini = 2296200 +/- 3900 km a2sini = 2307400 +/- 3800 km M1 (sin)3 i = 0.8365 +/- 0.0031 solar masses M2 (sin)3 i = 0.8303 +/- 0.0031 solar masses System1796Orbit1End System1797Orbit1Begin The system is a Symbiotic binary. Radial velocities were measured from absorption lines in the infrared. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 70300000 +/- 4500000 km f(m) = 0.024 +/- 0.005 solar masses System1797Orbit1End System884Orbit4Begin The system is a Symbiotic binary. Radial velocities were measured from absorption lines in the infrared. The period was determined by combining three earlier sets of radial velocities with the above velocities. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 44200000 +/- 2300000 km f(m) = 0.0115 +/- 0.0018 solar masses System884Orbit4End System1798Orbit1Begin The system is a Symbiotic binary. Radial velocities were measured from absorption lines in the infrared. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 20800000 +/- 1700000 km f(m) = 0.00100 +/- 0.00024 solar masses System1798Orbit1End System1799Orbit1Begin The system is a Symbiotic binary. Radial velocities were measured from absorption lines in the infrared. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 73000000 +/- 1900000 km f(m) = 0.0333 +/- 0.0027 solar masses System1799Orbit1End System1800Orbit1Begin The system is a Symbiotic binary. Radial velocities were measured from absorption lines in the infrared. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 60300000 +/- 2300000 km f(m) = 0.0218 +/- 0.0025 solar masses System1800Orbit1End System42Orbit2Begin The system is a Symbiotic binary. Unit weight radial velocities were measured from absorption lines in the infrared. Other velocities are from the literature. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 48600000 +/- 1800000 km f(m) = 0.0196 +/- 0.0022 solar masses System42Orbit2End System877Orbit2Begin The system is a Symbiotic binary. Unit weight radial velocities were measured from absorption lines in the infrared. Other velocities are from the literature. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 74770000 +/- 530000 km f(m) = 0.3224 +/- 0.0068 solar masses System877Orbit2End System1179Orbit2Begin The system is a Symbiotic binary. Unit weight radial velocities were measured from absorption lines in the infrared. Other velocities are from the literature. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the eccentric-orbit solution is to be prefered over a circular-orbit solution. asini = 78200000 +/- 3500000 km f(m) = 0.0262 +/- 0.0035 solar masses System1179Orbit2End System451Orbit2Begin The system is a Symbiotic binary. System451Orbit2End System996Orbit2Begin The system is a Symbiotic binary. Unit weight radial velocities were measured from absorption lines in the infrared. Other velocities are from the literature. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. Thus, omega is undefined. asini = 104700000 +/- 6100000 km f(m) = 0.221 +/- 0.038 solar masses System996Orbit2End System1335Orbit2Begin The system is a Sumbiotic binary. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the eccentric-orbit solution is to be prefered. asini = 60800000 +/- 2300000 km f(m) = 0.0135 +/- 0.0015 solar masses System1335Orbit2End System258Orbit2Begin The following data are used: P: Palomar 5m telescope (Hartmann et al. 1981, ApJ, 249, 662); H: Heintz W.D., 1981, ApJS, 46, 247; K: KPNO Coude (Hartmann et al. 1981, ApJ, 249, 662); M: Mount-Hopkins echelle (Hartmann et al. 1981, ApJ, 249, 662); RVM: Radial-Velocity-Meter, this work Weights are inversely proportional to the System258Orbit2End System1801Orbit1Begin System1801Orbit1End System1638Orbit2Begin Radial velocities from Beavers & Eitter (1986 ApJS, 62, 147) are marked. Compared to the 1991 paper, more unpublished data from the RVM instrument (after JD 2448117) are added. System1638Orbit2End System1802Orbit1Begin Radial velocities from Beavers & Eitter (1986 ApJS, 62, 147) are marked. System1802Orbit1End System1803Orbit1Begin System1803Orbit1End System1162Orbit3Begin Combined spectroscopic-interferometric orbit. Radial velocities from MacClure et al. (1983, PASP, 95, 201) are marked as 'MCl'. System1162Orbit3End System1480Orbit3Begin Combined spectroscopic-visual orbit, only few radial velocities. System1480Orbit3End System1804Orbit1Begin Small eccentricityy is significant. Blended dips (marked '+b') are not used in the orbital solution. System1804Orbit1End System1475Orbit2Begin Combined spectroscopic-interferometric orbit. The orbital elements were obtained by direct fitting to the blended correlation dips, without explicit derivation of the radial velocities. System1475Orbit2End System136Orbit3Begin Combined spectro-interferometric orbit: major semiaxis (arcsec) 0.05338 +- 0.00052, position angle of ascending node (deg) 49.29 +- 0.42. Codes for types of observations: (P) DAO photographic; (SF) DAO spectrometer with F star mask; (SK) DAO spectrometer with K star mask; (K) KPNO CCD. The following amounts have been added to the raw DAO spectrometer data to give the results in this table, which are in the system of Scarfe et al. 1990: SF, -0.8 km s-1; SK, 0.4 km s-1. A colon following the above code indicates an observation rejected from the final solution because it produced a large residual in a preliminary one. System136Orbit3End System1796Orbit2Begin -Ellipticity is "assumed" in the paper. -HD 95559 is possibly a triple system. However, no evidence for a third component in spectra. System1796Orbit2End System1805Orbit1Begin This is a triple system. Spectroscopic orbit refers to the primary component of ADS 14859 visual binary, Cepheid. Pulsational component of radial velocity was subtracted using the "pseudo-orbit" with the following parameters: P = 3.3325099 +- 0.000013 d T = 2444370.0 +- 0.3 JD e = 0.05 +- 0.03 omega = 92.2 +- 35.5 deg. Weights of old observations (not included here) are 0.1, weights of modern CCD observations are 1.0. RVs have been corrected for different zero-points by adding the correction as indicated in the notes ("Corr."). Unknown RV errors are replaced by zeroes. System1805Orbit1End System1021Orbit3Begin Star belongs to NGS 6523 = M8. Radial velocities are from IUE. The 6.14d orbit of Morrison and Conti (1978) is revised here. System1021Orbit3End System1806Orbit1Begin Radial velocities from CfA (Pilachowski et al. 1989) are marked as "CfA", the remaining data are from CORAVEL. System1806Orbit1End System1807Orbit1Begin Radial velocities from CfA (Pilachowski et al. 1989) are marked as "CfA", the remaining data are from CORAVEL. Only one orbital cycle is covered. System1807Orbit1End System1808Orbit1Begin Radial velocities from CfA (Pilachowski et al. 1989) are marked as "CfA", the remaining data are from CORAVEL. Only one orbital cycle is covered. System1808Orbit1End System1809Orbit1Begin The average internal error is 0.86 km/s. System1809Orbit1End System1810Orbit1Begin Observations are from Palomar (P) and from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were wighted 0.3 relative to other data. System1810Orbit1End System1811Orbit1Begin Observations are from Palomar (P) and from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were wighted 0.3 relative to other data. System1811Orbit1End System1812Orbit1Begin Weak secondary is observed in cross-correlation but not processed for the SB solution. Observations are from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were wighted 0.3 relative to other data. System1812Orbit1End System1813Orbit1Begin Observations are from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). System1813Orbit1End System1814Orbit1Begin Observations are from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). System1814Orbit1End System1815Orbit1Begin This orbit refers to the "sharp-lined" component of the triple system S1082, also called "B". Other component is a close system of 1.0677978 day period, see ... T = Tillinghast reflector; M = MMT. System1815Orbit1End System1816Orbit1Begin Observations are from CORAVEL (C) and from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were wighted 0.3 relative to other data. System1816Orbit1End System1817Orbit1Begin Observations are from CORAVEL (C) and CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were wighted 0.3 relative to other data. System1817Orbit1End System1818Orbit1Begin Observations are from Palomar (P) and CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1818Orbit1End System1819Orbit1Begin Observations are from Palomar (P), CORAVEL (C) and from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1819Orbit1End System1820Orbit1Begin Observations are from Palomar (P) and from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1820Orbit1End System1821Orbit1Begin This is a spectroscopic triple star, with two system of lines visible: the SB1 (of which the orbit is given here) and a tertiary with a constant RV with a mean of 35.2 km/s. Blended dips were split by fitting a double Gaussian. Unsplit dips (marked :) are not used in the orbit solution. Observations are from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1821Orbit1End System1822Orbit1Begin Observations are Palomar (P) and from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1822Orbit1End System1823Orbit1Begin Observations are from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1823Orbit1End System1824Orbit1Begin Observations are from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1824Orbit1End System1825Orbit1Begin Observations are from Palomar (P), CORAVEL (C) and from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1825Orbit1End System1826Orbit1Begin Observations are from Palomar (P) and from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1826Orbit1End System1827Orbit1Begin Non-member of the M67 cluster. Observations are from CfA digital RV spectrometers at MMT (M) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1827Orbit1End System1828Orbit1Begin Observations are from Palomar (P), CORAVEL (C) and from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1828Orbit1End System1829Orbit1Begin Observations are from CfA digital RV spectrometers at MMT (M), Weyeth 1.5m (W) and Tillinghast 1.5m (remaining). The Tillinghast data were weighted 0.3 relative to other data. System1829Orbit1End System1830Orbit1Begin Proper-motion non-member. Observations at Palomar are marked "P" (adjusted zero point, weight4), all other observations -- weight 1: "C" -- CORAVEL, "V" -- Dominion observatory (Victoria), remaining observations are from the Cambridge radial velocity spectrometer. System1830Orbit1End System1831Orbit1Begin Observations marked as "M" were obtained at MMT, weight 1. Remaining observations are from the Tillinghast 1.5m telescope, weight 0.3. System1831Orbit1End System1832Orbit1Begin Observations marked as "M" were obtained at MMT, weight 1. Remaining observations are from the Tillinghast 1.5m telescope, weight 0.3. System1832Orbit1End System1833Orbit1Begin System1833Orbit1End System1834Orbit1Begin This id the short-priod sub-system of S1082 that contains a tertiary component with 1188.5-d period. Two stars in this system are blue stragglers. Radial velocities from Sandquist et al. (2003AJ....125..810S) obtained at McDonald observatpry are listed here, although they were not used in the orbit computing. The latter authors argue that the orbit may be eccentric, but do not provide the elements. The center-of-mass velocity listed is relative. T0 in the original paper is likely to refer to the time of the primary eclipse, that is why omega is here listed as 90deg. System1834Orbit1End System1835Orbit1Begin Zero-point corrections from -7.7 to 10.6 km/s are applied to each observation, all corrections for BMES94 are +1.3 km/s. Lines of the tertiary component C are also observed in the spectrum, but no orbit is given. The T0 listed in the paper does not correspond to time of maximum velocity as indicated. The value given here is more likely to be so. System1835Orbit1End System1835Orbit2Begin C95 - data from Casey et al. (1995AJ....109.2156C). Semi-amplitudes K1 and K2 are not given in the publication, re-calculated from the masses. The errors used in fitting the orbit are 2 km/s for the primary, 10 km/s for the secondary and for the data of Casey et al. System1835Orbit2End System1836Orbit1Begin C95 - data from Casey et al. (1995AJ....109.2156C). The errors used in fitting the orbit are 10 km/s for all velocities. Semi-amplitudes K1 and K2 are not given in the publication, re-calculated from the masses. Five orbits with periods from 126 to 270 days are given by the authors, the best-fitting orbit is given here. The "primary" is the center-of-mass of the system AB calculated from the mass ratio as V_AB = (3*V_A + 1.6*V_B)/4.6, the "secondary" is the third component C. System1836Orbit1End System1010Orbit2Begin In addition to the IUE (international Ultraviolet Explorer) spectra, we also obtained seven optical spectra in the range 3804-4220A. These spectra were made with the MSO (Mount Stromlo Observatory) 74 inch telescope and coude spectrograph using grating C (600 grooves mm-1, blazed at 12500A in first order) in third order with a BG12 order-sorting filter. - SWP: short-wavelength prime camera spectra from IUE. System1010Orbit2End System343Orbit2Begin Orbital elements were fitted to the primary RVs, only K2 and V0=20.4 +- 2.1 km/s were then found for the secondary. Weights are inversely proportional to the errors. The period 29.13434 +- 0.00020 d was determined using the data of Hilditch et al. (1991). The longitude of periastron changes because of line-of-apsides rotation. System343Orbit2End System1272Orbit2Begin -Also: O6.5 III for primary spec. type. -They set the weights of the International Ultraviolet Explorer (IUE), Canada-France-Hawaii Telescope (CFHT), and Kitt Peak National Observatory (KPNO) measurements to unity, and all the other measurements were assigned a weight of 0.05. This weight is approximately equal to the square of the ratio of the errors between the high-quality and the subsidiary measurements. The subsidiary measurements have a larger scatter as a result of a lower S/N and the use of line samples with significant line-to-line velocity differences. System1272Orbit2End System1837Orbit1Begin The orbit is based mostly on speckle data. The element K1 was not given in the publication, calculated from the author's data with other elements fixed. RV obtained from H-alpha line. The low-resolution Skinakas data are not suitable for the RV measurements. The BOL data do not resolve the double-peaked Halpha structure. The Ritter data marked with a colon have the lowest S/N ratio. -Rit: Ritter Observatory -CAO: 2.6m Shajn telescope of the Crimean Astrophysical Observatory (Ukraine) -ESO: 1.52m telescope at the ESO (La Silla, Chile) -Ski: Skinakas Observatory (Crete, Greece) -BOL: Cassini telescope at the Loiano Observatory (BOL, Italy) System1837Orbit1End System1767Orbit1Begin The radial velocities are related to the CORALIE standard system. CORALIE high-resolution fiber-fed echelle spectrograph (Queloz et al. 2000) was mounted on the Nasmyth focus on the 120 cm New Swiss telescope at La Silla (ESO, Chile). System1767Orbit1End System1838Orbit1Begin System1838Orbit1End System1839Orbit1Begin System1839Orbit1End System1840Orbit1Begin System1840Orbit1End System1841Orbit1Begin System1841Orbit1End System1842Orbit1Begin System1842Orbit1End System1843Orbit1Begin System1843Orbit1End System1844Orbit1Begin System1844Orbit1End System1845Orbit1Begin System1845Orbit1End System1846Orbit1Begin System1846Orbit1End System1847Orbit1Begin System1847Orbit1End System1848Orbit1Begin System1848Orbit1End System1849Orbit1Begin System1849Orbit1End System1850Orbit1Begin System1850Orbit1End System1851Orbit1Begin System1851Orbit1End System12Orbit2Begin This orbit supercedes the earlier paper 4, 1988Obs...108..174S. Radial velovities are on the international scale and are derived by cross-correlation from the IUE spectra. System12Orbit2End System411Orbit2Begin This orbit supercedes the earlier paper 2, 1987Obs...107...68S. Radial velovities are on the international scale and are derived by cross-correlation from the IUE spectra. The secondary component is detected in cross-correlation, but does not fit any sensible orbit. System411Orbit2End System443Orbit2Begin This orbit supercedes the earlier paper 5, 1989Obs...109...74S. Radial velovities are on the international scale and are derived by cross-correlation from the IUE spectra. The secondary RVs were used only to derive K2. System443Orbit2End System974Orbit2Begin Member of the young cluster NGC 6383. The period is derived by combining the new observations with historical data and then fixed in the orbital solution. System974Orbit2End System676Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. The data affected by the eclipses were given zero weight. System676Orbit2End System1852Orbit1Begin Radial velocities are derived from the IUE spectra by cross-correlation. The systemic velocity given refers to the primary, for the secondary it was found to be -60.0 +- 2.6 km/s. System1852Orbit1End System927Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. The star belongs to the NGC 6231 cluster. System927Orbit2End System1853Orbit1Begin The star belongs to the NGC 2244 cluster. Radial velocities are derived from the IUE spectra by cross-correlation. System1853Orbit1End System873Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System873Orbit2End System1037Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System1037Orbit2End System925Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System925Orbit2End System1021Orbit4Begin Radial velocities are derived from the IUE spectra by cross-correlation. System1021Orbit4End System444Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System444Orbit2End System186Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System186Orbit2End System489Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System489Orbit2End System1854Orbit1Begin Radial velocities are derived from the IUE spectra by cross-correlation. Elements are obtained by combining the IUE data with Levato et al. (1988 ApJS 68 319) data. System1854Orbit1End System1855Orbit1Begin -Observations: High resolution (10 km s^-1), each covering a region 45 Angstroms wide centered on 5187 Angstroms (or in few cases, 5197 Angstroms), were obtained with nearly identical echelle spectrographs and photo-counting detectors at three different telescopes: 1.5m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), the 1.5m Wyeth reflector at the Oak Ridge Observatory (ORO), and the Multiple Mirror Telescope (MMT). System1855Orbit1End System1856Orbit1Begin - Most data obtained at Multiple Mirror Telescope, 1.5m Tillinghast reflector at the Fred L. Whipple Observatory, the 1.5m Wyeth reflector at Oak Ridge Observatory and the Hale 5m telescope. RVs are recuperated from the WEBDA database and are extended compared to the original publication. System1856Orbit1End System1857Orbit1Begin Data obtained at Multiple Mirror Telescope, 1.5m Tillinghast reflector at the Fred L. Whipple Observatory, the 1.5m Wyeth reflector at Oak Ridge Observatory and the Hale 5m telescope. RVs are recuperated from the WEBDA database and are extended compared to the original publication. System1857Orbit1End System1858Orbit1Begin -Single-lined naked T-Tauri binary (NTTS). -Data obtained in the 1.5m Tillinghast reflector (T) at the Fred L. Whipple Observatory and the Multiple Mirror Telescope (M) -No Simbad entry found. System1858Orbit1End System1859Orbit1Begin -Single-lined naked T-Tauri binary (NTTS). -Data obtained at the 1.5m Tillinghast reflector (T) at the Fred L. Whipple Observatory and the Multiple Mirror Telescope (M) System1859Orbit1End System1860Orbit1Begin -Single-lined naked T-Tauri Star (NTTS) binary -Data obtained in the 1.5m Tillinghast reflector (T) at the Fred L. Whipple Observatory and the Multiple Mirror Telescope (M) System1860Orbit1End System1861Orbit1Begin -Double-lined NTTS (naked T-Tauri) binary -Data obtained in the 1.5m Tillinghast reflector (T) at the Fred L. Whipple Observatory and the Multiple Mirror Telescope (M) System1861Orbit1End System1862Orbit1Begin -Single-lined naked T-Tauri Star (NTTS) binary -Data obtained in the 1.5m Tillinghast reflector (T) at the Fred L. Whipple Observatory and the Multiple Mirror Telescope (M) -No aliases found in Simbad System1862Orbit1End System1863Orbit1Begin -NIR = Near Infrared observations -Spectral classification of the primary has an uncertainty of less than one subtype. System1863Orbit1End System1864Orbit1Begin -Single-lined spectroscopy binary; a classical T Tauri. -The measured eccentricity of the orbit is not distinguishable from zero, although the measurement error is fairly large. -Data taken using: 1.5m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO) and the Multiple Mirror Telescope (MMT) System1864Orbit1End System1865Orbit1Begin -Double-lined binary; classical T Tauri. --Data obtained at Multiple Mirror Telescope(M), 10m Keck telescope at Mauna Kea(K), 3m telescope at Lick Obsevatory(L), 2.7m (McD) and 2.1m(Mc) 1m telescopes at MacDonald Observatory. -Authors recommend to use orbital data taken with CfA instead of CfA + LKM (Lick,Keck, McDonald), because the former set of data is biased. -n1 and n2 are refered to the total number of telescope observations. In this paper not all the observations have RV1, RV2 results. System1865Orbit1End System912Orbit2Begin -Data taken using CfA (Center for Astrohysics, Harvard) Digital Speedometer on the 1.5m Tillinghast reflector at the Whipple Observatory on Mount Hopkins, Arizona. -To derive the velocities simultaneusly for both components they used TODCOR, a new two-dimensional correlation technique. System912Orbit2End System1866Orbit1Begin System1866Orbit1End System1867Orbit1Begin System1867Orbit1End System1868Orbit1Begin System1868Orbit1End System1869Orbit1Begin System1869Orbit1End System1550Orbit2Begin System1550Orbit2End System1870Orbit1Begin System1870Orbit1End System1871Orbit1Begin System1871Orbit1End System1872Orbit1Begin System1872Orbit1End System1873Orbit1Begin System1873Orbit1End System1874Orbit1Begin System1874Orbit1End System1875Orbit1Begin System1875Orbit1End System1876Orbit1Begin System1876Orbit1End System1877Orbit1Begin System1877Orbit1End System1878Orbit1Begin System1878Orbit1End System1879Orbit1Begin System1879Orbit1End System1880Orbit1Begin System1880Orbit1End System1881Orbit1Begin System1881Orbit1End System1882Orbit1Begin System1882Orbit1End System1883Orbit1Begin System1883Orbit1End System1884Orbit1Begin System1884Orbit1End System1885Orbit1Begin System1885Orbit1End System1886Orbit1Begin System1886Orbit1End System1887Orbit1Begin System1887Orbit1End System1888Orbit1Begin System1888Orbit1End System1889Orbit1Begin System1889Orbit1End System1890Orbit1Begin System1890Orbit1End System541Orbit2Begin System541Orbit2End System1891Orbit1Begin System1891Orbit1End System1892Orbit1Begin System1892Orbit1End System1893Orbit1Begin System1893Orbit1End System1894Orbit1Begin System1894Orbit1End System1895Orbit1Begin System1895Orbit1End System1896Orbit1Begin -In our orbital solution, we assumed the orbital period following the 1985 edition of the General Catalogue of Variable Stars, P = 0.4942624 days. The O-C deviation for the primary eclipse epoch T0 is relatively large and equals 0.0206 days, which is much larger than the error of determination of T0. This shift may be partly due to an obvious asymmetry in the radial velocity curve of the less massive component in the first half of the orbital cycle System1896Orbit1End System1897Orbit1Begin - Bond (1975, PASP 87, 877) noted diffuse spectral lines and then obtained a fragmentary light curve indicating that the star is a W UMa-type binary. Since then, the binary has been the subject of several time-of-minima studies, the most recent one by Muyesseroglu, Gurol, & Selam,1996,Inf. Bull. Variable Stars, No. 4380. We have taken the value of the period, P = 0.3551501 days, from the study of Aslan & Derman (1986, Ap&SS 66, 281). System1897Orbit1End System1898Orbit1Begin - "a" means that half-weigh is given in the orbital solution for RV1 -We adopted P = 0.470691 days for our data, a number based on the values given by Awadalla (1994, A&A 289, 137) and Binnendijk (1964, AJ 69, 157). System1898Orbit1End System1899Orbit1Begin - Recent photometric observations of SV Equ were reported by Cook (1997, AAVSO 26, 14) who gave the new time-of-minimum prediction with the period P = 0.88097307 days. These observations were obtained very close in time to our observations, but they disagree in the time of minimum T0. We do not see any obvious reasons why the O-C for contemporaneous observations should be as large as -0.028 days, but note that the graph of the data in Cook (1997) indicates rather large photometric errors. System1899Orbit1End System1900Orbit1Begin -The orbital period of 0.42 days is somewhat long for a typical W-type system, and the spectral type of F9 V is relatively early for a W-type system. The light curve has a moderately large amplitude of about 0.6 mag and the primary (deeper) eclipses appear to be total or very close to total, so that the system has the potential of an excellent combined light and radial velocity solution. System1900Orbit1End System1901Orbit1Begin - 'RV2a' marks the observations were secondary is given half-weight. -For guidance on the orbital phases, we used the recent determination of Agerer and Huebscher (1998, Inf. Bull. Variable Stars No. 4562). To phase our observations, we used the value of the period from the study by Binnendijk (1972, AJ 77, 246). System1901Orbit1End System1902Orbit1Begin - 'RV1a' and 'RV2a' marks the observations given half-weight. -- Niarchos et al. (1994, A&A 292, 494) made the plausible and apparently correct assumption that the system is of the A type and attempted to determine the mass ratio. Their value, q_ph = 0.726, is very far from our spectroscopic determination, q_sp = 0.348(29), once again demonstrating the dangers of spectroscopically unconstrained light-curve solutions for partially eclipsing systems. They attempted to estimate the spectral type and preferred the range A7 to F0, rather than the previous estimates of A5 to A7. The Tycho's experiment color (B-V)_T = 0.45 (7) indicates a mid-F spectral type. Our spectral type is A8-F0 V, so that there is a disagreement between the color and the spectral type. System1902Orbit1End System1903Orbit1Begin -The period used for phasing our observations was determined by Akalin & Derman (1997, A&AS 125, 407). System1903Orbit1End System1904Orbit1Begin - 'RV1a' marks the observations given half-weight. - The assumed period, as well as the recent timing of the eclipse, comes from the photometric study by Cereda et al. (1988, A&AS, 76, 256). Since the system was not recently observed, the accumulated uncertainty in the period, as well as a likely change in its length since the observations of Cereda et al. (1988), has led to a large difference between the spectroscopic and predicted values of T0 of 0.2208 days. We handled the implied problem of relating our radial velocity to the photometric data of Cereda et al. (1988) by assuming that the system is of the A type, as indicated by the fact that the secondary (shallower) eclipses are apparently total. System1904Orbit1End System1905Orbit1Begin - 'RV2a' marks the observations were secondary is given half-weight. - The radial velocity variations have been observed by us for the first time. System1905Orbit1End System1906Orbit1Begin - O-C is listed instead of errors - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -The light curve shows two equally deep minima, so that the choice of the contact binary type is somewhat arbitrary. We chose to use the original ESA (1997) ephemeris, which then leads to the A-type system (the more massive, hotter star eclipsed at minimum corresponding to our T0). Note, however, that T0 = 2,451,510.5416, determined by Keskin, Yasarsoy, & Sipahi (2000) from photometric observations obtained during the span of our spectroscopic observations, must then refer to the secondary minimum. These observations are in excellent agreement with our observations in terms of the initial epoch, if allowance of a half-period is made. System1906Orbit1End System1907Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. - Because of the relative faintness of EL Aqr and large zenith distance as seen from the David Dunlap Observatory (DDO), our radial velocity observations have relatively large scatter. The system is of the A type and has a small mass ratio, q = 0.203 +- 0.008. The ephemeris of Agerer & Hubscher (1999), based on photometric observations obtained during our observations (T0 = 2,451,080.4443), agrees very well with our determination of T0. System1907Orbit1End System1908Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -We have not been able to detect a third component in the broadening functions, which is surprising in view of the well-defined signatures of two different components in the classification spectrum. System1908Orbit1End System1909Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -DN Cam has not been observed photometrically since the discovery by Hipparcos. Our determination of T0 is fully consistent with the original ephemeris, T0 = 2,448,500.488. It should be noted that the HIP light curve shows practically equally deep eclipses, so that the matter of the type of the system (A or W) is uncertain and awaits detailed modeling. System1909Orbit1End System1910Orbit1Begin - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -Our independent estimates of the spectral type are not entirely consistent, A9 and F2, but agree with the spectral type estimated before (F2 in SIMBAD). -The original HIPPARCOS epoch, T0 = 2,448,500.427, agrees well with our determination of T0. Again, the eclipses are almost equally deep in this case. System1910Orbit1End System1911Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -V776 Cas is the brighter member of the visual binary ADS 1485. The companion, at a separation of 5".38, is 2 mag fainter than the contact binary. We avoided the companion in our radial velocity observations of V776 Cas but observed its velocity on two occasions with the following results: HJD = 2,451,769.800, Vr = -26.4 km s-1 and HJD = 2,451,806.715, Vr = -27.4 km s-1. System1911Orbit1End System1912Orbit1Begin - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. -The discovery of spectral signatures of the secondary component in SX Crv was not easy. In fact, without any new photometric data, we unnecessarily collected many observations during conjunctions, assigning our initial inability to detect the secondary to a possible problem with the initial epoch and/or to a variable period. Only later on did we realize that a weak signature of the secondary was detectable in our broadening functions, in spite of the large ratio of masses of 15:1. To calculate the orbital phases, we used the HIPPARCOS data on the period and the initial epoch (T0 = 2,448,500.1539). - The HIP light curve is rather poorly covered, so it is difficult to say if the secondary eclipse of SX Crv is total. It may be actually the case because for a small q total eclipses take place over a wide range of the inclinations; also, an amplitude as "large" as the observed 0.2 mag is not easy to obtain for such a small mass ratio without the inclination being sufficiently large to produce total eclipses. System1912Orbit1End System1913Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. - V351 Peg was discovered to be an eclipsing binary by the Hipparcos mission. It is listed in the HIPPARCOS catalog with the period equal to one-half of the actual one (0.5933 days), apparently due to the identical depths of the eclipses. We used a period 2 times longer than in the HIP catalog but kept the original initial epoch for consistency with these observations; then the system is of the W type. The system was subsequently photometrically observed by Gomez-Forrellad et al. (1999). Their published value, advanced to the actual time of the observations, is T0 = 2,450,722.3918. Our determination is fully consistent with this determination. System1913Orbit1End System1914Orbit1Begin - a = Data have been given half weight in the orbital solution. Note that "a" is associated with RV1 or RV2. - O-C is listed instead of errors -Observations leading to entirely unseparable broadening- and correlation-function peaks are left blank; these observations may be eventually used in more extensive modeling of broadening functions. System1914Orbit1End System1915Orbit1Begin - O-C is listed instead of errors -The velocity amplitudes are relatively small, which would be consistent with the small photometric amplitude (0.07 mag), both probably caused by a low orbital inclination. The small photometric amplitude could also result from a moderate distortion of its detached components. System1915Orbit1End System1916Orbit1Begin Observations using the Coude Auxiliary Telescope(CAT) equipped with the Coude Echelle Spectrometer of the European Southern Observatory. SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System1916Orbit1End System1482Orbit2Begin New observations are obtained with the Coude Auxiliary Telescope (CAT) at ESO. The RVs from Bonsack (1981) and Tokovinin (1997) are merged in a single orbital solution. The small eccentricity is significant. SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System1482Orbit2End System214Orbit2Begin New observations using the Coude Auxiliary Telescope (CAT) equipped with the Coude Echelle Spectrometer of the European Southern Observatory. The orbit is computed by merging the new data with those of Sahade (1950). SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System214Orbit2End System1917Orbit1Begin Observations using the Coude Auxiliary Telescope (CAT) equipped with the Coude Echelle Spectrometer (CES) of the European Southern Observatory and the 2.1m telescope of the Complejo Astronomico El Leoncito (CASLEO) by using a Boller & Chivens (B7C) Cassegrain spectrograph. -ESO(CAT)+CES configuration: sigma (standard deviation) =0.7 km/s, -CASLEO + B&C spectrograph: sigma =3.4 km/s. The orbital solution uses the RV by Abt (1970). The orbital period of 9.91d found by Morrell & Levato (1991) is shown here to be wrong. SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System1917Orbit1End System339Orbit2Begin Observations using the Coude Auxiliary Telescope (CAT) equipped with the Coude Echelle Spectrometer of the European Southern Observatory, the 2.1m telescope of the Complejo Astronomico El Leoncito (CASLEO) by using a Boller & Chivens Cassegrain spectrograph and the 0.9m telescope of the Catania Astrophysical Observatory, which is fibre linked to a REOSC echelle spectrograph. -ESO(CAT)+CES configuration: sigma (standard deviation) =0.7 km/s -CASLEO + B&C spectrograph: sigma =3.4 km/s -SLN + REOSC spectrograph: sigma=1.1 km/s The observations by Blaauw & van Albada (1963) are used in the orbital solution. The secondary is estimated to be 1mag fainter than the primary. SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System339Orbit2End System865Orbit2Begin -Observations using the Coude Auxiliary Telescope (CAT) equipped with the Coude Echelle Spectrometer of the European Southern Observatory and the 0.9m telescope of the Catania Astrophysical Observatory, which is fibre linked to a REOSC echelle spectrograph. -ESO(CAT)+CES configuration: sigma (standard deviation) =0.7 km/s -SLN + REOSC spectrograph: sigma=1.1 km/s The RV of van Hoof et al. (1963) are used in the orbital solution. SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System865Orbit2End System1191Orbit2Begin -Observations using the 0.9m telescope of the Catania Astrophysical Observatory, which is fibre linked to a REOSC echelle spectrograph. -SLN + REOSC spectrograph: sigma=1.1 The orbit is computed using also the RV from Batten et al. (1982) SB9: The T0 listed in the paper was wrong. The authors supplied us with a revised value. System1191Orbit2End System1918Orbit1Begin System1918Orbit1End System1919Orbit1Begin The preliminary result gave a single-lined binary (SB1) with a period of 5.97 days, but the residuals (+-2.92 km s-1) are too large for its rotational velocity. The residuals showed a variation with time, yielding an orbit with a period of 1487 +- 72 days. Raboud & Mermilliod 1998 suspect a period "around 2900 days," so we or they may be off by a factor of 2. Correcting for that motion the residuals for the short period are +-0.70 km s-1, which is consistent with those of other stars of the same rotational velocities. Thus, this seems to be a triple system. Negative speckle results and occultation results (Peterson & White 1984 and Peterson et al. 1989). System1919Orbit1End System1919Orbit2Begin The preliminary result gave a single-lined binary (SB1) with a period of 5.97 days, but the residuals (+-2.92 km s-1) are too large for its rotational velocity. The residuals showed a variation with time, yielding an orbit with a period of 1487 +- 72 days. Raboud & Mermilliod 1998 suspect a period "around 2900 days," so we or they may be off by a factor of 2. Correcting for that motion the residuals for the short period are +-0.70 km s-1, which is consistent with those of other stars of the same rotational velocities. Thus, this seems to be a triple system. Negative speckle results and occultation results (Peterson & White 1984 and Peterson et al. 1989). System1919Orbit2End System1920Orbit1Begin -This appears to be an double-lined binary (SB2) in which the lines are always partially blended. In refining the orbital elements we gave those near the gamma velocity lower weight. Negative speckle results. System1920Orbit1End System528Orbit2Begin Our orbital elements are similar to those of Sanford (1931). Negative speckle and occultation results. System528Orbit2End System1922Orbit1Begin Negative speckle and occultation results. System1922Orbit1End System1923Orbit1Begin Our spectra show a peculiar situation of possibly a sharp blended double-lined pair combined with a very broad-lined star. The first set of velocities in Table 2 refer to the broad lines; the next two sets refer to the sharp double lines. It has not been possible to derive orbital elements, except perhaps a rough period for the sharper pair of about 48 days. It is possible that the broad-lined star plus sharp pair represent the speckle binary seen by Mason et al. 1993 at 0".14-0".05 and in occultation measures by Peterson et al. 1989 at 0".115. This star is considered to be a Delta Scuti star by Tsevtkov 1993. System1923Orbit1End System1924Orbit1Begin Our spectra show a double-lined spectrum whose components are always blended by rotation, but at least they are clearly discernible most of the time. Noted as an double-lined binary (SB2) in the BSC. Negative speckle and occultation results. System1924Orbit1End System1925Orbit1Begin We find this to be an single-lined binary (SB1) with a period of 994 days and K = 9.8 km s-1. These confirm the elements derived by Mermilliod & Mayor (1989), who found a period of 998 days and K = 9.6 km s-1. These imply an angular separation of 0".023. Peterson & White found occultation evidence for a separation of 0".0181 and magnitude difference of 1.9 mag; they suggest a period of about 4 yr. It seems likely that both of these refer to the same pair. Negative speckle results. System1925Orbit1End System719Orbit2Begin We confirm the orbital elements by Vinter-Hansen (1940) and derive elements by combing her data with ours. We did not see the secondary lines within our spectral range. Herbig & Turner (1953) derived spectral types of G0 III-IV (primary) and A3 (secondary). System719Orbit2End System1926Orbit1Begin This appears to be a double-lined binary with components that are always blended by high rotational velocities. Only the primary elements are useful and, in particular, only the period seems accurate. System1926Orbit1End System726Orbit2Begin Our orbital elements agree well with those by Harper (1926). System726Orbit2End System727Orbit2Begin Our orbital elements agree with most of those found by Conti & Barker (1973) except we find e = 0.30 compared with their e = 0.36. System727Orbit2End System1927Orbit1Begin The spectrum appears to be a double-lined binary with components always blended by moderate rotation. Although combined orbital elements were derived, they are probably not very accurate. This star is listed as a Delta Scuti variable by Breger (1979). System1927Orbit1End System1205Orbit2Begin System1205Orbit2End System1482Orbit3Begin System1482Orbit3End System1928Orbit1Begin Usenko (1990 Kinem. Phys. Celest. Bodies, 6, No.3) suggested the presence of a B5 companion from the star's position in the two-color diagram. System1928Orbit1End System1928Orbit2Begin The radial velosities were published by the same authors in IBVS 4130 (1994). In this paper the authors calculate the new orbital elements using the same measured velocities. System1928Orbit2End System1929Orbit1Begin To calculate the orbital elements authors used measured (n=79) and published (n=56) radial velocities. They did not publish their velocities. System1929Orbit1End System1185Orbit2Begin To calculate the orbital elements authors used measured (n=83) and published (n=117) radial velocities. They did not publish their velocities. System1185Orbit2End System1720Orbit2Begin To calculate the orbital elements authors used measured (n=131) and published (n=49) radial velocities. They did not publish their velocities. System1720Orbit2End System1930Orbit1Begin To calculate the orbital elements authors used measured (n=58) and published (n=9) radial velocities. They did not publish their velocities. System1930Orbit1End System1107Orbit2Begin To calculate the orbital elements authors used measured (n=69) and published (n=93) radial velocities. They did not publish their velocities. System1107Orbit2End System988Orbit2Begin Authors calculated orbital elements using all available data. System988Orbit2End System1180Orbit2Begin Radial-velocity curve of A-component was constructed on the measured and published radial velocity data. System1180Orbit2End System1931Orbit1Begin The period was taken by authors from Stefl et al.(1990, Bull. Astron. Inst. Czechoslov. 41, 29) The epoch T0 given by the authors referred to the secondary, here corrected. System1931Orbit1End System340Orbit3Begin Two spectrograms have been taken with the 6-m telescope at the Special Astrophysical Observatory, and five ones with the 2.6 m telescope at the Crimean Astrophysical Observatory. The period P has been taken from Bondar' et al.(1997, Astron. Zh. 74, 701) The radial-velocity curve was constructed based on the measured and published radial velocities. System340Orbit3End System341Orbit2Begin Four spectrograms were taken at 6-m Special Astrophysical Observatory telescope, and five ones were taken at 2.6-m Crimean Astrophysical Observatory telescope (Crimea). The radial velocites were determined by two different methods from first four spectrograms. There is another set of radial velocities for the primary star. JD RV1 Err1 48578.498 90 11 48579.440 38 7 48581.560 -42 16 48582.561 -15 10 e, K1, K2, V0, rms1, rms2 were derived using data from all previous publications. P, T0 were taken from Bondar', N.I. and Vitrichenko, E.A., Astron. Lett., 1995, vol. 21, p.627 System341Orbit2End System1932Orbit1Begin Authors used P and T0 of Hill et. al (1976 AAp. 51, 1) Radial-velocity curve was constructed from 1924-1991 observations of different authors in joint solution with BVR light curves. Amplitude K1 is not given by the authors, derived from the given component masses. There is another set of radial velocities measured as mean velocity for the three Balmer lines. System1932Orbit1End System1933Orbit1Begin -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA:13/8/0 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 2.22/0.97/- -rms2 for the orbital solution from CORALIE, FOCES and CfA: 0.49/1.08/- -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1933Orbit1End System1934Orbit1Begin -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA: 12/8/12 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 0.30/2.10/1.39 -rms2 for the orbital solution from CORALIE, FOCES and CfA: 0.59/3.11/3.75 -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1934Orbit1End System1935Orbit1Begin -The orbital period is derived from the photometry (Covino et al. 2000,A&A, 361, L49). -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA:12/8/10 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 0.62/1.24/1.72 -rms2 for the orbital solution from CORALIE, FOCES and CfA: 1.08/5.87/7.58 -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1935Orbit1End System1936Orbit1Begin -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA:10/11/32 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 0.49/3.28/1.78 -rms2 for the orbital solution from CORALIE, FOCES and CfA: 0.43/1.39/1.57 -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1936Orbit1End System1937Orbit1Begin -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA:16/12/18 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 0.68/1.72/2.95 -rms2 for the orbital solution from CORALIE, FOCES and CfA: 0.65/1.99/2.38 -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1937Orbit1End System1938Orbit1Begin -Because of the variety of telescopes and instruments used to measure the radial velocities, some care is required in order to account for possible systematic differences between CORALIE (the two-fiber-fed high-resolution spectrograph on the 1.2 m Swiss Euler telescope, at La Silla, Chile), the FOCES (Fiber Optics Cassegrain Echelle Spectrograph at the 2.2 m telescope at the Calar Alto Observatory), and CfA (the high-resolution single-order echelle spectra at using the Multiple Mirror Telescope (MMT) in Arizona, the 1.5 m Tillinghast reflector at the Fred L. Whipple Observatory (FLWO), also in Arizona, and the 1.5 m Wyeth reflector at the Oak Ridge Observatory (ORO), in Massachusetts at the Harvard-Smithsonian Center for Astrophysics) observations, as well as differences in the internal precision. In particular, we have allowed for differences in the zero point of the velocity scale by including an offset for the FOCES and CfA velocities, and adopting the CORALIE system as the reference because of the higher intrinsic precision of those observations. These offsets were included as unknowns in the least-squares problem, and are solved for simultaneously with the other orbital elements. -Number of measurements used for the orbital solution from CORALIE, FOCES and CfA:15/8/26 -rms1 for the orbital solution from CORALIE, FOCES and CfA: 0.33/1.90/1.31 -rms2 for the orbital solution from CORALIE, FOCES and CfA: 1.76/2.83/7.83 -The relative weights of observations from the three telescopes were determined by re-normalizing the internal errors of each set of observations to the standard deviation of the corresponding residuals from a preliminary solution, while maintaining the relative weights of the individual velocities within each series. This procedure was iterated until convergence. As a test, separate solutions were derived for each telescope when allowed by the number of observations. No significant differences in the elements were seen other than trivial offsets in the V0 velocity. Therefore, for the final solutions we combined the observations as described above. In three cases the formal eccentricity turned out to be insignificant, and we therefore adopted circular orbits. Three of the systems are triple-lined, and the velocities measured for the third component are also plotted and are near the center-of-mass velocity of the binary in all cases. System1938Orbit1End System1939Orbit1Begin -Observations were made with the photoelectric scanner CORAVEL attached to the 1.5 m Danish Ritchey-Chretien telescope at the European Southern Observatory, Chile. System1939Orbit1End System1940Orbit1Begin -Observations were made with the photoelectric scanner CORAVEL attached to the 1.5 m Danish Ritchey-Chretien telescope at the European Southern Observatory, Chile. System1940Orbit1End System1941Orbit1Begin This star seems not to be a pre-main-sequence object, as other two SBs studied in this paper. The authors do not provide the individual radial velocities. System1941Orbit1End System1942Orbit1Begin -T0=epoch of inferior conjunction -The H-alpha emission that originates from the red dwarf is used to obtain the red dwarf radial velocities. The H-alpha emission centroid was measured using IRAF's SPLOT routines. The shift in H-alpha emission was converted into radial velocities, which were corrected for the Earth's motion. The radial velocity measurements of Kawka,Vennes,Dupuis & Koch, 2000,AJ,120,3250 and from this work were combined to calculate an improved orbital period of the binary system. System1942Orbit1End System1943Orbit1Begin -T0= epoch of inferior conjunction -K1= Red dwarf semiamplitude -(*) = Radial velocity measurements were measured from low-dispersion spectra. For the calculation of the period these velocities had a reduced weight (0.25) compared with the radial velocities obtained from high-dispersion spectra -High resolution spectra: using the Cassegrain spectrograph attached to the 74 inch (1.9 m) telescope at Mount Stromlo Observatory (MSO) using the 1200 line mm-1 grating blazed at 7500 Angstrom. We have used the 2K CCD camera binned 2 × 2. The spectra range from 6230 to 6830 Angstrom , with a dispersion of 0.50 Angstrom pixel-1. -Low resolution spectra:We have also obtained spectra using the 300 line mm-1 grating blazed at 5000 Angstrom. The spectral range of the spectra up to March 10 was 3335 to 6465 Angstrom with a dispersion of 2.846 Ansgtrom pixel-1, then the grating was tilted to produce spectra with the range of 3850 to 6970 Angstrom with a dispersion of 2.83 Angstrom pixel-1. System1943Orbit1End System1944Orbit1Begin -T0=epoch of inferior conjunction. -K1=Red dwarf semiamplitude -(*) = Radial velocity measurements were measured from low-dispersion spectra. For the calculation of the period these velocities had a reduced weight (0.25) compared with the radial velocities obtained from high-dispersion spectra -High resolution spectra: using the Cassegrain spectrograph attached to the 74 inch (1.9 m) telescope at Mount Stromlo Observatory (MSO) using the 1200 line mm-1 grating blazed at 7500 Angstrom. We have used the 2K CCD camera binned 2 × 2. The spectra range from 6230 to 6830 Angstrom , with a dispersion of 0.50 Angstrom pixel-1. -Low resolution spectra:We have also obtained spectra using the 300 line mm-1 grating blazed at 5000 Angstrom. The spectral range of the spectra up to March 10 was 3335 to 6465 Angstrom with a dispersion of 2.846 Ansgtrom pixel-1, then the grating was tilted to produce spectra with the range of 3850 to 6970 Angstrom with a dispersion of 2.83 Angstrom pixel-1. -We have measured the radial velocity of the white dwarf from the STIS spectra, where the extreme velocity difference is 309 +- 70 km s-1. The difference in phase of the measurements is 0.4 to 0.6 phases; therefore the measured velocity amplitude sets the minimum amplitude for the white dwarf. On the other hand, the predicted semiamplitude of the white dwarf calculated from the semiamplitude of the red-dwarf and the mass ratio is 165 +- 35 km s-1, which suggests that the Space Telescope Imaging Spectrograph (STIS) spectra were observed near quadrature where the maximum velocities occur, and q =< 0.79. System1944Orbit1End System1945Orbit1Begin -T0=epoch of inferior conjunction -A search for the best period using the EW measurements resulted in a period of P= 1.26243 +- 0.00008 with the epoch of minimum emission T0=2451461.906 +- 0.027(HJD). This period agrees with the period obtained from radial velocities within the uncertainties. System1945Orbit1End System1266Orbit2Begin The systemic velocity of the secondary is listed as -64.0+/-4.7 km/s System1266Orbit2End System1321Orbit2Begin The systemic velocity of the secondary is listed as -6.8+/-8.3 km/s System1321Orbit2End System12Orbit3Begin Radial velocities are derived from the IUE spectra by cross-correlation. System12Orbit3End System1401Orbit2Begin The systemic velocity of the secondary is listed as -17.9+/-2.8 km/s System1401Orbit2End System443Orbit3Begin Radial velocities are derived from the IUE spectra by cross-correlation. System443Orbit3End System422Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System422Orbit2End System106Orbit2Begin Radial velocities are derived from the IUE spectra by cross-correlation. System106Orbit2End System1946Orbit1Begin Radial velocities are derived from the IUE spectra by cross-correlation. System1946Orbit1End System1946Orbit2Begin System1946Orbit2End System342Orbit2Begin System342Orbit2End System352Orbit2Begin System352Orbit2End System1947Orbit1Begin System1947Orbit1End System1947Orbit2Begin System1947Orbit2End System1948Orbit1Begin System1948Orbit1End System1948Orbit2Begin System1948Orbit2End System635Orbit2Begin System635Orbit2End System635Orbit3Begin System635Orbit3End System636Orbit2Begin The two systemic velocities differ by 33.8 km/s. In the paper, V0 of the secondary is listed as -4.6+/-2.8 km/s. In order to present just one plot with the two curves, we substracted 33.8 km/s from all the radial veloci- ties of the secondary. System636Orbit2End System1949Orbit1Begin System1949Orbit1End System1949Orbit2Begin System1949Orbit2End System926Orbit2Begin System926Orbit2End System924Orbit2Begin System924Orbit2End System1950Orbit1Begin System1950Orbit1End System1206Orbit2Begin System1206Orbit2End System1206Orbit3Begin The systemic velocity of the secondary is listed as -12.3+/-15.0 km/s System1206Orbit3End System1272Orbit3Begin System1272Orbit3End System1951Orbit1Begin System1951Orbit1End System1952Orbit1Begin System1952Orbit1End System1203Orbit2Begin The systemic velocity of the secondary is listed as -14.1+/-2.7 km/s System1203Orbit2End System1222Orbit2Begin The systemic velocity of the secondary is listed as -0.1+/-5.9 km/s System1222Orbit2End System1399Orbit2Begin System1399Orbit2End System1953Orbit1Begin -Orbital elements were derived with the differential-correction program of Barker et al. (1967, ROB, No. 130 ), as modified and described by Fekel et al. (1999,A&AS, 137, 369). Our final elements for both binaries converged at an eccentricity so close to zero that a formal zero-eccentricity solution was adopted (see Lucy & Sweeney 1971,AJ, 76, 544). -The standard error of an observation of unit weight is 4.62 kms-1 using all available measurements of the primary and secondary component. Some of Balona's (1987,S. Afr. Astr. Obs. Circ., 11, 1) O-C residuals are 12 kms-1, and two of Balona's secondary O-C residuals are as large as 23 kms-1 -Spectra appear as composites, it is necessary to separate the two stellar spectra at all phases in order to extract activity features from each spectrum. This is done by generating an artificial composite spectrum from two non-active MK standard stars closely matching our object stars. The procedure includes rotational broadening, radial-velocity shifting, and intensity weighting of both standard-star spectra in the Fourier domain. The resulting difference spectrum is minimized by a least-squares approach. The input set of reference spectra then gives the overall best-fit combination. Finally, we subtract the 'synthetic' binary spectrum from each observed spectrum to eliminate the contribution from the underlying inactive part of the stellar photospheres and chromospheres. System1953Orbit1End System1954Orbit1Begin --Orbital elements were derived with the differential-correction program of Barker et al. (1967, ROB, No. 130 ), as modified and described by Fekel et al. (1999,A&AS, 137, 369). Our final elements for both binaries converged at an eccentricity so close to zero that a formal zero-eccentricity solution was adopted (see Lucy & Sweeney 1971,AJ, 76, 544). -The standard error for the primary was 0.41 kms-1, and was calculated using all 38 cross-correlation measurements. The secondary-star orbit was computed independently from the primary star by using the radial velocities of the residual H-alpha emission feature. H-alpha is the only line that is detected from the secondary star and the accuracy of the secondary measurements is comparably poor. Its standard error of an observation of unit weight is 8.6 kms-1. -Spectra appear as composites, it is necessary to separate the two stellar spectra at all phases in order to extract activity features from each spectrum. This is done by generating an artificial composite spectrum from two non-active MK standard stars closely matching our object stars. The procedure includes rotational broadening, radial-velocity shifting, and intensity weighting of both standard-star spectra in the Fourier domain. The resulting difference spectrum is minimized by a least-squares approach. The input set of reference spectra then gives the overall best-fit combination. Finally, we subtract the 'synthetic' binary spectrum from each observed spectrum to eliminate the contribution from the underlying inactive part of the stellar photospheres and chromospheres. System1954Orbit1End System1955Orbit1Begin - Data are the Observed Radial Velocities. - P and T0 from Zhai,Zhang,Zhang,1983, Inf. Bull. Variable Stars, No. 2275 - The orbit plot shows one deviant pair of points, presumably a typing error in Julian date or swap with other star in the original paper. System1955Orbit1End System1955Orbit2Begin - P and T0 from Zhai,Zhang,Zhang,1983, Inf. Bull. Variable Stars, No. 2275 - Data are the Orbital radial velocities: two small corrections are employed to obtain the "orbital" velocities from the observed values. First are the corrections derived from measures of the spectra of an extensive series of synthetic binaries, created from a sky spectrum observed with the same equipment, as discussed in (Popper & Jeong,1994,PASP,106,189). Second are the corrections arising from the effects of tidal distortion and mutual irradiation (Wilson,1990,ApJ,356,613) that reduce the center of light to the center of mass, yielding the orbital velocities. - The orbit plot shows one deviant pair of points, presumably a typing error in Julian date or swap with other star in the original paper. System1955Orbit2End System1956Orbit1Begin - Data are the Observed Radial Velocities. - P and T0 from D. H. Kaiser 1996, private communication - The orbit plot shows one deviant pair of points, presumably a typing error in Julian date or swap with other star in the original paper. System1956Orbit1End System1956Orbit2Begin - Data are the Orbital radial velocities: two small corrections are employed to obtain the "orbital" velocities from the observed values. First are the corrections derived from measures of the spectra of an extensive series of synthetic binaries, created from a sky spectrum observed with the same equipment, as discussed in (Popper & Jeong,1994,PASP,106,189). Second are the corrections arising from the effects of tidal distortion and mutual irradiation (Wilson,1990,ApJ,356,613) that reduce the center of light to the center of mass, yielding the orbital velocities. - P and T0 from D. H. Kaiser 1996, private communication - The orbit plot shows one deviant pair of points, presumably a typing error in Julian date or swap with other star in the original paper. System1956Orbit2End System1036Orbit2Begin -In an attempt to derive a precise ephemeris, the authors combined all of their better data and the 26 velocities from Hutchings, 1987, PASP, 312, 57 runs into a single time series. There are two sets of allowed periods, one near 0.1469 d and the other near 0.1474 d; these differ by 1/44 cycle per day. Because of their time sampling, the present data unfortunately do not discriminate between frequencies spaced by this amount. There is also some ambiguity in the choice of cycle count between the present velocities and Hutchings' observations 10 years earlier. System1036Orbit2End System1957Orbit1Begin -The orbital period determined here is similar to those of many other dwarf novae, and also similar to those of other old novae that have not become dwarf novae (Warner, 1995, Cataclysmic Variables.Cambridge Univ. Press, Cambridge; Ritter, Kolb, 1998, A&AS, 312, 83). System1957Orbit1End System1958Orbit1Begin -Velocities were measured using the derivative of a Gaussian as the convolution function, optimized for a 10 Angstrom FWHM line. The strongest periodicity in the 1997 July data was at 1.468 +- 0.016 d, with a daily cycle-count alias near 0.6 d. We found no convincing features at shorter periods, despite a sampling strategy designed to turn up the short periods more typical of cataclysmic variables. The Monte Carlo test indicates that the 1.47-d period is preferred over the 0.6-d period at the 98 per cent confidence level in the 1997 data. -We obtained the 1999 June spectra to confirm the unexpectedly long period. The new velocities showed periodicity at 1.489+- 0.017 d, consistent with the fit to the 1997 velocities, and the sinusoidal fit at 1.49 d was dramatically better than at 0.6 d. The 1999 velocities were significantly 'quieter' than the 1997 velocities, and gave well-determined fit parameters. This second detection independently confirmed the existence of a long periodicity, and the good fit removes any significant doubt concerning the choice of the longer period. The weighted average of the periods from the two runs is 1.478 +- 0.012 d. System1958Orbit1End System1959Orbit1Begin -Dwarf Nova star - To measure radial velocities we used a convolution function consisting of positive and negative Gaussians of FWHM 10 Angstrom separated by 36 Angstrom. This emphasized the steep sides of the line profiles and suppressed information from the line cores. -rms1 is the root mean square scatter around the best-fitting sinusoid. While the formal error bars on K1 are reasonably small, we caution against assuming that K1 is a good indicator of the motion of either star. System1959Orbit1End System1960Orbit1Begin - Dwarf Nova - The authors measured Halpha velocities by convolving with a double-Gaussian function, this time with a 34 Angstrom separation. Their 1997 September observations did not give a unique period, so they obtained more spectra in 1997 December and 1998 January. The periodogram shows much fine-scale ringing because of alternate choices of cycle count assigned to the relatively long intervals between observing runs, but one frequency does stand considerably higher than the others. The Monte Carlo procedure of Thorstensen & Freed, 1985, AJ, 90, 2082 confirms that this frequency may be selected with high confidence. System1960Orbit1End System1274Orbit2Begin -Dwarf Nova star - The authors tried several line-measuring algorithms on H-alpha, and the best behaved velocities came from measures of the peak of the line. The convolution function used was the derivative of a narrow (6 Angstrom) Gaussian. Measurements of the base of the line gave the same results for the period but at lower signal-to-noise ratio. The periodogram shows a strong signal at 5.93 cycles day-1 and no indication of a signal at the 0.073 day (13.7 cycles day-1 period found by Shafter (1985, AJ, 90, 643). A. W. Shafter (1998, private communication) kindly supplied his original velocity time series to us for reanalysis, and indeed a 0.073 day sinusoid fits his velocities very well; furthermore, there is no indication of any power at our period. However, there are only eight points, taken in two groups of four on a single night. Shafter's logs indicate that his velocity data may have been taken during a decline from outburst, which might have affected the velocities. Because our data are more extensive, we believe that our period determination supersedes Shafter's. We think that Shafter's result probably arose from a statistical accident in which eight points masqueraded as a good sinusoid. Statistical accidents occur more frequently in period searches than one might think because a single data set is fitted at a substantial number of trial frequencies, so a good fit at a selected frequency represents the best of a number of trials (Scargle, 1982, ApJ, 263, 835, discusses this issue). System1274Orbit2End System1961Orbit1Begin V0 should be increased by 1.8 km/s. Some observations were neglected in the orbital solution because of strong influence of the proximity effects and large deviations from circular model. The period has been adopted after Liu, Yang, & Tam (1987, IBVS no.3080) System1961Orbit1End System1962Orbit1Begin Some observations were neglected in the orbital solution because of strong influence of the proximity effects and large deviations from circular model. The period was adopted after Faulkner (1986, PASP 98, 690). V0 should be increased by 1.8 km/s. System1962Orbit1End System1963Orbit1Begin Some observations were neglected in the orbital solution because of strong influence of the proximity effects and large deviations from circular model. The period was taken from Derman, Demircan, & Selam (1991, AApS 90, 301) System1963Orbit1End System1964Orbit1Begin EF Dra is a triple system; the third component is probably a physical companion, since its radial velocity is -38 km/s. P was taken from Plewa et al.(1991, Acta Astron. 41, 291) System1964Orbit1End System1965Orbit1Begin The period was derived from photometric observations of Robb (1992, private comm.) and Agerer & Hubscher (1995, IBVS no.4222). System1965Orbit1End System1966Orbit1Begin Some observations were neglected in the orbital solution because of strong influence of the proximity effects and large deviations from circular model. The period was taken from Yang et al. (1991, Acta Astron. Sinica 32, 326). V0 should be increased by 1.8 km/s. System1966Orbit1End System1967Orbit1Begin Radial velocities were measured with the accuracy of 1 km/s. The period was taken from Zhang, Zhang, & Zhai (1992, Acta Astron. Sinica 33, 131). System1967Orbit1End System1968Orbit1Begin The period was taken from Markworth & Michaels (1982, PASP 94, 350). System1968Orbit1End System1969Orbit1Begin The period was taken from Leung, Zhai, & Zhang (1985, AJ 90, 515). V0 should be increased by 1.8 km/s. System1969Orbit1End System1970Orbit1Begin V0 should be increased by 1.8 km/s. The period was derived from photometric observations of O. Demircan (1997, private comm.) and Muyesseroglu, Gurol & Selam (1996, IBVS no.4380). System1970Orbit1End System1971Orbit1Begin Four velocities obtained when the components' lines were blended are listed but given 0.00 weight in the orbital solution. a1sini = 4900000 +/- 20000 km a2sini = 5990000 +/- 40000 km M1 (sin)3 i = 0.139 +/- 0.002 solar masses M2 (sin)3 i = 0.114 +/- 0.001 solar masses System1971Orbit1End System1972Orbit1Begin - Red giant binary in cluster IC 4651 - In order to distinguish between field and cluster stars and detect the spectroscopic binaries in the cluster, radial-velocity observations were made during the years 1989-1997 with the photoelectric scanner CORAVEL (Mayor 1985, in Stellar Radial Velocities, IAU Colloq. 88, ed. A. G. D. Philip, & D. W. Latham. L. Davis Press, Schenectady, 35) on the Danish 1.54-m telescope at ESO, La Silla. The observations are referred to the accurate velocity zero-point determined from a large number of observations of minor planets and standard stars by Udry et al. (1999, in Precise Stellar Radial Velocities, IAU Colloq. 170, ed. J. B. Hearnshaw, & C. D. Scarfe, ASP Conf. Ser., 185, 367). The observing list comprised all known red giants in and near the cluster, plus all candidate main-sequence and turnoff stars brighter than the limiting magnitude of CORAVEL (B ~ 15) from the then largest known photometric surveys of the cluster, by Eggen (1971 ApJ, 166, 87) and Anthony-Twarog et al. (1988,AJ, 95, 1453). System1972Orbit1End System1973Orbit1Begin - Orbital element omega corrected by the authors with respect to the published value which was in error. - Red giant binary in cluster IC 4651 -In order to distinguish between field and cluster stars and detect the spectroscopic binaries in the cluster, radial-velocity observations were made during the years 1989-1997 with the photoelectric scanner CORAVEL (Mayor 1985, in Stellar Radial Velocities, IAU Colloq. 88, ed. A. G. D. Philip, & D. W. Latham. L. Davis Press, Schenectady, 35) on the Danish 1.54-m telescope at ESO, La Silla. The observations are referred to the accurate velocity zero-point determined from a large number of observations of minor planets and standard stars by Udry et al. (1999, in Precise Stellar Radial Velocities, IAU Colloq. 170, ed. J. B. Hearnshaw, & C. D. Scarfe, ASP Conf. Ser., 185, 367). The observing list comprised all known red giants in and near the cluster, plus all candidate main-sequence and turnoff stars brighter than the limiting magnitude of CORAVEL (B ~ 15) from the then largest known photometric surveys of the cluster, by Eggen (1971 ApJ, 166, 87) and Anthony-Twarog et al. (1988,AJ, 95, 1453). System1973Orbit1End System1974Orbit1Begin - Red giant binary in cluster IC 4651 - In order to distinguish between field and cluster stars and detect the spectroscopic binaries in the cluster, radial-velocity observations were made during the years 1989-1997 with the photoelectric scanner CORAVEL (Mayor 1985, in Stellar Radial Velocities, IAU Colloq. 88, ed. A. G. D. Philip, & D. W. Latham. L. Davis Press, Schenectady, 35) on the Danish 1.54-m telescope at ESO, La Silla. The observations are referred to the accurate velocity zero-point determined from a large number of observations of minor planets and standard stars by Udry et al. (1999, in Precise Stellar Radial Velocities, IAU Colloq. 170, ed. J. B. Hearnshaw, & C. D. Scarfe, ASP Conf. Ser., 185, 367). The observing list comprised all known red giants in and near the cluster, plus all candidate main-sequence and turnoff stars brighter than the limiting magnitude of CORAVEL (B ~ 15) from the then largest known photometric surveys of the cluster, by Eggen (1971 ApJ, 166, 87) and Anthony-Twarog et al. (1988,AJ, 95, 1453). System1974Orbit1End System1975Orbit1Begin - System identification in the published Table 2 was wrong, corrected by the authors. - Red giant binary in cluster IC 4651 - In order to distinguish between field and cluster stars and detect the spectroscopic binaries in the cluster, radial-velocity observations were made during the years 1989-1997 with the photoelectric scanner CORAVEL (Mayor 1985, in Stellar Radial Velocities, IAU Colloq. 88, ed. A. G. D. Philip, & D. W. Latham. L. Davis Press, Schenectady, 35) on the Danish 1.54-m telescope at ESO, La Silla. The observations are referred to the accurate velocity zero-point determined from a large number of observations of minor planets and standard stars by Udry et al. (1999, in Precise Stellar Radial Velocities, IAU Colloq. 170, ed. J. B. Hearnshaw, & C. D. Scarfe, ASP Conf. Ser., 185, 367). The observing list comprised all known red giants in and near the cluster, plus all candidate main-sequence and turnoff stars brighter than the limiting magnitude of CORAVEL (B ~ 15) from the then largest known photometric surveys of the cluster, by Eggen (1971 ApJ, 166, 87) and Anthony-Twarog et al. (1988,AJ, 95, 1453). System1975Orbit1End System1976Orbit1Begin - System identification in the published Table 2 was wrong, corrected by the authors. - Red giant binary in cluster IC 4651 - In order to distinguish between field and cluster stars and detect the spectroscopic binaries in the cluster, radial-velocity observations were made during the years 1989-1997 with the photoelectric scanner CORAVEL (Mayor 1985, in Stellar Radial Velocities, IAU Colloq. 88, ed. A. G. D. Philip, & D. W. Latham. L. Davis Press, Schenectady, 35) on the Danish 1.54-m telescope at ESO, La Silla. The observations are referred to the accurate velocity zero-point determined from a large number of observations of minor planets and standard stars by Udry et al. (1999, in Precise Stellar Radial Velocities, IAU Colloq. 170, ed. J. B. Hearnshaw, & C. D. Scarfe, ASP Conf. Ser., 185, 367). The observing list comprised all known red giants in and near the cluster, plus all candidate main-sequence and turnoff stars brighter than the limiting magnitude of CORAVEL (B ~ 15) from the then largest known photometric surveys of the cluster, by Eggen (1971 ApJ, 166, 87) and Anthony-Twarog et al. (1988,AJ, 95, 1453). System1976Orbit1End System1919Orbit2Begin - The RV curve given by authors corresponds to omega about 160 deg., adjusted here but not given in the paper. - V0 changes due to the motion in wide orbit of this triple system, center-of-mass value is given here - Abt & Willmarth,1999, ApJ 521, 682 published the orbital elements for a triple stars system. However, early attempts to compute an orbit produced residuals larger (2.98 km s-1) than the measurement errors (0.52 km s-1) which could be explained by a change in the systemic velocity. Therefore, this star was continuously monitored, from the end of 1979 to 1997 to follow the variation of the systemic velocity. Only the Am primary is visible. All efforts to detect a correlation for any of the two other components were unsuccessful. - The spectroscopic orbit is solved by taking into account the two periods. Thus the radial velocities of the short period (P=5d.9701) are corrected by the motion of the center of masses to compute the short solution and these corrections are used to solve for the long period (P=2878d). If the short period solution agrees with Abt & Willmarth (1999), our value for the long period system is twice as large as their value. An attempt to plot our observations in phase with their period failed. Therefore the correct value is P=2878d. System1919Orbit2End System1977Orbit1Begin -Abt & Willmarth,1999, ApJ 521, 682 published the orbital elements for this triple system. However, early attempts to compute an orbit produced residuals larger (2.98 km s-1) than the measurement errors (0.52 km s-1) which could be explained by a change in the systemic velocity. Therefore, this star was continuously monitored, from the end of 1979 to 1997 to follow the variation of the systemic velocity. Only the Am primary is visible. All efforts to detect a correlation for any of the two other components were unsuccessful. -The spectroscopic orbit is solved by taking into account the two periods. Thus the radial velocities of the short period (P=5d.9701) are corrected by the motion of the center of masses to compute the short solution and these corrections are used to solve for the long period (P=2878d). If the short period solution agrees with Abt & Willmarth (1999), our value for the long period system is twice as large as their value. An attempt to plot our observations in phase with their period failed. Therefore the correct value is P=2878d. System1977Orbit1End System528Orbit3Begin - The present orbital solution is in very good agreement with that found by Sanford, 1931, ApJ, 74, 201, although we obtained an eccentricity somewhat larger than Sanford's value (e=0.2), but in good agreement with Abt & Willmarth, 1999, ApJ, 521, 682 value (e=0.3). System528Orbit3End System1922Orbit2Begin - The epoch T0 given by authors has large error and is offset with respect to the RV curve; it adjusted here to fit. - This star is also considered as the third component of the visual quadruple system ADS 6921. - Two additional radial velocities were taken during the survey for magnetic fields of Ap stars with the spectrograph Elodie (Babel et al. 1995, 1997) and were taken into account in the final solution. System1922Orbit2End System1978Orbit1Begin - The data were collected from 1979 to 1996, independently by J.-C. Mermilliod (JCM) and by J.-M. Carquillat (JMC), which explains the large number of observations obtained for this star. - The amplitude of the radial-velocity variation is still quite comfortable for CORAVEL, but may require good precision measurements to detect it with classical spectrographs and a long-term observing program. System1978Orbit1End System237Orbit2Begin - Our orbital parameters are in good agreement with Abt, 1961, ApJS 6, 37 elements. System237Orbit2End System241Orbit2Begin - The epoch T0 given by authors has large error and is offset with respect to the RV curve; it is adjusted here to fit. -The observations agrees well with Abt,1985, ApJS 59, 229 System241Orbit2End System1979Orbit1Begin - Some RV points are not present on the published RV curve. - The mean errors on the radial velocities reflect the limit inherent to CORAVEL for measuring Am stars and the effect of rotation. System1979Orbit1End System299Orbit2Begin - The epoch T0 given by authors is offset with respect to the RV curve; it is adjusted here to fit. - CORAVEL observations began in 1979 and ended in 1993 with a 10-year gap between 1983 and 1993, without observation. The eccentricity is not well constrained by our observations and the differences observed between our elements and Conti, 1969, ApJ 156, 661 elements are probably not significant. System299Orbit2End System1980Orbit1Begin - The epoch T0 given by authors is offset with respect to the RV curve; it is adjusted here to fit. - The system shows a radial-velocity dispersion which is larger than the standard radial-velocity error and P(Chi^2)= 0.000. A Fourier analysis gives a possible period of 32.528d. No long-term variation is obviously seen in a simple plot of the radial-velocity in function of time (from 1979 to 1999). The orbital solution is fitted with the value of the Fourier period. The orbital parameters represent a possible solution, but due to the small amplitude of the orbit, and to the radial-velocity errors, the orbital solution is not absolutely certain. - During some observing runs an observation of vB 132 (the secondary of the triple system) was obtained. vB 132 does not show any radial-velocity variation either on short or long time scales. The separation between vB 131 (the primary) and vB 132 leads us to predict a long period system and a small radial-velocity variation, which CORAVEL is not able to measure. System1980Orbit1End System372Orbit2Begin - V0 changes due to the motion in the outer orbit of this multiple system. The center-of-mass value is given here. - It is a visual hierarchical quadruple system. The components are noted Aa, Ab and Ba, Bb. A is SB1 with a period of 4.45 days and B is SB2 with a period of 4.48 days. The visual orbit has a period of 18.2 years. - Due to the large eccentricity of the visual system, the highest precision is needed and we used only the latest data given on the web site of the CHARA (Center for High Angular Resolution Astronomy) interferometric catalogue (Hartkopf et al. 1999, Third Catalog of Interferometric Measurements of Binary Stars, CHARA Contribution No. 4). System372Orbit2End System374Orbit2Begin - It is a visual hierarchical quadruple system. The components are noted Aa, Ab and Ba, Bb. A is SB1 with a period of 4.45 days and B is SB2 with a period of 4.48 days. The visual orbit has a period of 18.2 years. - Due to the large eccentricity of the visual system, the highest precision is needed and we used only the latest data given on the web site of the CHARA (Center for High Angular Resolution Astronomy) interferometric catalogue (Hartkopf et al. 1999,Third Catalog of Interferometric Measurements of Binary Stars, CHARA Contribution No. 4). System374Orbit2End System1981Orbit1Begin System1981Orbit1End System1982Orbit1Begin System1982Orbit1End System1983Orbit1Begin -The eccentricity has been fixed to 0.00, consistent with its short period (Mermilliod & Mayor 1992 in Binaries as Tracers of Stellar Formation, ed. A. Duquennoy, & M. Mayor (Cambridge: Cambridge University Press), 183; 1996,in Cool Stars, Stellar Systems and the Sun, ed. R. Pallavicini, & A. K. Dupree, ASPC, 109, 373) System1983Orbit1End System310Orbit2Begin - The system has a faint physical tertiary at about 10" separation. - The ephemeris for CD Tau, for both radial-velocity and light-curve solutions, was adopted as Min I (HJD)=244 1619.4075+3.435 137 E (Kholopov 1987, GCVS, 4th edn. Nauka, Moscow). We used the SBOP program (created by Dr P. B. Etzel in 1978 and later revised several times) and adopted the Lehmann-Filhes method (Lehmann-Filhes, 1894, Astron. Nachr., 163, 17; Underhill 1966, The Early Type Stars.Reidel,Dordrecht, p.127) for simultaneous solution of a double-lined radial-velocity curve. Inclination 87.7 deg., component masses 1.442 and 1.368 M_sun. - The errors of the parameters were conservatively adopted as twice the standard errors provided by the SBOP program. Our results show good agreement with the analysis of the previously published radial-velocity curve of Popper, 1971, ApJ, 166, 361, although the curve coverage and the individual accuracy of the measurements are significantly better in our study, leading to smaller formal errors. System310Orbit2End System1984Orbit1Begin - BD +00 1617C is part of a poorly studied trapezium system (BD+00 1617) at the heart of a dim and very young open cluster (Bochum 2). The three O stars appear equally spaced and on a straight line in the projection onto the sky. - Radial velocities have been first measured on the calibrated spectra by fitting individually each absorption line (with reference wavelengths taken from Moore 1959). This soon led to the recognition of star BD +00 1617A as a constant radial velocity star and the other two program stars as binaries. Using BD +00 1617A as a Radial Velocity standard star we have proceeded to re-evaluate radial velocities of BD +00 1617C by cross-correlation (with the IRAF task fxcor ). - The errors of the orbital solutions are of the order of 5% or less. The larger errors for the eccentricities may result from the uneven distribution of the observations along the orbital phase. System1984Orbit1End System1985Orbit1Begin - BD +00 1617B is part of a poorly studied trapezium system (BD+00 1617) at the heart of a dim and very young open cluster (Bochum 2). The three O stars appear equally spaced and on a straight line in the projection onto the sky. - Radial velocities have been first measured on the calibrated spectra by fitting individually each absorption line (with reference wavelengths taken from Moore 1959). This soon led to the recognition of star BD +00 1617A as a constant radial velocity star and the other two program stars as binaries. Using BD +00 1617A as a Radial Velocity standard star we have proceeded to re-evaluate radial velocities of BD +00 1617B by cross-correlation (with the IRAF task fxcor ). - The errors of the orbital solutions are of the order of 5% or less. The larger errors for the eccentricities may result from the uneven distribution of the observations along the orbital phase. System1985Orbit1End System217Orbit2Begin System217Orbit2End System1322Orbit2Begin a1sini = 4560000 +/- 10000 a2sini = 6270000 +/- 44000 M1 (sin)3 i = 0.1692 +/- 0.0024 solar masses M2 (sin)3 i = 0.1231 +/- 0.0011 solar masses System1322Orbit2End System488Orbit2Begin HPO = Haute-Provence Observatory KPNO = Kitt Peak National Observatory Fick = Fick Observatory The two components are on opposite sides of the Hertzsprung Gap. The slightly more massive G star is more evolved but fainter than the less massive and less evolved F star. a1 sin i = 9064000 +/- 14000 km a2 sin i = 9014000 +/- 19000 km m1 (sin)3 i = 0.9605 +/- 0.0041 solar masses m2 (sin)3 i = 0.9657 =/- 0.0034 solar masses System488Orbit2End System1986Orbit1Begin This star is one of several fainter visual companions to HD 165590 = V772 Her. a1 sin i = 12610000 +/- 80000 km a2 sin i = 13260000 +/- 130000 km m1 (sin)3 i = 0.534 +/- 0.009 solar masses m2 (sin)3 i = 0.507 +/- 0.008 solar masses System1986Orbit1End System1987Orbit1Begin There is a clear indication of a continuous period decrease. P was taken from Samec et al. (1998, IBVS no.4616) System1987Orbit1End System1988Orbit1Begin The period was taken from Schrimer (1992, IBVS no.3785) System1988Orbit1End System1989Orbit1Begin The period was taken from Evans et al. (1985, PASP 97, 648) System1989Orbit1End System1990Orbit1Begin System1990Orbit1End System1991Orbit1Begin System1991Orbit1End System1053Orbit2Begin System1053Orbit2End System1992Orbit1Begin In Comment "D" means data obtained by H. Duerbek at the 1.52 m ESO telescope. The period was taken from General Catalogue of Variable Stars. System1992Orbit1End System1993Orbit1Begin The period and T0 were taken from Niarchos, Hoffman, and Duerbeck (1994, AAp 103, 39). System1993Orbit1End System1994Orbit1Begin System1994Orbit1End System1995Orbit1Begin System1995Orbit1End System1996Orbit1Begin a1sini = 23780000 +/- 270000 km a2sini = 29080000 +/- 650000 km m1 (sin)3 i = 1.583 +/- 0.056 solar masses m2 (sin)3 i = 1.295 +/- 0.037 solar masses System1996Orbit1End System1997Orbit1Begin a1sini = 18880000 +/- 80000 km a2sini = 20500000 +/- 100000 km m1 (sin)3 i = 0.645 +/- 0.007 solar masses m2 (sin)3 i = 0.594 +/- 0.005 solar masses System1997Orbit1End System76Orbit2Begin The primary component, Polaris, is a Cepheid variable pulsating with a period of 3.97 days. The amplitude of the pulsation, however, had been diminishing until the mid-1990es, since then the pulsation of Polaris has had extremely low photometric and radial velocity amplitudes. The spectral type of the secondary is F0V. This spectroscopic binary and a faint visual companion form a system ADS 1477. System76Orbit2End System76Orbit3Begin The primary component, Polaris, is a Cepheid variable pulsating with a period of 3.97 days. The amplitude of the pulsation, however, had been diminishing until the mid-1990es, since then the pulsation of Polaris has had extremely low photometric and radial velocity amplitudes. The spectral type of the secondary is F0V. This spectroscopic binary and a faint visual companion form a system ADS 1477. System76Orbit3End System1107Orbit3Begin System1107Orbit3End System617Orbit2Begin The primary component, Y Car, is a doubly periodic Cepheid variable. The pulsation period of the fundamental mode is 3.64 days, while the period of the simultaneously excited first overtone is 2.56 days. The spectral type of the secondary component is B9.0V, and it is a binary star itself. System617Orbit2End System24Orbit2Begin System24Orbit2End System24Orbit3Begin The primary component, DL Cas, is a Cepheid variable pulsating with a period of 8.001 days. The spectral type of the secondary is B9V. The system is a member in the Galactic cluster NGC 129. System24Orbit3End System1998Orbit1Begin The primary component, AX Cir, is a Cepheid variable pulsating with a period of 5.273 days. The spectral type of the secondary is B6.0V. A faint visual companion was also detected by the Hipparcos. System1998Orbit1End System1172Orbit2Begin Hierarchical triple system. The primary component, SU Cyg, is a Cepheid variable pulsating with a period of 3.846 days. The secondary is a binary star, the spectral type of its brighter component is B8.0V. SB9: The original correction of 7.99 km/s subtracted to V0 has been discarded. System1172Orbit2End System1999Orbit1Begin The primary component, TX Del, is a Cepheid variable pulsating with a period of 6.166 days. System1999Orbit1End System1721Orbit2Begin The primary component, Z Lac, is a Cepheid variable pulsating with a period of 10.886 days. Based on ultraviolet spectra, the spectral type of the secondary cannot be earlier than A5V. System1721Orbit2End System2000Orbit1Begin System2000Orbit1End System2000Orbit2Begin The primary component, T Mon, is a Cepheid variable pulsating with a period of 27.025 days. The spectral type of the secondary is B9.8V. The system is a possible member in the association Mon OB2. System2000Orbit2End System709Orbit2Begin The primary component, S Mus, is a Cepheid variable pulsating with a period of 9.660 days. The spectral type of the secondary is B3.5V. System709Orbit2End System273Orbit2Begin The primary component, AW Per, is a Cepheid variable pulsating with a period of 6.464 days. The spectral type of the secondary is B8.2V. System273Orbit2End System273Orbit3Begin The primary component, AW Per, is a Cepheid variable pulsating with a period of 6.464 days. The spectral type of the secondary is B8.2V. System273Orbit3End System273Orbit4Begin The primary component, AW Per, is a Cepheid variable pulsating with a period of 6.464 days. The spectral type of the secondary is B8.2V. System273Orbit4End System1185Orbit3Begin System1185Orbit3End System1185Orbit4Begin The primary component, S Sge, is a Cepheid variable pulsating with a period of 8.382 days. The companion itself is a binary. System1185Orbit4End System2001Orbit1Begin The primary component, W Sgr, is a Cepheid variable pulsating with a period of 7.595 days. The spectral type of the secondary is A0V. Together with a visual companion, they form the multiple system ADS 11029. System2001Orbit1End System2001Orbit2Begin The primary component, W Sgr, is a Cepheid variable pulsating with a period of 7.595 days. The spectral type of the secondary is A0V. Together with a visual companion, they form the multiple system ADS 11029. System2001Orbit2End System1929Orbit2Begin The primary component, V350 Sgr, is a Cepheid variable pulsating with a period of 5.154 days. The spectral type of the secondary is B9.0V. System1929Orbit2End System960Orbit2Begin System960Orbit2End System960Orbit3Begin System960Orbit3End System2002Orbit1Begin Fick = Fick Observatory KPNO = Kitt Peak National Observatory The secondary is a white dwarf. a1sini = 41600000 +/- 1200000 km f(m) = 0.00351 +/- 0.00031 solar masses System2002Orbit1End System2003Orbit1Begin SAA0 = South African Astronomical Observatory KPNO = Kitt Peak National Observatory The primary is a mild Barium star and the secondary is a white dwarf. a1sini = 276000000 +/- 102000000 km f(m) = 0.03 +/- 0.03 solar masses System2003Orbit1End System2004Orbit1Begin SAA0 = South African Astronomical Observatory McDonald = McDonald Observatory Fick = Fick Observatory KPNO = Kitt Peak National Observatory IUE = International Ultraviolet Explorer satellite The secondary is a subdwarf B star. a1sini = 3552000 +/- 38000 km a2sini = 26500000 +/- 680000 km m1 (sin)3 i = 2.24 +/- 0.12 solar masses m2 (sin)3 i = 0.300 +/- 0.014 solar masses System2004Orbit1End System2005Orbit1Begin The primary is a chromospherically active binary. The period and time of maximum velocity were adopted from photometric determinations. In agreement with the photometric solution, The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. a1sini = 18300000 +/- 80000 km a2sini = 19140000 +/- 80000 km m1 (sin)3 i = 1.413 +/- 0.015 solar masses m2 (sin)3 i = 1.352 +/- 0.015 solar masses System2005Orbit1End System2006Orbit1Begin - Orbital elements: e, w, P assumed from Beavers & Eitter, 1988, BAAS, 20, 737 - The centroid of the Halpha absorption core was measured. The secondary is a white dwarf. System2006Orbit1End System305Orbit2Begin -- A visual quadruple system; the component A is a delta Scuti type and SB1; the component C is classified as F3 V and is paired with a hot white dwarf companion. The companion to component A is unknown. Hogkin et al. (1993, MNRAS, 263, 229) assign a spectral type range F2-6 IV-V for the C component, in agreement with our stimate of F2 V. System305Orbit2End System1484Orbit2Begin - A visual quadruple system; the component A is a delta Scuti type and SB1; the component C is classified as F3 V and is paired with a hot white dwarf companion which is not the spectroscopic secondary of the C system. - Data of Tokovinin (1997, A&AS 121 71) are merged to get the combined orbital solution System1484Orbit2End System1307Orbit2Begin - Our own velocity measurements coupled with Harper's (1927, Publ. Dom. Astrophys. Obs. Victoria, 4, 161) data (18 velocities) result in an accurate period of 21.72168 +- 0.00009 days, considerably refining the period based on contemporary data alone. However, we only utilize recent measurements to determine the velocity amplitude and the mass function. The secondary star has been found to be a high-mass white dwarf (Landsman et al. 1993, PASP, 105, 841 and Wonnacott et al. 1993, MNRAS, 262, 277). System1307Orbit2End System2007Orbit1Begin - Orbital elements are derived from the velocities corrected for systematic effects derived from synthetic binary spectra (Popper & Jeong 1994,1994, PASP, 106, 189) and for the small effects of mutual irradiation, derived from the formalism developed by Wilson (1990, ApJ, 356, 613). - The period is found by Wolf & Sarounova, (1996,Inf. Bull. Variable Stars, No. 4292) - V0(primary)=19.0 +-0.3, V0(secondary)= 16.0 +-0.9 - one typo corrected in the table 1: JD 2450265.9301 instead of 2450256.6301 System2007Orbit1End System2008Orbit1Begin - Orbital elements are derived from the velocities corrected for systematic effects derived from synthetic binary spectra (Popper & Jeong 1994,1994, PASP, 106, 189) and for the small effects of mutual irradiation, derived from the formalism developed by Wilson (1990, ApJ, 356, 613). - V0(primary)= -20.1 +-0.3, V0(secondary)=-20.0 +-0.2 System2008Orbit1End System2009Orbit1Begin - Orbital elements are derived from the velocities corrected for systematic effects derived from synthetic binary spectra (Popper & Jeong 1994,1994, PASP, 106, 189) and for the small effects of mutual irradiation, derived from the formalism developed by Wilson (1990, ApJ, 356, 613). - V0(primary)=20.3 +-0.6, V0(secondary)=19.7 +-0.5 - Period is mis-typed in the original paper System2009Orbit1End System2010Orbit1Begin - Orbital elements are derived from the velocities corrected for systematic effects derived from synthetic binary spectra (Popper & Jeong 1994,1994, PASP, 106, 189) and for the small effects of mutual irradiation, derived from the formalism developed by Wilson (1990, ApJ, 356, 613). - V0(primary)=-3.2 +-0.4, V0(secondary)= -1.7 +-0.3 - Period and epoch corrected from the values adopted by the author to match the orbit. System2010Orbit1End System2011Orbit1Begin - RV measured on emission line - The orbital parameters corresponds to the circular solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=638+-11, V0(93 Jan.)=670+-12,V0(93 Nov.)=617+-12. Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2011Orbit1End System2011Orbit2Begin - Em: RV measured on emission line, A: RV on absorbtion line - The orbital parameters corresponds to the elliptical solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocitiesV0: V0(84 Dec.)=638+-08, V0(93 Jan.)=666+-09,V0(93 Nov.)=614+-09. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2011Orbit2End System2012Orbit1Begin -RV measured from emission line. -The orbital parameters corresponds to the circular solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=453+-11 , V0(93 Jan.)=532+- 08 ,V0(93 Nov.)=474+-12 . Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2012Orbit1End System2012Orbit2Begin -RV measured from emission line. - The orbital parameters corresponds to the elliptical solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=451+- 16, V0(93 Jan.)=532+-07, V0(93 Nov.)=474+-12. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2012Orbit2End System2013Orbit1Begin - RV measured from emission-line. - The orbital parameters corresponds to the circular solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=442 +- 13, V0(93 Jan.)=468 +- 09, V0(93 Nov.)=430 +-09. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2013Orbit1End System2013Orbit2Begin - RV measured from emission-line. - The orbital parameters corresponds to the elliptical solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=451 +- 26, V0(93 Jan.)=455 +- 03, V0(93 Nov.)=435 +- 10. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2013Orbit2End System2014Orbit1Begin - RV measured from emission-line. - The orbital parameters corresponds to the circular solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=66 +- 10, V0(93 Jan.)=50 +- 12,V0(93 Nov.)=74+- 12. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2014Orbit1End System2014Orbit2Begin - RV measured from emission-line. - The orbital parameters corresponds to the elliptical solution. - Since the data were collected during three different runs with different instruments, three corresponding systemic velocities V0: V0(84 Dec.)=66 +- 10, V0(93 Jan.)=50 +- 13,V0(93 Nov.)=74 +- 13. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2014Orbit2End System476Orbit2Begin - Solution for C IV 5808 angstroms (emission) for circular orbits for the Galactic WR binary. - Period from Niemela, Massey & Conti (1984), since they based it on more observations and over several epochs. They give no error and it is assumed here to be 0.001. The period found with the data described in the present study is 15.6+-3.2d based on only one epoch. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System476Orbit2End System2015Orbit1Begin - Solution for C IV 5808 angstroms (emission) for circular orbits for the Galactic binary. Different standard errors (rms) were so determined for each run: Epoch rms 1984 December 33.4 1993 January 26.1 1993 November 47.2 System2015Orbit1End System803Orbit2Begin Slowly pulsating B-star. Known visual binary with late-type companion. System803Orbit2End System860Orbit2Begin Slowly pulsating B-star. System860Orbit2End System2016Orbit1Begin Slowly pulsating B-star. System2016Orbit1End System2017Orbit1Begin Slowly pulsating B-star. - Aerts et al. (1999, A&A 343, 872) already found a longer than expected period of 8.8d with a rather large amplitude of about 8 km/s in their radial velocity data. This period was not found in their extensive set of photometric data. Therefore, these variations can not be due to a large-amplitude, low-degree pulsation. Now, we are able to assign these spectroscopic variations to a short, eccentric orbital motion, with orbital parametersobtained here. Since this is the binary with the smallest orbital amplitude, the phase plot for the orbital period seems rather noisy in comparison with the other binaries in our sample. This effect is strengthened by the multiperiodic character of this star. System2017Orbit1End System2018Orbit1Begin - The line profiles show a lot of asymmetries due to pulsation and the large, global Doppler shifts point out that we are dealing with a spectroscopic binary - After removing the orbit, the first photometric pulsation frequency nu_1 = 0.84060 c/d also dominates the radial velocity variations. It accounts for 60% up to 80% of the (remaining) variance in the three data sets. System2018Orbit1End System2019Orbit1Begin - We find a standard deviation of 40 km/s for the radial velocity, which is far too large to be explained by pulsation only. Preliminary solutions for the orbital elements resulted in a slightly eccentric orbit with e=0.031, but after applying the Lucy & Sweeney test (1971,ApJ 76, 544 ), we conclude that we are dealing with circular orbit with a very short period. The dominant period in the Hipparcos photometry and the Geneva photometry is half the orbital period. - We show the photometric measurements folded with the orbital period as found in these measurements. The signal is close to sinusoidal. This kind of variation in our photometric data is typical for ellipsoidal variable stars. They are due to the non-spherical shape of the components in a non-eclipsing binary and to the contribution of reflection effects. - After prewhitening with the orbit, nu_1=0.2148 c/d is found as first frequency of pulsation in the radial velocities. In the phase diagrams the original Geneva V and Hipparcos H_p measurements are folded with this period. Also the Scargle periodogram of the original photometric data is shown there. It is easily seen that both the "orbital" signal and the "pulsational" signal are prominently present. Indeed, in the Hipparcos photometry, the "orbital" peak is slightly higher than the "pulsational" peak, while in the Geneva photometry it is vice versa. In both cases, both peaks are well above the p_0=0.01 level. We conclude that HD 92287 is an ellipsoidal variable star with a pulsating component. Since the observed orbital period is of the same order of magnitude as the period of pulsation, this object is extremely interesting in order to search for possible resonances between pulsational behaviour and orbital motion. System2019Orbit1End System2020Orbit1Begin - According to the SIMBAD astronomical database, this star is an eclipsing binary of the beta Lyrae type, although we find equal depths for the primary and secondary minima, which is more typical for eclipsing binaries of the W Ursae Majoris type. We find that HD 69144 is an ellipsoidal variable star. - The visual companion at 35" is optical. System2020Orbit1End System2021Orbit1Begin - The components should be very close to each other, so the tidal effects are certainly important. Indeed, we again find evidence for a deformation of the stellar surface, since the photometric measurements are clearly dominated by (twice) the orbital frequency. System2021Orbit1End System826Orbit2Begin This is a spectroscopically triple system in wich the contact binary is the fainter component of a relatively close visual double. There are 31 additional observations leading to entirely unseparable broadening and correlation function peaks. System826Orbit2End System2022Orbit1Begin There are 17 additional observations leading to entirely unseparable broadening and correlation function peaks. The period is twice the value given in the Hipparcos catalog in which the time of maximum light is given as the initial epoch. System2022Orbit1End System2023Orbit1Begin There are 17 additional observations leading to entirely unseparable broadening and correlation function peaks. The radial velocity amplitudes depend on the spectral type of the template star used to derive the BFs. System2023Orbit1End System2024Orbit1Begin This is a spectroscopically triple system in which the contact binary having solved orbit is the fainter component. The bright companion is itself a possible independent spectroscopic binary. There are 13 additional observations of contact bimary leading to entirely unseparable broadening and correlation function peaks. System2024Orbit1End System2025Orbit1Begin There are 13 additional observations leading to entirely unseparable broadening and correlation function peaks. System2025Orbit1End System2026Orbit1Begin This is a spectroscopically triple system in wich the contact binary having a solved orbit is the brigter component. There are 23 additional observations leading to entirely unseparable broadening and correlation function peaks. System2026Orbit1End System494Orbit2Begin This is a spectroscopically triple system in wich the contact binary having a solved orbit is the brigter component. Observations were obtained in two groups (16 and 55 observations) separated by one year. The authors obtained the second solution based only on the 55 observations of the second season: V0=+31.11 (err=1.26); K1=116.09 (err=1.52); K2=222.87 (err=3.60); T0=51400.1752 (err=0.0022). There are 11 additional observations leading to entirely unseparable broadening and correlation function peaks. System494Orbit2End System2027Orbit1Begin There are 9 additional observations leading to entirely unseparable broadening and correlation function peaks. System2027Orbit1End System2028Orbit1Begin There are 18 additional observations leading to entirely unseparable broadening and correlation function peaks. The observations were made in the region centered at 5184 A and in the region centered at 5303 A. The results of independent solutions were identical, so the authors made a combined solution for both spectral regions. System2028Orbit1End System2029Orbit1Begin This is a spectroscopically triple system in which the contact binary is the fainter component of a very close visual binary. The brighter component is SB1 star which has a preliminary solved orbit. There are 21 additional observations leading to entirely unseparable broadening and correlation function peaks. System2029Orbit1End System2030Orbit1Begin The system is a spectroscopic triple, with the third component having relative brightness of L3/(L1+L2)=0.26. The average radial velocities of the third component measured in two sets of observations are 48.38 (0.30) km/s and 43.90 (0.43) km/s. There are 25 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2030Orbit1End System35Orbit2Begin There are 11 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. The period was taken from Nelson (2001, IBVS no.5040) System35Orbit2End System2031Orbit1Begin There are 6 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2031Orbit1End System2032Orbit1Begin There are 14 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2032Orbit1End System2033Orbit1Begin There are 30 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. The period is twice as long as in the Hipparcos Catalogue. System2033Orbit1End System2034Orbit1Begin There are 16 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2034Orbit1End System2035Orbit1Begin There are 16 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2035Orbit1End System2036Orbit1Begin There are 16 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2036Orbit1End System2037Orbit1Begin There are 18 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. The period was taken from Lasala-Garcia (2001, IBVS no.5075) System2037Orbit1End System2038Orbit1Begin There are 28 additional observations leading to entirely unseparable broadening and correlation function peaks; these observations may be eventually used in more extensive modeling of broadening functions. System2038Orbit1End System2039Orbit1Begin The primary is a chromospherically active binary. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT time of periastron passage but is T_0 = time of maximum positive velocity. a1sini = 8680000 +/- 30000 km m1 (sin)3 i = 0.0584 +/- 0.0009 solar masses System2039Orbit1End System1945Orbit2Begin Pre-cataclismic binary composed of DA white dwarf primary and red dwarf dMe secondary. The WD RVs were measured at HST Goddard spectrograph (UV lines are shown in the comments), while the RD RVs are from the previous paper by Vennes & Thorstensen (1999, AJ, 112, 284), with some additional data that are not reported in the present paper. The M-dwarf amplitude corrected for the fact that H-alpha originates at the UV-irradiated hemisphere and does not reflect center-of-mass motion is K2_corrected= 109.6 +- 5.6. The center-of-mass velocity listed is for the DA component and includes gravitational redshift of 20-30 km/s, for dMe component it is 29.0 +- 2.4 km/s. System1945Orbit2End System2040Orbit1Begin Pre-cataclismic binary composed of DA white dwarf primary and red dwarf dMe secondary. The WD RVs were measured at HST Goddard spectrograph (UV lines are shown in the comments), while the RD RVs are from the Hamilton spectrograph at Lick. Velocities at H-alpha are used for orbit calculation, velocities at HeI 5875 line are given in the notes. The M-dwarf amplitude corrected for the fact that H-alpha originates at the UV-irradiated hemisphere and does not reflect center-of-mass motion is K2_corrected= 140.9 +- 2.9. The center-of-mass velocity listed is for the DA component and includes gravitational redshift of 20-30 km/s, for dMe component it is 22.9 +- 0.9 km/s. The RV of the visual companion at 3.2 arcseconds is +23.2 on JD 2449770.89945, the large common proper motion confirms its physical relation to the spectroscopic pair. System2040Orbit1End System2041Orbit1Begin Pre-cataclismic binary composed of DA white dwarf primary and red dwarf dMe secondary. The WD RVs were measured at HST Goddard spectrograph (UV lines are shown in the comments), while the RD RVs are from the Hamilton spectrograph at Lick. Velocities at H-alpha are used for orbit calculation, velocities at HeI 5875 line are given in the notes. The M-dwarf amplitude corrected for the fact that H-alpha originates at the UV-irradiated hemisphere and does not reflect center-of-mass motion is K2_corrected= 88.5 +- 1.6. The center-of-mass velocity listed is for the DA component and includes gravitational redshift of 20-30 km/s, for dMe component it is -29.5 +- 0.7 km/s. System2041Orbit1End System2042Orbit1Begin Combined solution of spectroscopic and photometric orbits. Masses are fitted directly, so K1 and K2 are re-calculated from the final data. Observations not used in the solution are omitted. The spectroscopic observations have been obtained with the Echelle+CCD spectrograph on the 1.82 m telescope operated by Osservatorio Astronomico di Padova atop Mt. Ekar (Asiago). System2042Orbit1End System2043Orbit1Begin Combined solution of spectroscopic and photometric orbits. Masses are fitted directly, so K1 and K2 are re-calculated from the final data. Observations not used in the solution are omitted. The spectroscopic observations have been obtained with the Echelle+CCD spectrograph on the 1.82 m telescope operated by Osservatorio Astronomico di Padova atop Mt. Ekar (Asiago). System2043Orbit1End System2044Orbit1Begin Combined solution of spectroscopic and photometric orbits. Masses are fitted directly, so K1 and K2 are re-calculated from the final data. Observations not used in the solution are omitted. The spectroscopic observations have been obtained with the Echelle+CCD spectrograph on the 1.82 m telescope operated by Osservatorio Astronomico di Padova atop Mt. Ekar (Asiago). System2044Orbit1End System2045Orbit1Begin Cataclismic variable. Orbital parameters obtained for absortion-line component. The H-alpha emission (RVs are given in the comments) varies in anti-phase with amplitude of K=58 +- 3 km/s. Because this is an interacting binary, neither velocity curve may faithfully reflect the motion of the underlying star. Individual RVs are not given in the article, provided by the author. System2045Orbit1End System2046Orbit1Begin Cataclismic variable. The orbital elements are derived for H-alpha emission lines. Because this is an interacting binary, the velocity curve may not reflect the motion of the underlying star. Individual RVs are not given in the article, provided by the author. System2046Orbit1End System2047Orbit1Begin Cataclismic variable. The orbital elements are derived for H-alpha emission lines. Because this is an interacting binary, the velocity curve may not reflect the motion of the underlying star. Individual RVs are not given in the article, provided by the author. System2047Orbit1End System2048Orbit1Begin Cataclismic variable. The orbital elements are derived for H-alpha emission lines. Because this is an interacting binary, the velocity curve may not reflect the motion of the underlying star. Individual RVs are not given in the article, provided by the author. System2048Orbit1End System2049Orbit1Begin Close binary with both degenerate companions. We define T_0 such that star 1 has the deeper H alpha core and is closest to the observer at time T_0. The projected orbital speed of star 1 is K_1 and its apparent mean velocity is V0_1 and similarly for star 2. Note that V0_1 is different from V0_2 because the apparent mean velocity is the sum of the radial velocity of the system and the gravitational redshift of each star, and this second quantity is different for each star (V0_1= 22.3 +- 0.6, V0_1=15.0 +- 1.2, average is given in the catalog). Orbital elements were computed by simultaneous fitting directly the observed spectra around H-alpha line, hence no individual radial velocities were derived. System2049Orbit1End System2050Orbit1Begin Close binary with both degenerate companions. We define T_0 such that star 1 has the deeper H alpha core and is closest to the observer at time T_0. The projected orbital speed of star 1 is K_1 and its apparent mean velocity is V0_1 and similarly for star 2. Note that V0_1 is different from V0_2 because the apparent mean velocity is the sum of the radial velocity of the system and the gravitational redshift of each star, and this second quantity is different for each star (V0_1=-18.4 +- 0.8 , V0_1=-7.4 +- 3.6, average is given in the catalog). Orbital elements were computed by simultaneous fitting directly the observed spectra around H-alpha line, hence no individual radial velocities were derived. System2050Orbit1End System2051Orbit1Begin Close binary with both degenerate companions. We define T_0 such that star 1 has the deeper H alpha core and is closest to the observer at time T_0. The projected orbital speed of star 1 is K_1 and its apparent mean velocity is V0_1 and similarly for star 2. Note that V0_1 is different from V0_2 because the apparent mean velocity is the sum of the radial velocity of the system and the gravitational redshift of each star, and this second quantity is different for each star (V0_1=33.2 1.3 , V0_1=38.7 1.6, average is given in the catalog). Orbital elements were computed by simultaneous fitting directly the observed spectra around H-alpha line, hence no individual radial velocities were derived. System2051Orbit1End System216Orbit2Begin The early-type eclipsing binary SZ Cam (HD 25638; SAO 13030; HR 1260; BD+ 61 676N; ADS 2984 B) is the northern component of a visual double star consisting of two components with nearly equal brightness and spectral type, which are the brightest members of the galactic cluster NGC 1502. The close spatial coincidence of two very similar stars repeatedly led to confusion with the proper identification of the visual companions (e.g., SZ Cam was erroneously designated as ADS 2984 A in the Bright Star Catalogue, and was also misidentified as HD 25639 in the BSC Supplement, while in all other sources it is cross-referenced with HD 25638). The eclipsing binary SZ Cam has a third component, detected by light-time effect and resolved by speckle interferometry. This tertiary is itself a close binary with 2.8-day period. To obtain consistent radial velocity curves for both components, the arithmetic mean of V0_1(5.7 kms^-1) and V0_2(-11.5 kms^-1) was used as systemic velocity of the eclipsing pair. System216Orbit2End System2052Orbit1Begin The eclipsing binary SZ Cam has a third component, detected by light-time effect and resolved by speckle interferometry. This tertiary is itself a close binary with 2.8-day period, its orbit is given here. System2052Orbit1End System2053Orbit1Begin The spectroscopic system is a primary component of the visual binary ADS 12040 with orbital period around 687 years. The radial verlocity of the visual secondary B is -48.2 km/s and is apparently constant. System2053Orbit1End System2054Orbit1Begin The spectroscopic pair is a secondary component in the Hyades visual binary ADS 3248 with 40-year period. The RV of the primary is around +44 km/s. Both center-of-mass velocity of the spectroscopic system and of A are slowly changing due to the motion in the visual orbit, likely semi-amplitudes are 6.7 and 7 km/s, respectively. Small corrections are made to account for this in the computation of the orbit of Bab. System2054Orbit1End System2055Orbit1Begin The short-period spectroscopic system is a secondary component in the visual binary ADS 363 with 54-year period. The RV difference between visual components suggests semi-amplitudes around 7 km/s for each. System2055Orbit1End System2056Orbit1Begin The spectroscopic system belongs to a visual binary with 4" separation and uncertain long-period orbit. The visual secondary has constant radial velocity. System2056Orbit1End System2057Orbit1Begin The spectroscopic system is a primary component in a 97-year visual binary ADS 12656. In some orbital phases thenunresolved blended lines of visual components were measured (marked as "Aa+B"), these data are included in the orbital solution with low weight. The velocity of the secondary is constant at -58.6 +- 0.4 km/s. System2057Orbit1End System2058Orbit1Begin The spectroscopic system is a secondary component in a 144-year visual binary ADS 10683. The RV of the primary is constant, -53.78 +- 0.16 km/s. Only measurements at phases where the lines of A and Ba are separated are used in the orbital solution. System2058Orbit1End System2059Orbit1Begin This 258-year visual binary shows lines of only one component in its spectrum. Those lines likely belong to the primary and show 50-day RV variation. System2059Orbit1End System2060Orbit1Begin M1 (sin i)**3 = 2.502 +/- 0.026 Msun M2 (sin i)**3 = 0.5143 +/- 0.0085 Msun q = M2/M1 = 0.2055 +/- 0.0025 a1 sin i = 5.117 +/- 0.059 x 10**6 km a2 sin i = 24.897 +/- 0.088 x 10**6 km a sin i = 43.12 +/- 0.15 Rsun System2060Orbit1End System463Orbit2Begin YY Gem is Castor C. Period and epoch of primary minimum fixed from linear ephemeris based on times of eclipse: P = 0.814282212 +/- 0.000000012 days Min I = 2,449,345.112327 +/- 0.000087 (HJD) Derived quantities: M1 (sin i)**3 = 0.5938 +/- 0.0046 Msun M2 (sin i)**3 = 0.5971 +/- 0.0046 Msun q = M2/M1 = 1.0056 +/- 0.0050 a1 sin i = 1.3569 +/- 0.0047 x 10**6 km a2 sin i = 1.3493 +/- 0.0047 x 10**6 km a sin i = 3.8882 +/- 0.0095 Rsun Time span of observations (days) = 456.9 System463Orbit2End System2061Orbit1Begin The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. The primary is a gamma Doradus variable. In addition to its orbital motion, this star also shows a radial velocity variation due to pulsation, which has a period of 1.3071 days and an amplitude of about 3 km/s. This radial velocity period is nearly identical to one of three photometric periods, 1.30702 days, determined for this star. The listed radial velocities include the pulsational variation. The secondary is likely to be an M dwarf. asini = 382000 +/- 19000 km f(m) = 0.000111 +/- 0.000016 solar masses System2061Orbit1End System2062Orbit1Begin The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. The primary is a chromospherically active star. asini = 729000 +/- 16000 km f(m) = 0.0041 +/- 0.0003 solar masses System2062Orbit1End System2063Orbit1Begin Time span of observations = 1325 days M1 (sin i)**3 = 0.185 +/- 0.016 solar masses M2 (sin i)**3 = 0.1574 +/- 0.0079 solar masses q = 0.853 +/- 0.037 a sin i = 2.602 +/- 0.061 solar radii Light ratio L2/L1 = 0.19 Rotational velocities: v1 sin i = 41 km/s v2 sin i = 35: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2063Orbit1End System2064Orbit1Begin Time span of observations = 1096 days M2 sin i = 0.178 +/- 0.029 (M1+M2)**(2/3) solar masses a1 sin i = 0.406 +/- 0.066 x 10**6 km Rotational velocity v sin i = 56 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2064Orbit1End System2065Orbit1Begin Time span of observations = 766 days M1 (sin i)**3 = 0.741 +/- 0.027 solar masses M2 (sin i)**3 = 0.596 +/- 0.012 solar masses q = 0.804 +/- 0.014 a sin i = 16.49 +/- 0.16 solar radii Light ratio L2/L1 = 0.09 Rotational velocities: v1 sin i = 7: km/s v2 sin i = 5: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2065Orbit1End System2066Orbit1Begin Time span of observations = 708 days M1 (sin i)**3 = 0.9683 +/- 0.0074 solar masses M2 (sin i)**3 = 0.942 +/- 0.011 solar masses q = 0.9728 +/- 0.0061 a sin i = 16.824 +/- 0.053 solar radii Light ratio L2/L1 = 2.14 Rotational velocities: v1 sin i = 26 km/s v2 sin i = 16 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2066Orbit1End System2067Orbit1Begin Time span of observations = 1326 days M1 (sin i)**3 = 1.062 +/- 0.029 solar masses M2 (sin i)**3 = 0.578 +/- 0.012 solar masses q = 0.5442 +/- 0.0077 a sin i = 20.04 +/- 0.16 solar radii Light ratio L2/L1 = 0.06 Rotational velocities: v1 sin i = 32 km/s v2 sin i = 4: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2067Orbit1End System2068Orbit1Begin Time span of observations = 2213 days M1 (sin i)**3 = 0.718 +/- 0.016 solar masses M2 (sin i)**3 = 0.679 +/- 0.011 solar masses q = 0.945 +/- 0.011 a sin i = 7.642 +/- 0.046 solar radii Light ratio L2/L1 = 0.36 Rotational velocities: v1 sin i = 18 km/s v2 sin i = 16 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2068Orbit1End System2069Orbit1Begin Time span of observations = 1388 days M2 sin i = 0.351 +/- 0.018 (M1+M2)**(2/3) solar masses a1 sin i = 1.032 +/- 0.052 x 10**6 km Rotational velocity v sin i = 54 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2069Orbit1End System2070Orbit1Begin Time span of observations = 1325 days M1 (sin i)**3 = 0.612 +/- 0.022 solar masses M2 (sin i)**3 = 0.603 +/- 0.016 solar masses q = 0.986 +/- 0.020 a sin i = 17.97 +/- 0.18 solar radii Light ratio L2/L1 = 0.71 Rotational velocities: v1 sin i = 27 km/s v2 sin i = 24 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2070Orbit1End System2071Orbit1Begin Time span of observations = 1419 days M1 (sin i)**3 = 0.235 +/- 0.022 solar masses M2 (sin i)**3 = 0.1357 +/- 0.0078 solar masses q = 0.577 +/- 0.024 a sin i = 15.66 +/- 0.42 solar radii Light ratio L2/L1 = 0.19 Rotational velocities: v1 sin i = 0: km/s v2 sin i = 0: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2071Orbit1End System2072Orbit1Begin Time span of observations = 1009 days M1 (sin i)**3 = 0.5864 +/- 0.0064 solar masses M2 (sin i)**3 = 0.5681 +/- 0.0072 solar masses q = 0.9687 +/- 0.0072 a sin i = 10.560 +/- 0.039 solar radii Light ratio L2/L1 = 0.68 Rotational velocities: v1 sin i = 8 km/s v2 sin i = 8: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2072Orbit1End System2073Orbit1Begin Time span of observations = 703 days M1 (sin i)**3 = 0.3220 +/- 0.0024 solar masses M2 (sin i)**3 = 0.3066 +/- 0.0019 solar masses q = 0.9523 +/- 0.0041 a sin i = 11.231 +/- 0.025 solar radii Light ratio L2/L1 = 0.55 Rotational velocities: v1 sin i = 9 km/s v2 sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2073Orbit1End System2074Orbit1Begin Time span of observations = 2194 days M1 (sin i)**3 = 0.422 +/- 0.032 solar masses M2 (sin i)**3 = 0.230 +/- 0.014 solar masses q = 0.544 +/- 0.022 a sin i = 2.158 +/- 0.048 solar radii Light ratio L2/L1 = 0.24 Rotational velocities: v1 sin i = 118 km/s v2 sin i = 95: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2074Orbit1End System2075Orbit1Begin Time span of observations = 884 days M1 (sin i)**3 = 0.3698 +/- 0.0090 solar masses M2 (sin i)**3 = 0.3438 +/- 0.0070 solar masses q = 0.930 +/- 0.013 a sin i = 4.623 +/- 0.033 solar radii Light ratio L2/L1 = 0.63 Rotational velocities: v1 sin i = 40 km/s v2 sin i = 28 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2075Orbit1End System2076Orbit1Begin Time span of observations = 1388 days M1 (sin i)**3 = 0.02259 +/- 0.00086 solar masses M2 (sin i)**3 = 0.01990 +/- 0.00073 solar masses q = 0.881 +/- 0.021 a sin i = 4.358 +/- 0.052 solar radii Light ratio L2/L1 = 0.60 Rotational velocities: v1 sin i = 18 km/s v2 sin i = 3: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2076Orbit1End System2077Orbit1Begin Time span of observations = 1217 days M2 sin i = 0.156 +/- 0.044 (M1+M2)**(2/3) solar masses a1 sin i = 0.309 +/- 0.086 x 10**6 km Rotational velocity v sin i = 54 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2077Orbit1End System2078Orbit1Begin Time span of observations = 1133 days M1 (sin i)**3 = 0.1110 +/- 0.0023 solar masses M2 (sin i)**3 = 0.1062 +/- 0.0038 solar masses q = 0.957 +/- 0.018 a sin i = 7.134 +/- 0.066 solar radii Light ratio L2/L1 = 4.0 Rotational velocities: v1 sin i = 20 km/s v2 sin i = 9 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2078Orbit1End System2079Orbit1Begin Time span of observations = 1454 days M1 (sin i)**3 = 0.544 +/- 0.011 solar masses M2 (sin i)**3 = 0.499 +/- 0.019 solar masses q = 0.916 +/- 0.019 a sin i = 9.184 +/- 0.089 solar radii Light ratio L2/L1 = 1.22 Rotational velocities: v1 sin i = 49 km/s v2 sin i = 19 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2079Orbit1End System2080Orbit1Begin Time span of observations = 1477 days M1 (sin i)**3 = 0.914 +/- 0.066 solar masses M2 (sin i)**3 = 0.622 +/- 0.027 solar masses q = 0.680 +/- 0.023 a sin i = 13.57 +/- 0.27 solar radii Light ratio L2/L1 = 0.10 Rotational velocities: v1 sin i = 33 km/s v2 sin i = 0: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2080Orbit1End System2081Orbit1Begin Erroneous time of periastron passage in original publication is corrected here. Time span of observations = 1144 days M2 sin i = 0.2440 +/- 0.0034 (M1+M2)**(2/3) solar masses a1 sin i = 2.901 +/- 0.041 x 10**6 km Rotational velocity v sin i = 14 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2081Orbit1End System2082Orbit1Begin Time span of observations = 1214 days M2 sin i = 0.2543 +/- 0.0085 (M1+M2)**(2/3) solar masses a1 sin i = 1.243 +/- 0.041 x 10**6 km Rotational velocity v sin i = 34 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2082Orbit1End System2083Orbit1Begin Time span of observations = 1507 days M1 (sin i)**3 = 0.5310 +/- 0.0082 solar masses M2 (sin i)**3 = 0.4233 +/- 0.0076 solar masses q = 0.7972 +/- 0.0084 a sin i = 24.32 +/- 0.13 solar radii Light ratio L2/L1 = 1.11 Rotational velocities: v1 sin i = 16 km/s v2 sin i = 7: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2083Orbit1End System2084Orbit1Begin Time span of observations = 1215 days M2 sin i = 0.3348 +/- 0.0036 (M1+M2)**(2/3) solar masses a1 sin i = 1.751 +/- 0.019 x 10**6 km Rotational velocity v sin i = 30 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2084Orbit1End System2085Orbit1Begin Time span of observations = 1172 days M2 sin i = 0.2248 +/- 0.0014 (M1+M2)**(2/3) solar masses a1 sin i = 4.189 +/- 0.025 x 10**6 km Rotational velocity v sin i = 2: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2085Orbit1End System2086Orbit1Begin Time span of observations = 1504 days M1 (sin i)**3 = 0.947 +/- 0.028 solar masses M2 (sin i)**3 = 0.893 +/- 0.047 solar masses q = 0.943 +/- 0.025 a sin i = 15.80 +/- 0.21 solar radii Light ratio L2/L1 = 4.1 Rotational velocities: v1 sin i = 37 km/s v2 sin i = 14 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2086Orbit1End System2087Orbit1Begin Time span of observations = 1411 days M1 (sin i)**3 = 0.9307 +/- 0.0062 solar masses M2 (sin i)**3 = 0.9116 +/- 0.0069 solar masses q = 0.9795 +/- 0.0044 a sin i = 13.506 +/- 0.031 solar radii Light ratio L2/L1 = 0.67 Rotational velocities: v1 sin i = 24 km/s v2 sin i = 17 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2087Orbit1End System2088Orbit1Begin Time span of observations = 1181 days M1 (sin i)**3 = 1.134 +/- 0.069 solar masses M2 (sin i)**3 = 1.068 +/- 0.043 solar masses q = 0.942 +/- 0.029 a sin i = 109.6 +/- 1.8 solar radii Light ratio L2/L1 = 0.24 Rotational velocities: v1 sin i = 8 km/s v2 sin i = 0: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2088Orbit1End System2089Orbit1Begin Time span of observations = 1916 days M2 sin i = 0.2641 +/- 0.0075 (M1+M2)**(2/3) solar masses a1 sin i = 55.2 +/- 1.6 x 10**6 km Rotational velocity v sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2089Orbit1End System2090Orbit1Begin Time span of observations = 887 days M2 sin i = 0.1984 +/- 0.0034 (M1+M2)**(2/3) solar masses a1 sin i = 6.90 +/- 0.12 x 10**6 km Rotational velocity v sin i = 1: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2090Orbit1End System2091Orbit1Begin Time span of observations = 764 days M1 (sin i)**3 = 0.756 +/- 0.039 solar masses M2 (sin i)**3 = 0.568 +/- 0.017 solar masses q = 0.751 +/- 0.018 a sin i = 8.62 +/- 0.12 solar radii Light ratio L2/L1 = 0.07 Rotational velocities: v1 sin i = 18 km/s v2 sin i = 0: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2091Orbit1End System2092Orbit1Begin Time span of observations = 2151 days M1 (sin i)**3 = 1.090 +/- 0.038 solar masses M2 (sin i)**3 = 0.712 +/- 0.017 solar masses q = 0.653 +/- 0.012 a sin i = 21.75 +/- 0.22 solar radii Light ratio L2/L1 = 0.16 Rotational velocities: v1 sin i = 24 km/s v2 sin i = 5: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2092Orbit1End System2093Orbit1Begin Time span of observations = 1118 days M2 sin i = 0.2250 +/- 0.0013 (M1+M2)**(2/3) solar masses a1 sin i = 5.916 +/- 0.034 x 10**6 km Rotational velocity v sin i = 1: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2093Orbit1End System2094Orbit1Begin Time span of observations = 1895 days M2 sin i = 0.332 +/- 0.015 (M1+M2)**(2/3) solar masses a1 sin i = 62.1 +/- 2.7 x 10**6 km Rotational velocity v sin i = 12 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2094Orbit1End System2095Orbit1Begin Time span of observations = 1404 days M2 sin i = 0.240 +/- 0.077 (M1+M2)**(2/3) solar masses a1 sin i = 0.55 +/- 0.18 x 10**6 km Rotational velocity v sin i = 120 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2095Orbit1End System2096Orbit1Begin Time span of observations = 2301 days M1 (sin i)**3 = 0.597 +/- 0.050 solar masses M2 (sin i)**3 = 0.445 +/- 0.030 solar masses q = 0.746 +/- 0.023 a sin i = 6.76 +/- 0.17 solar radii Light ratio L2/L1 = 0.13 Rotational velocities: v1 sin i = 20 km/s v2 sin i = 15: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2096Orbit1End System2097Orbit1Begin Time span of observations = 1181 days M2 sin i = 0.545 +/- 0.054 (M1+M2)**(2/3) solar masses a1 sin i = 1.26 +/- 0.12 x 10**6 km Rotational velocity v sin i = 81 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2097Orbit1End System2098Orbit1Begin Time span of observations = 2300 days M1 (sin i)**3 = 0.01861 +/- 0.00173 solar masses M2 (sin i)**3 = 0.00891 +/- 0.00086 solar masses q = 0.479 +/- 0.026 a sin i = 2.238 +/- 0.068 solar radii Light ratio L2/L1 = 0.07 Rotational velocities: v1 sin i = 29 km/s v2 sin i = 0: km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2098Orbit1End System2099Orbit1Begin Time span of observations = 1890 days M2 sin i = 0.423 +/- 0.029 (M1+M2)**(2/3) solar masses a1 sin i = 19.6 +/- 1.4 x 10**6 km Rotational velocity v sin i = 10 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2099Orbit1End System2100Orbit1Begin Time span of observations = 1399 days M2 sin i = 0.187 +/- 0.020 (M1+M2)**(2/3) solar masses a1 sin i = 0.709 +/- 0.076 x 10**6 km Rotational velocity v sin i = 39 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2100Orbit1End System2101Orbit1Begin Time span of observations = 1775 days M1 (sin i)**3 = 0.0845 +/- 0.0052 solar masses M2 (sin i)**3 = 0.0707 +/- 0.0027 solar masses q = 0.837 +/- 0.027 a sin i = 1.510 +/- 0.025 solar radii Light ratio L2/L1 = 0.22 Rotational velocities: v1 sin i = 51 km/s v2 sin i = 38 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2101Orbit1End System2102Orbit1Begin Time span of observations = 1125 days M1 (sin i)**3 = 0.2749 +/- 0.0082 solar masses M2 (sin i)**3 = 0.2610 +/- 0.0058 solar masses q = 0.949 +/- 0.015 a sin i = 13.29 +/- 0.11 solar radii Light ratio L2/L1 = 0.34 Rotational velocities: v1 sin i = 10 km/s v2 sin i = 9 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2102Orbit1End System2103Orbit1Begin Time span of observations = 2362 days M2 sin i = 0.368 +/- 0.065 (M1+M2)**(2/3) solar masses a1 sin i = 65. +/- 11. x 10**6 km Rotational velocity v sin i = 18 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2103Orbit1End System2104Orbit1Begin Time span of observations = 2097 days M2 sin i = 0.194 +/- 0.034 (M1+M2)**(2/3) solar masses a1 sin i = 0.74 +/- 0.13 x 10**6 km Rotational velocity v sin i = 62 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2104Orbit1End System5Orbit2Begin -Ascending node epoch: 2443031.537 -The mean internal error is ~ 2 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -In our analysis we have used 3 observations of Shajn (1951, Izv. Krymsk, Astrofiz. Obs. 7, 337.), 6 of Palmer et al. (1968, Roy. Obs. Bull. 135), 38 of Hube & Gulliver (1985, JRAS Can 79, 49)and the 10 values from out data. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System5Orbit2End System195Orbit2Begin -Ascending node epoch: 2437642.337 -The mean internal error is ~ 2 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Morbey & Brosterhus (1974, PASP, 86,455) have computed an orbital solution based on 40 published observations. We used the same published data set plus the 25 new observation from our data. Morbey & Brosterhus elements agree within the errors with our final orbital solution. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System195Orbit2End System237Orbit3Begin -Ascending node epoch: 2441227.411 -The mean internal error is ~ 2 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Our analysis is based on 3 observations of Plaskett et al. (1919, JRAS Can, 40, 325), 6 from Stilwell (1949, Publ. Dominion Obs. 7, 337), 13 of Abt (1961, ApJS, 6, 37), 5 of Abt (1970, ApJS, 19, 387) and 5 from our data. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System237Orbit3End System241Orbit3Begin -Ascending node epoch: 2441271.259 -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Our solution is based on 12 observations of Jantzen (1913, Astron. Nachr., 196, 117), 5 of Harper (1935, Publ. Dominion Obs., 6, 217), 8 of Abt (1961, ApJS, 6, 37), 20 of Abt & Levy (1985, ApJS, 59, 229), and the 10 Asiago observations listed in our radial velocity table. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System241Orbit3End System710Orbit2Begin -Ascending node epoch: 2436763.340 -The mean internal error is ~ 2 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Although few in number, our 3 Asiago observations are useful to check the orbital period. They have been obtained during a single night, 4630 days after the last Abt (1961, ApJS,6,37) observation. Lee (1916, ApJ, 43, 320) has published 60 observations, Campbell (1928, Pub. Lcik Obs. 16, 180 or 257) gives 1 observation, Harper (1937, Publ. Dominion Obs. 7, n.1) 2 more, Abt (1961) 9 data and Voikevitch-Oculitch (1925). Our solution, which is based on the above data except the Harper's ones which have unacceptable O-C residuals, is almost identical to the Lee's one en aconfirms the improvement of the period given by Abt (1961) -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System710Orbit2End System976Orbit2Begin -Ascending node epoch: 2443416.073 -The mean internal error is ~ 0.5 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Our orbital solution is based on 5 observations of Campbell & Moore (1928,Pub. Lick Obs. 16, 180; 1928, Pub. Lick Obs. 16, 257), 5 of Frost et al. (1929, Publ. Yerkes Obs., 7, 1), 18 of Abt (1961, ApJS,6,37), 24 of Abt & Levy (1985, ApJS, 59, 229) and our 67 Asiago Observations have been treated as nightly mean and those are the radial velocities showed in the paper. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System976Orbit2End System1406Orbit2Begin -Ascending node epoch: 2443432.076 -The mean internal error is ~ 2 km sec^-1. -The data and those already published have been combined to improve the spectroscopic orbits. In the orbit computation. the individual observation has been weighted according to the spectrograph dispersion as suggested by Abt & Smith (1969, PASP, 81, 332). - The computing of the standard deviations from the computed curves shows for most of the objects under study a significant improvement has been achived. -Our solution is based on 21 observation of Abt & Levy (1985, ApJS, 59, 229) and 16 of our Asiago. For of our observations are nightly means. The observations of Harper (1937, Publ. Dominion Obs. 7, n.1), Young (1939, Pub. David Dunl. Obs. 1, 71) and Palmer et al. (1968, Roy, Obs. Bull. 145) have not been used in the computation because they do not appear to follow any periodic pattern. -The star have been observed with the two-prism Cassegrain spectroghaph attached to the 1.2m telescope of the Asiago Astrophysical Observatory. System1406Orbit2End System2105Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2105Orbit1End System2106Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2106Orbit1End System2107Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2107Orbit1End System2108Orbit1Begin -Star in double system. -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2108Orbit1End System2109Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2109Orbit1End System2110Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2110Orbit1End System2111Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2111Orbit1End System2112Orbit1Begin -Triple-lined system. Only the SB1 orbit for the short-period pair is determined, the velocities of the other component are given in the comments. -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2112Orbit1End System2113Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2113Orbit1End System2114Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2114Orbit1End System795Orbit2Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System795Orbit2End System2115Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2115Orbit1End System2116Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2116Orbit1End System2117Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2117Orbit1End System2118Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2118Orbit1End System2119Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2119Orbit1End System2120Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2120Orbit1End System2121Orbit1Begin -Triple-lined system. Only the SB1 orbit for the short-period pair is determined, the velocities of the other component are given in the comments. -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2121Orbit1End System2122Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2122Orbit1End System2123Orbit1Begin -For the determination of radial velocities from these spectra for stars with a wide range of rotations, we have developed a digital cross-correlation procedure based on the XCSAO task (Kurtz M.J., Mink D.J., Wyatt W.F., 1992, in: Worrall DM., Biemesderfer C., Barnes J. (eds.) Astronomical Data Analysis Software and Systems 1, ASPC 25, 432) as implemented in the IRAF environment, using a large grid of synthetic template spectra covering the ranges in e efective temperature, gravity, and rotation of our programme stars. For more details see Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338. -We have verified that our radial-velocity zero-point, which was the key subject of Paper I(Nordstrom B., Latham D.W., Morse J., et al., 1994, A&A 287, 338), remains the same to within 100 m s^-1 when using this modified procedure. Thus, our previous results on the systematic and random errors of our radial velocities remain valid for the data presented here. -The second refinement in our technique was the use of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994, ApJ 420, 806), as implemented at CfA (Harvard-Smithsonian Center for Astrophysics) by G. Torres, to extract radial velocities of both components from the observed, blended spectra of 65 doublelined spectroscopic binaries in our sample. System2123Orbit1End System2124Orbit1Begin -Primary's radial velocities were determined from the original spectra (after masking the atmospheric line regions) and from the cleaned spectra. Both results did not differ from each other by more than 2 sigma (2 km/s). Secondary contribution was subtracted in a few iterations what increased primary velocities by only 1.5 sigma. -The primary subtracted spectra show many traces of the secondary lines. A cross-correlation funtion map, calculated using the K2 template, clearly shows maximun corresponding to V0=-12 km/1 and K2= 188 km/s. Direct cross-correlation of the secondary spectra with K2 template produced our set of radial velocities which, after rejecting phases -01 - 0.1 and 01 - 0.6 and a few other deviation points, led to the solution K2=181 +- 5.5 km/s (V0 value was fixed at -12.7 km/s). The difference between K2 obtained using both methods is about 1.5 sigma and at least partly is due to the facts taht the CCF-mapping method (CCF= Cross Correlation Function Map) does not allow to recognize and reject worse spectra. System2124Orbit1End System401Orbit2Begin -Phases were calculated according to the ephemeris adjusted to obtain primary transit at zero phase, which differs from Strassmeier et al. (1988,A&AS, 72,291) ephemeris by delta_phi=0.0226. System401Orbit2End System2125Orbit1Begin -The secondary semi-amplitudes, determined using the CCF-mapping (CCF= Cross Correlation Function Map) and direct cross-correlation, differed by almost 8 km/2 (198 km/s and 206 km, respectively) so, as the final result, we have adopted an average value with a properly increased error estimate; K2=202 +- 6.0 km.s System2125Orbit1End System2126Orbit1Begin -No individual RVs in the paper. -Radial velocities were measured for each star by fitting multiple Gaussians to the Halpha absorption line. The spectra were normalized and then the radial velocities were measured by eye. These velocities were removed from the individual spectra, which were then averaged. The average was fitted with a model consisting of a straight line and three Gaussian components, which were all fixed to have the same velocity. This model fit was then applied to the individual spectra with the velocity allowed to vary. A circular-orbit fit was determined from the measured velocities. The fitted velocities were removed from the spectra, which were then re-averaged. The cycle of averaging, orbit fitting, removing velocities and re-averaging was repeated three times, during which the model fits sharpened and the radial-velocity measurements converged to stable values. If a measured velocity was found to be 2sigma or more from the circular-orbit fit, the spectrum was checked for any irregularities. In two cases, points were rejected because of possible contamination of the spectra by cosmic rays at, or near, the core of Halpha. A fourth Gaussian component was necessary to get a suitable fit to the spectra of PG 0101+039. -The orbital period for each binary was determined by generating a periodogram ( Scargle 1989,ApJ, 343, 874), which highlighted the most likely orbital periods. The data were then fitted with circular orbits for the most likely of these periods. The chi 2 values for the orbital fits rose sharply for periods other than that represented by the peak in each of the periodograms. The reduced chi 2 values for the orbital fits to the next best periods were 27 which rules out any other orbital periods. -No spectral features were identified as belonging to the companion star in the system, whether it was a MS star or a WD. We used the multiple Gaussian fits, generated when we determined the radial velocities, to search for signs of the companion stars around Halpha. The models were subtracted from the data and the residuals were phase-binned and trailed. We also used back projection, computing the integrals of sinusoidal paths through the data for a large range of systemic velocities and semi-amplitudes, and plotting the result with the value of each integral being represented by the intensity in the plot, to search for any orbital variations in the residual spectra that might be due to a faint companion. Neither method revealed any contribution from the companion stars. This is not surprising due to the luminosity of the subdwarf being far higher than that of either a WD or low-mass MS companion. -The reduced chi^2 for the fit to PG 0101+039 is large in comparison with the fits for all the other binaries in the paper. The reduction and wavelength calibration were checked, but no errors were found and the chi 2 value remained unusually high. Single Gaussian fits were made to the He i (6678 Angstroms) line and the derived velocities yielded orbital parameters consistent with those measured from the Halpha lines, with a consistently large chi^2 value. The residual velocities were examined for any evidence of a companion star or rapid periodic radial pulsations as seen in EC14026 stars ( Kilkenny et al. 1997,MNRAS, 285, 640). The best-fitting period to the Halpha residuals was 55 min with an amplitude of 5 km s^-1, inconsistent with the influence of a companion star and far too long a period to be associated with the pulsations of EC14026 stars which have observed periods between 120 and 160 s ( Stobie et al. 1997,MNRAS, 285, 651). Further, no such period was detected in the He i residuals. It remains a possibility that the poor fit could be a result of real physical changes in the sdB component of the binary; however, systematic errors should also be considered. The errors in each radial-velocity measurement were smaller for PG 0101+039 (typically 1.8 km s^-1) than for all other binaries (typically 2.5-3 km s^-1) and hence the errors in all the derived orbital parameters are smaller for PG 0101+039. It is possible that at this accuracy, unaccounted-for systematic errors in the measurement of the velocity of the line features become significant. System2126Orbit1End System2127Orbit1Begin -No individual RVs in the paper. -Radial velocities were measured for each star by fitting multiple Gaussians to the Halpha absorption line. The spectra were normalized and then the radial velocities were measured by eye. These velocities were removed from the individual spectra, which were then averaged. The average was fitted with a model consisting of a straight line and three Gaussian components, which were all fixed to have the same velocity. This model fit was then applied to the individual spectra with the velocity allowed to vary. A circular-orbit fit was determined from the measured velocities. The fitted velocities were removed from the spectra, which were then re-averaged. The cycle of averaging, orbit fitting, removing velocities and re-averaging was repeated three times, during which the model fits sharpened and the radial-velocity measurements converged to stable values. If a measured velocity was found to be 2sigma or more from the circular-orbit fit, the spectrum was checked for any irregularities. In two cases, points were rejected because of possible contamination of the spectra by cosmic rays at, or near, the core of Halpha. -The orbital period for each binary was determined by generating a periodogram ( Scargle 1989,ApJ, 343, 874), which highlighted the most likely orbital periods. The data were then fitted with circular orbits for the most likely of these periods. The chi 2 values for the orbital fits rose sharply for periods other than that represented by the peak in each of the periodograms. The reduced chi 2 values for the orbital fits to the next best periods were 67 which rules out any other orbital periods. -No spectral features were identified as belonging to the companion star in the system, whether it was a MS star or a WD. We used the multiple Gaussian fits, generated when we determined the radial velocities, to search for signs of the companion stars around Halpha. The models were subtracted from the data and the residuals were phase-binned and trailed. We also used back projection, computing the integrals of sinusoidal paths through the data for a large range of systemic velocities and semi-amplitudes, and plotting the result with the value of each integral being represented by the intensity in the plot, to search for any orbital variations in the residual spectra that might be due to a faint companion. Neither method revealed any contribution from the companion stars. This is not surprising due to the luminosity of the subdwarf being far higher than that of either a WD or low-mass MS companion. System2127Orbit1End System2128Orbit1Begin -No individual RVs in the paper. -Radial velocities were measured for each star by fitting multiple Gaussians to the Halpha absorption line. The spectra were normalized and then the radial velocities were measured by eye. These velocities were removed from the individual spectra, which were then averaged. The average was fitted with a model consisting of a straight line and three Gaussian components, which were all fixed to have the same velocity. This model fit was then applied to the individual spectra with the velocity allowed to vary. A circular-orbit fit was determined from the measured velocities. The fitted velocities were removed from the spectra, which were then re-averaged. The cycle of averaging, orbit fitting, removing velocities and re-averaging was repeated three times, during which the model fits sharpened and the radial-velocity measurements converged to stable values. If a measured velocity was found to be 2sigma or more from the circular-orbit fit, the spectrum was checked for any irregularities. In two cases, points were rejected because of possible contamination of the spectra by cosmic rays at, or near, the core of Halpha. -The orbital period for each binary was determined by generating a periodogram ( Scargle 1989,ApJ, 343, 874), which highlighted the most likely orbital periods. The data were then fitted with circular orbits for the most likely of these periods. The chi 2 values for the orbital fits rose sharply for periods other than that represented by the peak in each of the periodograms. The reduced chi 2 values for the orbital fits to the next best periods were 4.2 which rules out any other orbital periods. -No spectral features were identified as belonging to the companion star in the system, whether it was a MS star or a WD. We used the multiple Gaussian fits, generated when we determined the radial velocities, to search for signs of the companion stars around Halpha. The models were subtracted from the data and the residuals were phase-binned and trailed. We also used back projection, computing the integrals of sinusoidal paths through the data for a large range of systemic velocities and semi-amplitudes, and plotting the result with the value of each integral being represented by the intensity in the plot, to search for any orbital variations in the residual spectra that might be due to a faint companion. Neither method revealed any contribution from the companion stars. This is not surprising due to the luminosity of the subdwarf being far higher than that of either a WD or low-mass MS companion. System2128Orbit1End System2129Orbit1Begin -No individual RVs in the paper. -Radial velocities were measured for each star by fitting multiple Gaussians to the Halpha absorption line. The spectra were normalized and then the radial velocities were measured by eye. These velocities were removed from the individual spectra, which were then averaged. The average was fitted with a model consisting of a straight line and three Gaussian components, which were all fixed to have the same velocity. This model fit was then applied to the individual spectra with the velocity allowed to vary. A circular-orbit fit was determined from the measured velocities. The fitted velocities were removed from the spectra, which were then re-averaged. The cycle of averaging, orbit fitting, removing velocities and re-averaging was repeated three times, during which the model fits sharpened and the radial-velocity measurements converged to stable values. If a measured velocity was found to be 2sigma or more from the circular-orbit fit, the spectrum was checked for any irregularities. In two cases, points were rejected because of possible contamination of the spectra by cosmic rays at, or near, the core of Halpha. -The orbital period for each binary was determined by generating a periodogram ( Scargle 1989,ApJ, 343, 874), which highlighted the most likely orbital periods. The data were then fitted with circular orbits for the most likely of these periods. The chi 2 values for the orbital fits rose sharply for periods other than that represented by the peak in each of the periodograms. The reduced chi 2 values for the orbital fits to the next best periods were 25 which rules out any other orbital periods. -No spectral features were identified as belonging to the companion star in the system, whether it was a MS star or a WD. We used the multiple Gaussian fits, generated when we determined the radial velocities, to search for signs of the companion stars around Halpha. The models were subtracted from the data and the residuals were phase-binned and trailed. We also used back projection, computing the integrals of sinusoidal paths through the data for a large range of systemic velocities and semi-amplitudes, and plotting the result with the value of each integral being represented by the intensity in the plot, to search for any orbital variations in the residual spectra that might be due to a faint companion. Neither method revealed any contribution from the companion stars. This is not surprising due to the luminosity of the subdwarf being far higher than that of either a WD or low-mass MS companion. System2129Orbit1End System614Orbit2Begin -No individual RVs in the paper. - Radial velocities measured using HeII(4686) line. The data for this solution comes from the current paper and Niemela (1976, Ap&SS,45,191), Niemela & Moffat (1982, ApJ,259,213). System614Orbit2End System614Orbit3Begin - Radial velocities measured using N V(4603) line. The data for this solution comes from the current paper and Niemela (1976, Ap&SS,45,191), Niemela & Moffat (1982, ApJ,259,213). -Emission-line from current research exhibits a considerably more negative systemic velocity than previous measurements. System614Orbit3End System614Orbit4Begin - Radial velocities measured using N IV(4058) line. System614Orbit4End System645Orbit2Begin -No individual RVs in the paper. - Radial velocities measured using HeII(4686) line. The data for this solution comes from the current paper and Niemela, Mandrini & Mendez (1985, RevMexAA,11,143). System645Orbit2End System645Orbit3Begin - Radial velocities measured using N V(4603) line. The data for this solution comes from the current paper and Niemela, Mandrini & Mendez (1985, RevMexAA,11,143). System645Orbit3End System738Orbit2Begin -No individual RVs in the paper. - Radial velocities measured using HeII(4686) line. The data for this solution comes from the current paper and Mandrini (1983, MSc Thesis, University of Buenos Aires, Argentina). System738Orbit2End System738Orbit3Begin - Radial velocities measured using N V (4603) line. The data for this solution comes from the current paper and Mandrini (1983, MSc Thesis, University of Buenos Aires, Argentina). System738Orbit3End System738Orbit4Begin - Radial velocities measured using N IV(4058) line. Emission shows somewhat more negative systemic radial velocity than previous measurements (Mandrini, 1983). System738Orbit4End System401Orbit3Begin -Our double-lined (SB2) spectroscopic orbit is very well defined, with small errors in the orbital parameters. We note that determinations of the radial velocity semiamplitude of the primary component, K1, agree well in the four existing solutions. -The ephemeris that we used was that of the photometric study of Pribulla et al. (2001,Inf. Bull. Variable Stars, 5056), which covered the time range actually slightly after our observations and gave a perfect agreement for the time of eclipses. Since the published T0 was already shifted from the actual time of observations, we recalculated the published moment to our T0 so that no whole cycles appear in the phase count in Table 2. We also used the orbital period from the same study simplifying it to the six decimal places, 0.593073 days, which was entirely suficient for the duration of our observations. We note that the orbital period cited in the Hipparcos Catalogue (ESA 1997, The Hipparcos and Tycho Catalogues (ESA SP-1200)) was slightly different 0.593075 days, while Pojmanski (1998,Acta Astron., 48, 711) used 0.593071 days. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System401Orbit3End System2130Orbit1Begin -a1 = These data have been given half weight in the orbital solution for RV1. -We caution that there exists certain confusion in the literature as to which component of ADS 2163 should be called A, and which B. On average the southern component, which we identify here with EE Cet, is the fainter of the two, and this agrees with the naming of the stars in the HIP catalog, where the visual binary appears under CCDM J02499+0856. However, in the ADS catalog the names are actually reversed and in SIMBAD it is the northern, brighter component that carries the name of EE Cet. Lampens et al. (2001,A&A, 374, 132) published photometric data for one epoch and gave V(A) = 9.47 and V(B) = 9.83, identifying the southern component as fainter. To complicate things even further, we found that the northern component of ADS 2163 is also a close binary system showing radial velocity variations; this component may very well be a variable star. However, currently we have insufficient radial velocity data to analyze this binary system; we hope to be able to provide such data in one of the subsequent papers of this series. We only note that Nordstrom et al. (1997,A&AS, 126, 21) gave its radial velocity, V0 = + 2.26 +- 0.04 km s^-1, which is similar to the center- of-mass velocity of EE Cet, V0 = +1.60+- 0.93 km s^-1. System2130Orbit1End System2131Orbit1Begin a1/2/12 = These data have been given half weight in the orbital solution for RV1, RV2 or both. - Previous spectral classification suggests a spectral type of about F8; our direct classification is G0 IV, although the spectral type and the luminosity class relate to the combined properties of the triple system. The average radial velocity of the third component, =-3.59 +- 0.12 km s^-1 (the error of a single observation is 0.93 km s^-1), is significantly different from the center-of-mass velocity of the binary, V0=-7.86 +-0.38 km s^-1. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. -We note that the close binary shows rather large radial velocity variations, so that its small photometric variation may be partly due to "dilution" of the close-binary variability signal in the combined light of the visual system. -Our radial velocity orbit is very well defined, mostly as a result of the brightness of the system at Vmax = 7.14. We could very well isolate the signature of the third, slowly rotating star. System2131Orbit1End System2132Orbit1Begin a1/2/12 = These data have been given half weight in the orbital solution for RV1, RV2 or both. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. - Our radial velocity orbit was based on the assumed period of 0.582714 days, as in the HIP catalog. For the initial time of the primary minimum, we used the data in Nelson (2001, Inf. Bull. Variable Stars, 5040), obtained during the span of our observations. The agreement is very good, given the somewhat larger error of our T0 for this star when compared with other binaries. The main reason for the larger error was the relative faintness of this binary (Vmax ~ 10.5) and the fact that we discovered a third "light" in the system. The spectral signature of the third star (which may, but does not have to be, physically associated with the binary) can be seen in the BF as a small feature projecting onto the prominent signature of the primary component. Similar noise fluctuations are common in BFs of faint stars, but this one is always present, at the same radial velocity at all orbital phases. By integrating the amount of light in this additional feature, we could estimate that, at the light maximum of the binary, L3/(L1 + L2) = 0.03 +- 0.01. Because the third-light contribution is so small, we neglected it in our measurement. However, it may have slightly affected the amplitude of the primary component K1 because of the facts that (1) the radial velocities of primary component are, by necessity, always close to V0 and (2) the third component appears to have a very small radial velocity relative to the binary system. - Herczeg (1993,PASP, 105, 911) pointed out that the orbital period of the system is lengthening. System2132Orbit1End System2133Orbit1Begin -GM Dra is a rather uncomplicated contact system of the W type, i.e., with the smaller star eclipsed during the deeper minimum (although the difference in the depth of the eclipses is very small). -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System2133Orbit1End System2134Orbit1Begin -a1 = These data have been given half weight in the orbital solution for RV1 -Our radial velocity orbit is very well defined, mostly thanks to the large brightness of the system, Vmax = 6.62. -Our initial T0 was based on the time determined by Keskin et al. (2000,Inf. Bull. Variable Stars,4855), which was obtained in the middle of our spectroscopic run, but gives a rather large O-C =+0.0224 days. We have no explanation for this discrepancy because our T0 is nominally accurate to 0.0016 days. The binary is a contact system of the W type with the less massive component eclipsed at the deeper minimum; however, the difference in depth is very small. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System2134Orbit1End System2135Orbit1Begin -a12 = These data have been given half weight in the orbital solution for RV1 and RV2 -The photometric variability of the star was discovered by the Hipparcos mission. The period assigned there was equal to one half of the true orbital period. Instead of the exact double of the HIP period, we used the value given by Gomez Forrellad et al. (1999,Inf. Bull. Variable Stars, 4702) of 0.346503 days. Their initial epoch T0 (obtained 3 years before our observations) and the new period predict the moment of the deeper eclipse which agrees well with our determination. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System2135Orbit1End System2136Orbit1Begin -The radial velocity of the only visible component is very well defined. For the initial phasing of our observations we used the original HIP (Hipparcos Project) prediction which gave a time deviation O-C = -0.035 days. System2136Orbit1End System2137Orbit1Begin a2 = These data have been given half weight in the orbital solution for RV2 -Rodriguez et al. (1998,1998, A&A, 336, 920) discovered variability of the star, apparently independently of the HIP (Hipparcos Project) discovery. They classified it as a W UMa type system with a relatively long orbital period of 0.802 days. Newer photometry of Yakut & Ibanoglu (2000,Inf. Bull. Variable Stars, 5002) (used for T0) confirmed that the HIP times-of-minima prediction; in fact, the HIP ephemeris gives a slightly smaller O-C for the time of the primary eclipse. The ubvy photometric data agree with the previous spectral type of F5 Vn, assuming no interstellar reddening. We would tend to give the star a slightly earlier spectral type, F3 V. -As for other triple-lined systems, we measured the radial velocities of the binary after removing the third-body signature from the BF first and then by analyzing the remaining contact-binary BF. -The radial velocity measurements for the third component show some residual dependence on the phase of the close binary, which may indicate some "cross-talk" in the measurements. The semiamplitude of the variations which correlate with the binary phase is about 2.5 km s^-1, which leads to a slightly elevated error per a single-observation of 1.50 km s^-1; for a single sharp-line star we could expect an error at the level of 1.2 1.3 km s^-1 or less. The mean radial velocity of the third component, = -30.64 +- 0.20 km s^-1, is significantly different from the center-of-mass velocity for the binary, V0 = -25.88 +-0.52 km s^-1, which may result from the motion on the 8.9 yr orbit. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System2137Orbit1End System2138Orbit1Begin a1/2/12 = These data have been given half weight in the orbital solution for RV1, RV2 or both. - The triple-star characteristics of the star were handled by us in the same way as for the previously described star in the paper, V2388 Oph. Again we see some unwelcome cross-talk in the radial velocities V3. This case is a bit more extreme than for V2388 Oph, with the error per single observation of 2.86 km s^-1 in place of the expected 1.2-1.3 km s^-1 or less. We do not have a ready explanation for the coupling between the velocities and why the scatter appears to be increased only within the first half of the orbit. The dependence of V3 on the binary-system phase has been observed in some triple stars in our program, but we usually have no simple explanation for its occurrence. However, we are not very concerned about its presence because our goal is the radial velocity orbit of the close binary system, which is in fact very well defined. The average velocity of the third component, = -16.02 +-0.37 km s^-1, can be compared with the center-of-mass velocity of the close binary, V0 = -8.02 +-1.10 km s^-1. - The binary is a long-period contact system of the A-type. Our spectral type suggests elevated luminosity, F5 III, but classification of strongly broadened spectra of contact binaries is not easy, especially when combined with the spectrum of the third component. However, a high luminosity would agree with the relatively large size of the system implied by the long orbital period. -Deviations relative to the simple sine-curve fits to the radial velocity data. Observations leading to entirely unseparable broadening- and correlation-function peaks are blank. These observations may be eventually used in more extensive modeling of broadening functions. System2138Orbit1End System1166Orbit2Begin - Period taken from Stover et al. 1981, ApJ, 240, 597. -Dwarf nova. The radial velocities of the secondary component resulting from the cross-correlation procedure were fitted with a sine curve, to determine the semi-amplitude, K2, phase-zero point, and V0 velocity. The orbital periods are already well-determined for the observed dwarf nova, so we use the values given in the literature. - No individual RVs in the article. System1166Orbit2End System1026Orbit2Begin - Period taken from Hessman 1988, A&AS, 72, 515 -Dwarf nova. The radial velocities of the secondary component resulting from the cross-correlation procedure were fitted with a sine curve, to determine the semi-amplitude, K2, phase-zero point, and V0 velocity. The orbital periods are already well-determined for the observed dwarf nova, so we use the values given in the literature. - No individual RVs in the article. System1026Orbit2End System1326Orbit2Begin - Period taken from Hessman et al. 1984,ApJ, 286,747 -Dwarf nova. The radial velocities of the secondary component resulting from the cross-correlation procedure were fitted with a sine curve, to determine the semi-amplitude, K2, phase-zero point, and V0 velocity. The orbital periods are already well-determined for the observed dwarf nova, so we use the values given in the literature. - No individual RVs in the article. System1326Orbit2End System918Orbit2Begin - Period taken from Horne et al. 1986,PASP, 98, 609. -Dwarf nova. The radial velocities of the secondary component resulting from the cross-correlation procedure were fitted with a sine curve, to determine the semi-amplitude, K2, phase-zero point, and V0 velocity. The orbital periods are already well-determined for the observed dwarf nova, so we use the values given in the literature. - No individual RVs in the article. System918Orbit2End System2139Orbit1Begin -RV(4922): RV measured using 4922 angstroms = HeI line. -RV(Hbeta): RV measured using H-beta Line. -Radial velocities of the binary components were derived by fitting multiple Gaussian profiles to blended features. In cases where the lines of both components were clearly separated, also the SPEFO code was used. When measuring radial velocities, we noticed that the Hbeta line profile strongly deviated from a simple Gaussian, while an approximation of the observed profile by two Gaussians of different widths and depths gave a reasonably good representation of the line features. Velocities of the primary component of the Hbeta line are systematically more negative by about 16 km s^-1 compared to the same component of the He I 4922 line. Most probably, this effect is due to the contribution of the Pickering He II 4859.32 angstrom line. The secondary component is not well separated, and hence its velocities less certain. The same behaviour was observed by us in the case of the O 8-type binary AB Cru (Lorenz et al. 1994,A&A, 291, 185), where this systematic deviation reached 27.7 km s^-1. Unfortunately, we do not know the strength of other He II lines to study the effect of blending of hydrogen Balmer lines with He II components on the radial velocities more quantitatively. The He I line components are well separated, and for the 4922 line easily measurable. The mean difference of both methods (SPEFO versus GAUSS) is +0.9 km s^-1 for the primary and +1.7 km s-1 for the secondary. However, the primary component in the 5015 line always exhibits some asymmetry. (SPEFO: this code compares the line profile with its reflection, see Horn et al. 1996 and Skoda 1996). -When the primary and secondary velocities are solved independently, the systemic velocities differ. For individual V0: K1=123.4, K2=309.8, V0_1 = +40.2, V0_2 = +32.2. System2139Orbit1End System1435Orbit2Begin -RV measured using 4922 angstroms = HeI line. -There are some doubts concerning the period of this binary. Gulliver et al. (1985) give 2.391253d +- 0.000002. This value is based on a series of radial velocity measurements covering 3300 days, so its actual accuracy is about one order of magnitude worse. Using the BV data published by Martin et al. (1990), van Hamme (1992) found "a phase shift of 0.9988''; we got a similar value. Choosing an epoch near the middle of the time interval covered by the Martin et al. measurements, the zero epoch time given in Table 4 can be calculated. According to the HIPPARCOS catalogue, another time of minimum is HJD 2448500.5980. With the van Hamme ephemeris, such a value gives a rather large O-C = -0.0433d. However, if the Kwee-van Woerden method (Kwee & van Woerden 1956) is applied to the HIPPARCOS photometric measurements, a somewhat different time results. - When the primary and secondary velocities are solved independently, the systemic velocities differ. Giving the secondary data half weight, the mean systemic velocity is 11.3 km s^-1, and the respective solution keeping V0 fixed at this value differs only slightly from the individual solutions with different V0 values for both components. A better coverage of the radial velocity curve is needed to disentangle the three spectra more reliably. For individualFor individual V0: K1=116.8, K2=275.8, V0_1=-9.0, V0_2=-15.8. System1435Orbit2End System1222Orbit3Begin -RV(4542) = measurement using line at 4542 angstroms. -RV(4686) = measurement using line at 4686 angstroms. - RV(Hbeta) = measurement using Hbeta line. -Note1: Instead of H-beta, radial velocities measured for H-alpha are given. -The period is variable (e.g., Mayer et al. 1998,A&AS, 130, 311; Degirmenci et al. 1999,A&AS, 134, 327), probably due to strong mass loss via stellar wind (Koch et al. 1979,PASP, 91, 47). Note that the variability of the period was not taken into account by Harries et al. (1997,MNRAS, 285, 277). -As judged by the weakness of the He I lines 4713 and 4922, the star is considerably earlier than O 8, i.e. the classification by Pearce (1952,PASP, 64, 1952) as O 6.5 for the primary and O 7.5 for the secondary appears more correct than that by Hiltner (1956,ApJS, 2, 317) (O 8). It should be remarked that the equivalent widths, as well as FWHMs, are larger for He II 4541 than for He II 4686 line. According to atmospheric models (Napiwotzki 2001,private communication) the equivalent widths of He II 4686 should be larger than that of He II 4541; but the models do explain the larger FWHM of He II 4541. One may compare the V382 Cyg spectra with those of other O-type stars published by Walborn & Fitzpatrick (1990,PASP, 91, 379); among supergiants, He II 4686 appears as an emission line. In our spectra of V382 Cyg, He II 4686 is a net absorption line, though an emission contribution probably reduces the absorption strength. One effect will be that in near quadrature spectra the emission will be most evident at wavelengths between the two binary components, i.e. around V0, the result would be as observed, and amplitudes of both components should be smaller than derived from the 4686 line. Velocities obtained from He II 4541 would then be more realistic, i.e., both K1,2 would be smaller by several percent, and masses would be smaller by about 10%. System1222Orbit3End System2140Orbit1Begin -Period from HIPPARCOS -RV(4922), RV(4713): RV measured using 4922 and 4713 angstroms= HeI lines. -RV(Hbeta): RV measured using H-beta Line. -RV(Halpha): RV measured using H-alpha line -Our spectra were taken before the binary character of the star was known, and, of course, without knowledge of its ephemeris, so the phase coverage is not very good. -The secondary line is only discernable - at favourable phases - as an extended wing of the 4922 primary line, and hence its position is only poorly determined -To solve the light curve as well as the radial velocity curve, we applied the code FOTEL (Hadrava 1990,Contrib. Astron. Inst. Skalnate Pleso, 20, 23; Hadrava, 1995,A&AS, 114, 393), which solves the light and velocity curves simultaneously. -Radial velocities as well as photometry do not provide sufficient constraints to define the system. It is clear that the deeper minimum is the secondary minimum, in the sense that the smaller, less luminous (and probably also less massive) star with nearly invisible spectral lines is eclipsed. At the phase when the more luminous star is behind the secondary component, the mutual distance of both components is so large that practically no eclipse occurs. -The minimum time of the deeper minimum derived from the FOTEL solution comes out very close to the time determined by HIPPARCOS data. The following ephemeris results: Sec.min.= HJD 2448508.517 + 9.36575d E This ephemeris has been used through this paper, since the time of the deeper minimum is well defined and independent of any orbital solution. System2140Orbit1End System901Orbit2Begin -Orbital elements corresponds to Solution IV in Table 2 in the paper. -To search for further periods we use only the new RVs found here and subtract orbital solution III. The window function of the data is completely dominated by the 1 d alias peaks. The highest peak in the periodogram of the residuals corresponds to a period of P1 = 58d (K1 = 0.58 km/s, probably a brown dwarf companion). In the residuals, the highest peak corresponds to 0.60d which is a 1 d alias of P2 = 1.49d, the period corresponding to the second highest peak. -From Table 2 the different periods found in the RVs are: -P1 = 57.67 +- 0.22 K1 = 0.58 -P2 = 1.4822 +- 0.0014 K2 = 0.51 -P3 = 0.210599 +- 0.000029 K3 = 0.17 -P4 = 0.223824 +- 0.000033 K4 = 0.16 -Harper's (1928, Publ. DAO, 4, 179) values for Solution IV: V0_Harper = -32.55 0.94 rms_Harper = 5.30 System901Orbit2End System410Orbit2Begin - Orbital elements derived for the data set including the new (320) RVs and the old (208) RV values of Scholz et al. 1997, A&A, 320, 791 (PaperI) -For the recalculation of orbital elements we first compare the iron RVs of Table 4, -13.996 kms^-1, with the RVs following from the orbital solution of Paper I which distinguishes between several solutions based on different data sets. From Paper I we choose solution 4 which shows minimum scatter. With the binary period of 4614.51d the orbital phase of our new CCD spectrograms is 0.58, and the corresponding RV is -13.05 kms^-1. Thus, the new CCD RVs are about 1 kms^-1 below the expected one. In order to improve the orbital elements we combine the RVs used for the derivation of solution 4 of PaperI with our RVs determined from the Fe lines. Weights were adopted according to the weighting scheme given in PaperI. Fixing the period of solution 4 we get the new orbital solution. This new orbital solution should be compared with solution 4 of PaperI. One can see that the orbital elements are only marginally changed but the accuracy is evidently improved. -Old orbital parameters derived from data from Kamper & Beardsley (1987, AJ, 94, 1302), Fekel & Tomkin (1993, AJ, 106, 1156), and Scholz et al. (1997, A&A, 320, 791 ): -P 4614.51 -K1 11.90 +- 0.17 -V0 11.74 +- 0.13 -e 0.8941 +- 0.0035 -T 43996.95 +- 0.77 -w 312.2 +- 1.4 -rms 0.92 System410Orbit2End System1348Orbit2Begin -deltaRV1/2: non-Keplerian velocity corrections. -The radial velocities were measured by using cross-correlation. A spectrum of 10 Lac was used as the template, and the H-delta and H-gamma lines were excluded from the cross-correlation calculation. The cross-correlation function (CCF) peaks were well separated at quadrature, and were fitted by using a digital profile constructed from the autocorrelation function of a template spectrum, artificially broadened by a 100 km s^-1 rotational broadening function. The fits to the CCF at quadratures was generally excellent , and it was found that the FWHM of the two digital profiles was constant to within 620 km s^-1. For the more blended CCFs the FWHM of the fitting functions were fixed to the mean values derived from the quadrature fits (310 and 245 km s^-1 for the primary and secondary respectively). We found no evidence, either in the spectra or in the CCFs, for a strengthening of the spectral features of either component when the star is appoaching (the Struve Sahade effect). -We measured velocities along with the non-Keplerian corrections required by the photometric solution. We solved the radial velocity curve by using the RVORBIT program (Hill 1986,unpublished DAO manual), fixing the period at 3.070507 d (Howarth et al. 1991,Observatory, 111, 167) and solving for the systemic velocity, the two semi-amplitudes, the eccentricity, the longitude of periastron and the time of periastron. The resulting eccentricity (e = 0.017 +- 0.084) was insignificant, so we adopted a circular orbit, fitting for the systemic velocity, the two semi-amplitudes and the time of maximum positive velocity of the primary. -We note that the semi-amplitude of the primary (94.6 +- 1.1 km s^-1) is slightly larger than that found by Howarth et al. (89.0 +- 1.3 km s^-1), but the semi-amplitude of the secondary is in excellent agreement with their value. Howarth et al. found a statistically significant eccentricity of 0.0310 +- 0.0068 from their IUE radial velocity curve, which had better phase coverage than that presented here. One possible explanation is that the Howarth et al. measurements (which were made using Gaussian fits to the CCFs rather than digital profiles) are affected by systematic errors owing to blending at conjunction phases, which may introduce a spurious eccentricity. We stress that the derived semi-amplitudes from the two radial velocity curves are in good agreement, despite this small discrepancy in the orbital eccentricity. System1348Orbit2End System216Orbit3Begin -The system is triple, composed by a close binary orbiting (period=2.7) a masive companion (period=50.7 days). The RVs of the tertiary are given in the paper. -A circular orbit fit was made to the to the measured radial velocities, fixing the period at 2.698393 days (Mayer et al. 1994,A&A, 288, L13) and solving for the time of maximum positive velocity and the two semi-amplitudes. - The primary semi-amplitude differs considerably from that quoted by Mayer et al. (1994) based on a preliminary analysis of their spectra. -The non-Keplerian corrections were found to be negligible for this detached system. System216Orbit3End System322Orbit2Begin - Triple system, comprising a semi-detached binary (P = 1.9 days) and a gravitationally bound tertiary (P = 294 days) which contributes ~15 25 per cent to the total radiation. -deltaRV1/2: non-Keplerian velocity corrections. -The double-peaked cross-correlation functions (CCFs) were fitted by using two-component Gaussian profiles, which gave a satisfactory fit at all phases. We found no evidence for the Struve-Sahade effect. The results is a circular orbit solution to the radial velocity curve, fixing the period at 1.811474 days (Mayer&Drechsel 1987). The semi-amplitudes of these new velocity curves are quite different from those reported by Mammano et al. (1977, A&A, 59, 9), owing presumably to our data having significantly higher spectral resolution, by more than a factor of 2, and to our improved techniques of measuring radial velocities. -We have studied the observed minus calculated O-C residuals between the observed velocities of both components and the values calculated according to our orbital solution for IU Aur. The data were obtained effectively at three epochs, separated by 276 and 758 days. These residuals do not show clear evidence for any motion about a third body, but we note, in agreement with Mammano et al., that these (O-C) residuals are substantially larger than we would expect for the quality of spectra employed in this study. System322Orbit2End System969Orbit3Begin -Orbital elements computed from visual and spectroscopic observations by the method described by Morley (1975, PASP, 87, 689). The visual elements are: a=0.97", Node = 152.7 deg. P = 46.43 +- 0.03 years, T0= 1962.52 +- 0.02. System969Orbit3End System306Orbit3Begin -Orbital elements for primary and secondary were determined separately as SB1 solutions, with fixed period (adopted from Bagnuolo & Hartkopf 1989, AJ, 98, 2275) and circular orbit. The elements for the primary (cooler, sharp-lined) star are given in the catalog (except for the mean V0 for both components), the secondary's (hotter) elements are: V0=26.98 +-0.39, T0=42118.825 +-0.260. -rms: mean error of an observation of unit weight. System306Orbit3End System583Orbit2Begin -The improved orbit of the close sub-system Aab of the visual binary 20 Leo AB is computer here. -New velocities and Fekel and Bopp (1977,PASP,89,658 ) data were combined in order to calculate the orbital elements of the spectroscopic binary. -The quality of the velocities was determined from the scatter in a solution for the elements for each component. The rms1 and rms2 have weights of 0.4 and 1.0 respectively. The rms residual for the simultaneous solution was determined to be 1.66 km s^-1. -Once velocities were weighted, orbital elements for the double-lined case were computed assuming a nonzero eccentricity. The eccentricity was found to be negligible and zero eccentricity therefore was adopted. System583Orbit2End System1331Orbit2Begin -Observations using plates. -We have considered all plates to have equal weight: internal mean errors of measurement are about 1.5 km s^-1, with only a few lying outside the range 1 km s^-1 to 2 km s^-1. -The close agreement between spectroscopic and photometric times of T0 leads us to believe that the true orbit is circular. -We do not believe that there is evidence for any variation in V0, although the possibility cannot be completely ruled out. The present value appears to differ significantly from those of Batten (1961,Pub. Dominion Astrophys. Obs. 11, 395) and Steward (1958, JRASC, 52, 11), but we have already explained that the true uncertainty in our value of V0 is probably greater than the formal errors suggest. - We cannot rule out the possibility that pulsations of the primary star are affecting the value derived for K1. -We used lines 432.5767 nm FeI and 450.8283 nm FeII when we found that the scatter of their measures was satisfactory and that their mean residuals did not differ significantly from zero. The remaining five lines each gave self-consistent results, but their mean residuals from the plate means defined by the five best lines ranged in absolute value from 6 km s^-1 to 20 km s^-1. We can identify at least one plausible blending component for each of them, and we have more or less arbritrary adjusted the rest wavelengths of this second set of five lines to give the same mean velocity as does the first set. This would be a questionable procedure if we were aiming to set up a standard wavelength system suitable for all A-type spectra. Our concern, however, is to strengthen the measurements of the spectrum of one star (not all of the best five lines can always be measured) and we are more interested in the range of velocity variation (K1) than the mean value (V0). We have found no significant differences between orbital solutions based on measures of the first five lines and all ten, but V0 is about 0.6 kms^-1 more negative when the ten-line set is used. As expected, the larger number of lines leads to smaller random errors, but the possibility that a systematic error exists in V0, of the order of -1 km s^-1, should be remembered when comparisons are made between our results and the earlier ones. -Period and eccentricity assumed (as defined by Sterne 1941, Pr. Nat. Acad. Sci. Washington, 97, 175) -rms: mean error of a single plate. System1331Orbit2End System2141Orbit1Begin - rms = external mean error of an average plate. -DAO48: data taken with the 1.2 m telescope and the coude spectrograph of the Dominion Astrophysical Observatory (DAO) at a reciprocal dispersion of 1.0 nm mm^-1. -DAO72:data taken with the 1.8 m telescope and the Cassegrain spectrograph of the Dominion Astrophysical Observatory (DAO) at a reciprocal dispersion of 1.5 nm mm^-1. System2141Orbit1End System1172Orbit3Begin -Long-period spectroscopic orbit of the hot secondary component B to the classical Cepheid SY Cyg. This star B is also a 4.675-day spectroscopic binary. To derive the long-period orbit of the Bab center-of-mass around the Cepheid, the short-period variations and constant velocity were subtracted (hence V0=0; true center-of-mass velocity of the Cepheid is -21.45 km/s), and the long-period elements of A were adopted from Evans (1988 ApJS, 66, 343). -LWR = long-wavelength redundant IUE camera. -LWP = long-wavelength prime IUE camera. -SWP = short-wavelength prime IUE camera. -The orbital elements were calculated with the same Chi^2 minimization program used to determine the Cepheid's orbit (Evans 1988, ApJS, 32, 399). The program was run in the triple star mode in order to determine the velocity amplitude of the center of mass of SU Cyg Ba and Bb in the long-period, simultaneously. The other long period orbital elements were fixed at the values determined from the Cepheid's orbit, and the short-period orbit was assumed to be circular. System1172Orbit3End System2142Orbit1Begin -Short-period spectroscopic orbit of the hot secondary component B to the classical Cepheid SY Cyg. This star B is also a 4.675-day spectroscopic binary. To derive the short-period orbit, the long-period variations and constant velocity were subtracted (hence V0=0; true center-of-mass velocity of the Cepheid is -21.45 km/s). -LWR = long-wavelength redundant camera -LWP = long-wavelength prime camera -SWP = short-wavelength prime camera System2142Orbit1End System709Orbit3Begin -The primary is a Cepheid S Mus. The orbital parameters did not change by more than the formal errors when two different Cepheid's pulsation periods were used. The RVs have the pulsational component (P=9.66d, 5 harmonics) subtracted. -The orbital solution are performed as described by Evans. -The orbital solution is was made giving the new data (Bohm-Vitense) very low weight (weight =0.01). The mean residual of the new data from this solution (-1.8+-0.2) km s^-1) was added to the new data for the final solution, to put all data on a consistent velocity scale). -A: Paddock (Campbell and Moore, 1928,Pub.Lick Obs.,16,180); dispersion 41 Angstrom mm^-1. -B: Stibbs, 1955, MNRAS,136,91; 49 Angstrom mm^-1. -C: Evans 1968,MNRAS,141,109; 49 Angstrom mm^-1. -D: Evans 1980,S.Afr.Astron.Obs.,1,257; 49 Angstrom mm^-1. -E: Evans 1980,S.Afr.Astron.Obs.,1,257; 29 Angstrom mm^-1. -F: Bohm-Vitense et al. 1990,ApJ,229,212; 2.4 Angstrom mm^-1. System709Orbit3End System709Orbit4Begin -This orbital parameters are calculated since the eccentricity of the adopted solution (Orbit 1) is very small.The most important difference between the circular solution and the full solution is that the velocity amplitude is 0.9 km s^-1 smaller in the circular solution. System709Orbit4End System415Orbit2Begin -About eccentricity: The secondary minimum is exactly centered on phase 0.5 (in photometric light curve); hence a circular orbit can be assumed, and is also supported by the symmetric shape of the radial velocity curve. -P and T0 according to Vogt & Sterken (1993,IBVS, 3958) -Radial velocities used to evaluate V0 and K1: results from He I lines in case of DAO, Ondrejov, Rozen, Asiago and Calar data, and from NII, SII lines in case of Lick and ESO data. -CalarAlto_XXX_D: used HeI 6678. -The range in the Notes is the spectral coverage in angstroms. - DAO: Photographic spectra were obtained at the Dominion Astrophysical Observatory (Canada) with the coude spectrograph of the 1.2 m telescope, with a dispersion of 6.5 Angstroms mm^-1; -Ondrejov: this spectra were obtained at the Dominion Astrophysical Observatory (Canada) with the coude spectrograph of the 2 m telescope, with a dispersion of 17 Angstroms mm^-1. -Rozen: this spectra were obtained at the Dominion Astrophysical Observatory (Canada) with the coude spectrograph of the 2 m telescope and a dispersion of 17 Angstroms mm^-1 -RETICON: electronic spectra were taken at the Dominion Astrophysical -Observatory with the coude spectrograph of the 2 m telescope with -dispersion 20 Angstroms mm^-1 CCD: data taken the Cassegrain -spectrograph of the 1.8 m telescope with dispersion 15 Angstroms -mm^-1 -For the present purpose, the old data were not used. From the new DAO spectra radial velocities were determined using lines of HeI, SiII and MgII. From these velocities we get K1 = 92.2 km s^-1 and V0 = +27.9 km s^-1. System415Orbit2End System1948Orbit3Begin -A quarduple system consisting of the eclipsing 6-day system (called B) and another binary (A) which orbit is given here. The likely period of AB is 40-50 yrs, as estimated from the light-time effect. -Comment Notes: ECH = ESO 1.5 m with ECHELEC spectrograph, CAT = 1.4 m ESO CAT/coude echelle spectrograph(CES). -Data of Morrison and Conti (MC, 1980 ApJ 239, 212) are used to refine the period, but a V0=-8.1 is found for that data set. The solutions somewhat depend on the assumed data weighting. Since the rms values for MC velocities and for our data were about 12 and 7 km/s, respectively, we gave the MC velocities a weight of 1, to ECHELEC velocities a weight of 2, and to CAT velocities a weight of 3. An independent solution of the MC data con rmed the original results by MC. -The large rms value of our high resolution data is somewhat unexpected and must be due to intrinsic variability of unknown nature. The error of fitting the Gaussians to line profiles is not larger than 2 km/s. The deviations of the velocities from the anticipated orbital curve therefore represent real shifts of line positions. -We first tried to obtain a solution of our radial velocity data alone. However, due to a gap in the phase coverage of the velocity curve, the correlation among spectroscopic elements turned out to be strong, and solutions tended to be non-unique: e.g., possible solutions implied a relatively broad parameter range for K1. More decisive results were expected when our data were combined with the older published data. However, a combined solution of different data sets requires the assumption of different velocities for widely separated epochs. In view of the long-term radial velocity changes due to the mutual orbit of the two binary systems A and B, different values of V0 are to be expected for data with long time separations. MC also noted a discrepancy between velocities obtained from different lines, so the intended combination of the MC and LMS data with our measurements required some caution. Therefore, we only considered HeI measurements. -Expected light-time effect: From our detailed line blend fitting we found that the systemic velocities of both binaries changed on a time base of approximately 17 years by 11 and +36 kms 1 for systems A (long period) and B (short period), respectively. System1948Orbit3End System635Orbit4Begin -A quarduple system consisting of the eclipsing 6-day system (called B, the orbit is here) and another 20.7-day binary (A). The likely period of AB is 40-50 yrs, as estimated from the light-time effect. - Few velocities of the secondary were measured, but no K2 amplitude is derived. -Spectral type according to Walborn (1973, ApJ, 179, 517) -Comment Notes: ECH = ESO 1.5 m with ECHELEC spectrograph, CAT = 1.4 m ESO CAT/coude echelle spectrograph(CES). -Expected light-time effect: From our detailed line blend fitting we found that the systemic velocities of both binaries changed on a time base of approximately 17 years by 11 and +36 kms 1 for systems A (long period) and B (short period), respectively. System635Orbit4End System2144Orbit1Begin -Eclipsing binary. No individual RV data. -Eccentricity e=0 is assumed by the authors. -V0 is the arithmetic mean of two different solutions. V0_1= -0.03 km s^-1 and V0_2=-1.80 km s^-1. The V0 error us due to the uncertainty of the V0_1 and V0_2. H-Beta and HeII(4859) have been used to determine V0_1 and V0_2 respectively. -Using photometry the following ephemeris has been determined by the authors: JD(phi=0) = 2448687.4928(5) + 3.4133135(2)E -The radial velocity curve of each stellar component was fitted separately, using sine functions and the Newton-Raphson method as parameter optimization procedure. System2144Orbit1End System2145Orbit1Begin (*) = due to total eclipse only primary lines are visible - Circular orbit assumed. Err1/2: mean fit error (Chi^2-based estimation of profile fit quality) - Instrument used for observation: ECH=1.52m ESO telescope + Echelle spectrograph; CAT=1.4m ESO CAT/coude Echelle spectrograph (CES) -Systemic velocities for each component: V0_1 = 23.6 km s^-1 and V0_2= 3.0 km s^-1. The large difference of the systemic velocities, which of course cannot be real, is a well-known and so far unexplained effect in early-type SB2 systems and was already discussed by Mayer et al. (1991, BAC 42, 230). In order to obtain consistent radial velocity curves for both stellar components, the arithmetic mean was taken as the final systemic velocity. -The differences between calculated (i.e. fitted) and observed radial velocities of H-alpha are very similar to those of He I 4922 in the respective range of the orbital phase, and no systematic deviation is present. Only the H based velocities from one ECHELEC spectrum (given one third weight of the CAT spectra) are about 25 km s^-1 below the fitted curve both for the primary and secondary component. -Period and T0 calculated from photometry. The period before the year 1992 appears to be slightly shorter (1.4950932 days). The secondary eclipse minimum of the light curve shows a phase of totality lasting about 0.030 in phase (about 1 hour). System2145Orbit1End System1022Orbit3Begin -rms in this case is the mean error of an observation of unit weight. -Data comes from the complete series of Lick Observatory radial-velocity measurements was published by Berman (1932, Lick Obs. Bull, 16, 24). We remeasured the plates by modern methods (the original measurements were by Hartmann spectrocomparator against a spectrum of Arcturus as a standard) to see if we could eliminate the large residuals and improve the determination of period. - The first five spectrograms (1897-1902) were obtained with the original Mills 3-prism spectrograph and the remainder (after 1905) with the new Mills spectrograph (Lick Observatory). -For the New Mills Spectrograph: Correction of -0.78 km/s is applied to bring to the Victoria system. The internal mean errors of velocities derived from these lines range from 0.27 kms^-1 to 0.96 kms^-1: the mean is 0.46 kms^-1 and only four exceed 0.6 km s^-1. There are a few large differences between our measurements and Berman's (for the primary component, the differences range from -2.27 kms^-1 to +0.88 kms^-1 in the sense Berman minus Victoria) but the two sets (including the data obtained with the original instrument) of measures correlates well.Most individual differences are less than 1 kms^-1 and the mean is -0.42 +- 0.13 kms^-1. -For the Original Mills Spectrograph: the standard deviation of a single measure was 2.0 kms^-1 for 19 of them and only just exceeded that value for the twentieth. We have probably somewhat exaggerated the internal precision of our measures (internal mean errors range from 0.29 kms^-1 to 0.67 kms^-1, with a mean of 0.44 kms^-1) and have certainly sacrificed information about the true zero point. Of the five plates, our measures of two - the first and the last - differ rather strongly from Berman's, in opposite directions as judged from the mean for all five. Thus, the systematic difference between us is large and uncertain. For our first set of measures it was it was -3.79 +- 0.69 kms^-1 (Berman minus Victoria) and we were dissatisfied enough to remeasure all five plates. The mean difference between our two sets of measures is -0.95 +- 0.64 kms^-1. -The orbital elements corresponds to the combined solution of our data and Heintz (1988, JRASC, 82, 140) are: P = 88.30 yr (32251.6 d) T0 = 19834.30 (JD 2445431.699) e = 0.495 w(A) = 193.2 K1 = 3.37 K2 = 4.20 ,V0 = -7.15 System1022Orbit3End System2146Orbit1Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System2146Orbit1End System2147Orbit1Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System2147Orbit1End System2148Orbit1Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System2148Orbit1End System2149Orbit1Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System2149Orbit1End System2150Orbit1Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System2150Orbit1End System1580Orbit2Begin (*) = Velocities from Luck and Bond (1991,ApJS, 77,515) - Present observations were made at the Dominion Astrophysical Observatory in Victoria, using the radial-velocity spectrometer at the coude focus of the 1.2-m telescope. It is capable of a precision of about +-0.3 km s^-1, although with the limited integration time for each observation, the observational error for the sgCH stars is closer to double that value. - The orbit were first calculated using only the data from the present set of observations, giving the velocities from Luck and Bond (1991) zero weight. Residuals from the velocity curves of their observations were calculated and a systematic difference of +0.85 km s-^1 was found with a mean error of +- 0.38 km s^-1. The Luck and Bond data were all shifted by -0.8 km s^-1, therefore, and the orbits were calculated again, giving all observations unit weight.The resulting average residual for the Luck and Bond data from the final orbital calculations is +0.04 +- 0.15 km s^-1. System1580Orbit2End System2151Orbit1Begin -Observation were performed with the radial-velocity spectrometer on the 1.2-m telescope of the Dominion Astrophysical Observatory. Although the instrument is capable of a precision of about +- 0.3 km s^-1, because of the faintness of the R stars and the limited time spend per observation, the final errors were larger than this. System2151Orbit1End System2152Orbit1Begin -Observation were performed with the radial-velocity spectrometer on the 1.2-m telescope of the Dominion Astrophysical Observatory. Although the instrument is capable of a precision of about +- 0.3 km s^-1, because of the faintness of the R stars and the limited time spend per observation, the final errors were larger than this. System2152Orbit1End System2153Orbit1Begin -The JD epochs and T0 are given in "MJD" in Griffin's notation (0.5 day shift). -"rej_V2" : Two V2 Cambridge observations, which differ from the mean by more than 3 standard deviations, have been rejected. -Data source: P = Palomar observation (Griffin and Gunn,1974,ApJ,191,545); C=Cambridge Observation, (Griffin, 1967,ApJ,148,465) ; S = Dominion Astrophysical Observatory (D.A.O.) observation (Scarfe, present work); H= Heintz (1981, ApJS, 46,247); G = D.A.O. observation (Griffin, R. and R., Observatory,102,217) -The DAO data of C.D.S. have been adjusted to the International Astronomical Union (IAU) system in the manner described by Fletcher et al. (1982,PASP,94,1017). All other velocities have been measured differentially against the Cambridge reference star 63 Aur (Griffin, 1967, ApJ,148,465;Griffin, 1969,MNRAS,145,163) and an effort has been made to place them on the IAU system by the application of a correction of -0.8 km s^-1 (Griffin and Herbig, 1981, MNRAS, 196,33) -All of our own observations except for a few near to the descending in the short orbit show some degree of blending, but many can be resolved either by eye (on Cambridge traces) or by computer. -The constancy of the visual secondary's velocity indicates that we may safely assume that the systemic velocity of the short-period pair, V0_A, has also remained constant, and combine all the resolved observations of the primary into a single solution for the short-period elements. A solution led to an eccentricity smaller than its standard error. A circular orbit was therefore tried, and the resulting increase in the sum of squared residuals, from 28.46 to 28.85 km^2 s^-2 was not significant. System2153Orbit1End System1873Orbit2Begin -The system is a K-dwarf binary. -New observations are added to those of Griffin (1987, Obs, 108, 194) to improve the orbit. -Only a short abstract is published with the elements, but no RVs. System1873Orbit2End System2154Orbit1Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2154Orbit1End System290Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System290Orbit2End System407Orbit3Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System407Orbit3End System2155Orbit1Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2155Orbit1End System450Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System450Orbit2End System548Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System548Orbit2End System678Orbit2Begin -Ba II star system. -Excellent agreement with the orbit of Griffin & Griffin (180, MNRAS, 193, 957). Their RVs were given a correction of -0.8 km/s and combined with the new data to derive the orbit. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System678Orbit2End System1566Orbit2Begin -Ba II star system. -The JD2447314.781 point is apparently removed from the orbit computation. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System1566Orbit2End System2156Orbit1Begin -Ba II star system. -V0 given in Table 4 wrongly as -16.4 km/s is corrected to 16.4 km/s. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2156Orbit1End System1568Orbit2Begin -Ba II star system. -The observations do not yet cover the complete orbital cycle. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System1568Orbit2End System2157Orbit1Begin -Ba II star system. -The observations do not yet cover the complete orbital cycle. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2157Orbit1End System1279Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System1279Orbit2End System1306Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System1306Orbit2End System2158Orbit1Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2158Orbit1End System1581Orbit2Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System1581Orbit2End System2159Orbit1Begin -Ba II star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2159Orbit1End System2160Orbit1Begin -CH star system. - The observation JD2445051.664 VR=-258.56 is apparently excluded by the authors from the orbital solution. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2160Orbit1End System2161Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2161Orbit1End System2162Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2162Orbit1End System2163Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2163Orbit1End System2164Orbit1Begin -CH star system. -More than 17 points is apparent on the RV curve given by the authors, but no mention of other data used is made in the paper or in the tables. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2164Orbit1End System2165Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2165Orbit1End System2166Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2166Orbit1End System2167Orbit1Begin -CH star system. -The standard deviation of a single observation for late-type stars brighter than about 11th magnitude, such as those reported in this paper, is better than 0.5 km s^-1. The velocities have been standadized to the system of velocities published by Fletcher et al (1992, PASP, 94, 1017), except for a small scale error which affects the velocities in that paper at the 01-0.2 km s^-1 level. System2167Orbit1End System817Orbit2Begin -Short-period orbit of the single-lined triple system. The RVs are as observed and include both short- and long-period variations superimposed. -In comment column, P indicates a photographic observation; F1, F2 and K indicate spectrometer observations with the old and new F-star masks and the K-star mask, respectively. All observatinos were obtained by C.D.Scarfe, except those labeled as Harris (1977) and Funakawa (1980). The observation on 1981 April 20 was accorded zero weight in the solutions. -In adition to spectroscopy solution, visual-binary elements were obtained from speckle data, with the spectrospically determined period imposed to them. In each case the representation of the data by the combined solution is closely similar to that by the separate ones. We have tried without success to establish a connection between the speckle residuals and the short spectroscopic period. System817Orbit2End System818Orbit2Begin -Long-period orbit of the single-lined triple system. The RVs are as observed and include both short- and long-period variations superimposed. -The value for w refers to the primary. -In adition to spectroscopy solution, visual-binary elements were obtained from speckle data, with the spectrospically determined period imposed to them. In each case the representation of the data by the combined solution is closely similar to that by the separate ones. We have tried without success to establish a connection between the speckle residuals and the short spectroscopic period. -The elements in common between the visual and spectroscopic solutions (e, w and T for the wide pair), showed a good agreement, and combined solution was therefore obtained, satisfying the speckle and spectroscopic data simultaneously. -In comment column, P indicates a photographic observation; F1, F2 and K indicate spectrometer observations with the old and new F-star masks and the K-star mask, respectively. All observatinos were obtained by C.D.Scarfe, except those labeled as Harris (1977) and Funakawa (1980). The observation on 1981 April 20 was accorded zero weight in the solutions. System818Orbit2End System375Orbit2Begin Double-lined orbit of the short-period sub-system in a triple star. The long-period variation is not removed from the individual RVs, the solution of short- and long-period orbits was found simultaneously, and V0 reflects the long-period motion. DAO - Dominion Astrophysical Observatory 1.2 m telescope. KPNO - Kitt Peak National Observatory, observations with the feed telescope coude and coude spectrograph. -Preliminary solutions of the radial velocities alone showed that the effect of applying light-time corrections to the times of the observations is negligible on either the elements or their uncertainties. Such corrections reduce the sum of the weighted squares of residuals by only a statistically insignificant 7%, and none have therefore been used in the final solution. Moreover, no improvement in the precision of the periods was achieved by including observations other than our own; hence, nor have those older data been used. -We have retained the weighting scheme adopted by Fekel & Scarfe (1986, AJ, 92, 1162); in it, all the new observations of the primary star, Aa, were given weight 3.0, and all velocities of the secondary, Ab, received half the weight given to the corresponding primary-star velocity. Because the radial velocities are much more numerous than System375Orbit2End System2169Orbit1Begin Long-period sub-system in a triple star. The RVs correspond to the center-of-mass of the 14.57-day sub-system (calculated from the known mass ratio, not observed directly). The orbit is a combined solution using eight Center for High Angular Resolution Astronomy (CHARA) speckle observations. A simultaneous solution of those data, together with all of our radial velocities, has been found, with the threedimensional differential correction program (Fekel et al. 1997, AJ, 113, 1095). The element w was changed to correspond to the Aab center-of-mass. -We have retained the weighting scheme adopted by Fekel & Scarfe (1986, AJ, 92, 1162); in it, all the new observations of the primary star, Aa, were given weight 3.0, and all velocities of the secondary, Ab, received half the weight given to the corresponding primary-star velocity. Because the radial velocities are much more numerous than System2169Orbit1End System1412Orbit2Begin -V0_a = -15 +- 1 km s^-1 and V0_b= 9 +- 5 -All observations were given the same weight (1.0) except the one RV2 observation labeled as "weight_0" in comment column (weight = 0.0) -The Period was held fixed at its photometrically determined value (Barlow and Forbes, 1980, Inf. Bull. Variable Stars, 1882, 130, 69). System1412Orbit2End System2170Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4043.0 days = 971.2 periods f(M) = 0.00828 +/- 0.00040 solar masses a1 sin i = 1.533 +/- 0.025 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). They have been included here. System2170Orbit1End System2171Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6265.9 days = 0.4 periods f(M) = 0.0271 +/- 0.0044 solar masses a1 sin i = 523. +/- 111. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2171Orbit1End System2172Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4085.8 days = 2.0 periods f(M) = 0.0188 +/- 0.0077 solar masses a1 sin i = 125. +/- 17. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2172Orbit1End System2173Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1499.9 days = 107.6 periods f(M) = 0.000629 +/- 0.000020 solar masses a1 sin i = 1.452 +/- 0.015 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2173Orbit1End System2174Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 7099.5 days = 0.7 periods f(M) = 0.063 +/- 0.031 solar masses a1 sin i = 522. +/- 179. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2174Orbit1End System2175Orbit1Begin Time span of observations = 1627 days M1 (sin i)**3 = 0.02993 +/- 0.00079 solar masses M2 (sin i)**3 = 0.02816 +/- 0.00076 solar masses q = 0.941 +/- 0.014 a sin i = 12.52 +/- 0.11 x 10**6 km Light ratio L2/L1 = 0.90 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 4 km/s System2175Orbit1End System2176Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5146.0 days = 1.1 periods f(M) = 0.260 +/- 0.010 solar masses a1 sin i = 533.5 +/- 8.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2176Orbit1End System2177Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1189.7 days = 1.9 periods f(M) = 0.0826 +/- 0.0061 solar masses a1 sin i = 91.9 +/- 2.4 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2177Orbit1End System2178Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5201.9 days = 9.1 periods f(M) = 0.0025 +/- 0.0014 solar masses a1 sin i = 27.4 +/- 5.2 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2178Orbit1End System2179Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5025.3 days = 11.2 periods f(M) = 0.00798 +/- 0.00097 solar masses a1 sin i = 34.4 +/- 1.4 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2179Orbit1End System545Orbit2Begin Time span of observations = 3286 days M1 (sin i)**3 = 0.792 +/- 0.067 solar masses M2 (sin i)**3 = 0.638 +/- 0.033 solar masses q = 0.80 +/- 0.03 a sin i = 77.3 +/- 1.8 x 10**6 km Light ratio L2/L1 = 0.25 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 6 km/s System545Orbit2End System2180Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5214.0 days = 0.9 periods f(M) = 0.0122 +/- 0.0015 solar masses a1 sin i = 213. +/- 14. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2180Orbit1End System2181Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5706.2 days = 3.3 periods f(M) = 0.0035 +/- 0.0023 solar masses a1 sin i = 64. +/- 15. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2181Orbit1End System2182Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 910.6 days = 11.3 periods f(M) = 0.0137 +/- 0.0016 solar masses a1 sin i = 13.06 +/- 0.52 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2182Orbit1End System2183Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3622.9 days = 1.7 periods f(M) = 0.0188 +/- 0.0020 solar masses a1 sin i = 130.4 +/- 5.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2183Orbit1End System2184Orbit1Begin Time span of observations = 3067 days M1 (sin i)**3 = 0.287 +/- 0.015 solar masses M2 (sin i)**3 = 0.2214 +/- 0.0069 solar masses q = 0.77 +/- 0.02 a sin i = 19.89 +/- 0.28 x 10**6 km Light ratio L2/L1 = 0.20 Rotational velocities: v1 sin i = 5 km/s v2 sin i = 5 km/s System2184Orbit1End System2185Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3723.9 days = 1.5 periods f(M) = 0.054 +/- 0.016 solar masses a1 sin i = 205. +/- 21. x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2185Orbit1End System2186Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5582.9 days = 25.5 periods f(M) = 0.00206 +/- 0.00028 solar masses a1 sin i = 13.55 +/- 0.61 x 10**6 km Rotational velocity v sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2186Orbit1End System2187Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5280.7 days = 4.7 periods f(M) = 0.00097 +/- 0.00065 solar masses a1 sin i = 31.4 +/- 6.8 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2187Orbit1End System2188Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4874.7 days = 1.2 periods f(M) = 0.00670 +/- 0.00052 solar masses a1 sin i = 138.6 +/- 4.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2188Orbit1End System2189Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6601.9 days = 1.2 periods f(M) = 0.0155 +/- 0.0013 solar masses a1 sin i = 228.6 +/- 10.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2189Orbit1End System2190Orbit1Begin Time span of observations = 3399 days M1 (sin i)**3 = 0.975 +/- 0.095 solar masses M2 (sin i)**3 = 0.765 +/- 0.053 solar masses q = 0.79 +/- 0.04 a sin i = 756 +/- 22 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 4 km/s System2190Orbit1End System2191Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3367.8 days = 1.9 periods f(M) = 0.00462 +/- 0.00028 solar masses a1 sin i = 71.0 +/- 1.4 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2191Orbit1End System2192Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 200.8 days = 7.9 periods f(M) = 0.001132 +/- 0.000051 solar masses a1 sin i = 2.638 +/- 0.040 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2192Orbit1End System1707Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1886.0 days = 2.0 periods f(M) = 0.00226 +/- 0.00034 solar masses a1 sin i = 37.2 +/- 2.0 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1707Orbit2End System2193Orbit1Begin Time span of observations = 2665 days M1 (sin i)**3 = 0.969 +/- 0.099 solar masses M2 (sin i)**3 = 0.739 +/- 0.043 solar masses q = 0.76 +/- 0.04 a sin i = 274.3 +/- 7.6 x 10**6 km Light ratio L2/L1 = 0.10 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 2 km/s System2193Orbit1End System1676Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 867.6 days = 3.8 periods f(M) = 0.0099 +/- 0.0012 solar masses a1 sin i = 23.43 +/- 0.93 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1676Orbit2End System2194Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6211.0 days = 2.4 periods f(M) = 0.00345 +/- 0.00077 solar masses a1 sin i = 83.8 +/- 6.2 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2194Orbit1End System2195Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6886.1 days = 3.5 periods f(M) = 0.041 +/- 0.017 solar masses a1 sin i = 159. +/- 22. x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2195Orbit1End System2196Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 826.8 days = 4.0 periods f(M) = 0.00379 +/- 0.00049 solar masses a1 sin i = 15.99 +/- 0.69 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2196Orbit1End System2197Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5426.2 days = 14.0 periods f(M) = 0.075 +/- 0.013 solar masses a1 sin i = 65.8 +/- 3.8 x 10**6 km Rotational velocity v sin i = 10 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2197Orbit1End System2198Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5418.1 days = 18.5 periods f(M) = 0.0000189 +/- 0.000007 solar masses a1 sin i = 3.45 +/- 0.43 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2198Orbit1End System2199Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6913.1 days = 1.9 periods f(M) = 0.0174 +/- 0.0092 solar masses a1 sin i = 179. +/- 29. x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2199Orbit1End System2200Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1908.8 days = 290.4 periods f(M) = 0.05832 +/- 0.00096 solar masses a1 sin i = 3.984 +/- 0.022 x 10**6 km Rotational velocity v sin i = 12 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2200Orbit1End System2201Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 719.1 days = 100.6 periods f(M) = 0.0822 +/- 0.0023 solar masses a1 sin i = 4.725 +/- 0.043 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2201Orbit1End System2202Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1628.7 days = 2.1 periods f(M) = 0.0339 +/- 0.0036 solar masses a1 sin i = 80.6 +/- 2.8 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2202Orbit1End System2203Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2682.6 days = 10.1 periods f(M) = 0.00048 +/- 0.00014 solar masses a1 sin i = 9.49 +/- 0.94 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2203Orbit1End System2204Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2477.1 days = 1.9 periods f(M) = 0.0140 +/- 0.0021 solar masses a1 sin i = 84.0 +/- 4.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2204Orbit1End System1492Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1929.7 days = 4.1 periods f(M) = 0.000467 +/- 0.000089 solar masses a1 sin i = 13.69 +/- 0.88 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1492Orbit2End System1704Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2300.8 days = 2.0 periods f(M) = 0.0055 +/- 0.0010 solar masses a1 sin i = 56.1 +/- 3.7 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1704Orbit2End System2205Orbit1Begin Time span of observations = 3275 days M1 (sin i)**3 = 0.468 +/- 0.017 solar masses M2 (sin i)**3 = 0.3818 +/- 0.0085 solar masses q = 0.816 +/- 0.015 a sin i = 12.81 +/- 0.13 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 0 km/s System2205Orbit1End System2206Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5500.9 days = 1.7 periods f(M) = 0.00112 +/- 0.00054 solar masses a1 sin i = 67. +/- 12. x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2206Orbit1End System2207Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5483.0 days = 2.0 periods f(M) = 0.26 +/- 0.14 solar masses a1 sin i = 371. +/- 67. x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2207Orbit1End System2208Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4840.7 days = 25.0 periods f(M) = 0.0173 +/- 0.0038 solar masses a1 sin i = 25.4 +/- 1.8 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2208Orbit1End System760Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 503.9 days = 31.1 periods f(M) = 0.01077 +/- 0.00040 solar masses a1 sin i = 4.140 +/- 0.052 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System760Orbit2End System2209Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3165.1 days = 273.1 periods f(M) = 0.000434 +/- 0.000036 solar masses a1 sin i = 1.136 +/- 0.032 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2209Orbit1End System2210Orbit1Begin Time span of observations = 5837 days M1 (sin i)**3 = 0.420 +/- 0.033 solar masses M2 (sin i)**3 = 0.372 +/- 0.018 solar masses q = 0.89 +/- 0.04 a sin i = 263.2 +/- 5.6 x 10**6 km Light ratio L2/L1 = 0.45 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 6 km/s System2210Orbit1End System2211Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3694.0 days = 5.6 periods f(M) = 0.0047 +/- 0.0022 solar masses a1 sin i = 37.4 +/- 5.9 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2211Orbit1End System2212Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 7160.3 days = 1.1 periods f(M) = 0.0301 +/- 0.0032 solar masses a1 sin i = 311. +/- 16. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2212Orbit1End System908Orbit3Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1792.1 days = 7.9 periods f(M) = 0.2647 +/- 0.0089 solar masses a1 sin i = 69.76 +/- 0.78 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System908Orbit3End System2213Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3576.1 days = 26.8 periods f(M) = 0.0512 +/- 0.0020 solar masses a1 sin i = 28.37 +/- 0.36 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2213Orbit1End System2214Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1152.9 days = 7.5 periods f(M) = 0.0775 +/- 0.0062 solar masses a1 sin i = 35.68 +/- 0.95 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2214Orbit1End System2215Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6361.8 days = 1.0 periods f(M) = 0.0774 +/- 0.0043 solar masses a1 sin i = 416. +/- 12. x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2215Orbit1End System2216Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4517.6 days = 12.7 periods f(M) = 0.00080 +/- 0.00019 solar masses a1 sin i = 13.6 +/- 1.1 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2216Orbit1End System2217Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3378.8 days = 1.3 periods f(M) = 0.0142 +/- 0.0037 solar masses a1 sin i = 133. +/- 12. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2217Orbit1End System2218Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1930.0 days = 2.3 periods f(M) = 0.00654 +/- 0.00051 solar masses a1 sin i = 49.0 +/- 1.3 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2218Orbit1End System1672Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1937.7 days = 1.9 periods f(M) = 0.00301 +/- 0.00095 solar masses a1 sin i = 42.7 +/- 4.5 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1672Orbit2End System1673Orbit2Begin Time span of observations = 201 days M1 (sin i)**3 = 0.557 +/- 0.011 solar masses M2 (sin i)**3 = 0.546 +/- 0.010 solar masses q = 0.98 +/- 0.01 a sin i = 47.92 +/- 0.30 x 10**6 km Light ratio L2/L1 = 0.90 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 4 km/s System1673Orbit2End System2219Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2016.6 days = 5.9 periods f(M) = 0.00229 +/- 0.00024 solar masses a1 sin i = 18.79 +/- 0.67 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2219Orbit1End System2220Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2627.8 days = 1.1 periods f(M) = 0.0690 +/- 0.0045 solar masses a1 sin i = 211.2 +/- 5.7 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2220Orbit1End System1491Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 557.8 days = 1.7 periods f(M) = 0.00690 +/- 0.00038 solar masses a1 sin i = 26.74 +/- 0.47 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1491Orbit2End System1696Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 773.8 days = 9.5 periods f(M) = 0.000247 +/- 0.000042 solar masses a1 sin i = 3.45 +/- 0.19 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1696Orbit2End System2221Orbit1Begin Time span of observations = 1195 days M1 (sin i)**3 = 0.460 +/- 0.025 solar masses M2 (sin i)**3 = 0.395 +/- 0.013 solar masses q = 0.86 +/- 0.02 a sin i = 32.61 +/- 0.47 x 10**6 km Light ratio L2/L1 = 0.30 Rotational velocities: v1 sin i = 8 km/s v2 sin i = 12 km/s System2221Orbit1End System2222Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4790.0 days = 19.3 periods f(M) = 0.0440 +/- 0.0024 solar masses a1 sin i = 40.81 +/- 0.73 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2222Orbit1End System2223Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4894.7 days = 1.7 periods f(M) = 0.0275 +/- 0.0098 solar masses a1 sin i = 177. +/- 22. x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2223Orbit1End System1702Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2067.5 days = 1.2 periods f(M) = 0.0122 +/- 0.0015 solar masses a1 sin i = 95.4 +/- 4.4 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1702Orbit2End System2224Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 7068.7 days = 1.8 periods f(M) = 0.00055 +/- 0.00012 solar masses a1 sin i = 58.6 +/- 4.4 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2224Orbit1End System1703Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3636.0 days = 7.4 periods f(M) = 0.097 +/- 0.010 solar masses a1 sin i = 84.0 +/- 2.8 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1703Orbit2End System2225Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4845.8 days = 1.7 periods f(M) = 0.0611 +/- 0.0040 solar masses a1 sin i = 235.5 +/- 5.5 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2225Orbit1End System2226Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6564.0 days = 8.1 periods f(M) = 0.00157 +/- 0.00047 solar masses a1 sin i = 29.5 +/- 3.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2226Orbit1End System2227Orbit1Begin Time span of observations = 1685 days M1 (sin i)**3 = 0.236 +/- 0.018 solar masses M2 (sin i)**3 = 0.1939 +/- 0.0094 solar masses q = 0.82 +/- 0.03 a sin i = 132.5 +/- 2.8 x 10**6 km Light ratio L2/L1 = 0.35 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 4 km/s System2227Orbit1End System1698Orbit2Begin Time span of observations = 1826 days M1 (sin i)**3 = 0.906 +/- 0.030 solar masses M2 (sin i)**3 = 0.799 +/- 0.022 solar masses q = 0.88 +/- 0.02 a sin i = 204.8 +/- 2.0 x 10**6 km Light ratio L2/L1 = 0.50 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 4 km/s System1698Orbit2End System1699Orbit2Begin Time span of observations = 416 days M1 (sin i)**3 = 0.797 +/- 0.035 solar masses M2 (sin i)**3 = 0.611 +/- 0.015 solar masses q = 0.765 +/- 0.015 a sin i = 11.07 +/- 0.13 x 10**6 km Light ratio L2/L1 = 0.12 Rotational velocities: v1 sin i = 12 km/s v2 sin i = 0 km/s System1699Orbit2End System2228Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2637.9 days = 87.4 periods f(M) = 0.000178 +/- 0.000045 solar masses a1 sin i = 1.60 +/- 0.13 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2228Orbit1End System1705Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2975.0 days = 16.2 periods f(M) = 0.0325 +/- 0.0049 solar masses a1 sin i = 30.2 +/- 1.5 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1705Orbit2End System2229Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4044.2 days = 2.8 periods f(M) = 0.0029 +/- 0.0011 solar masses a1 sin i = 53.5 +/- 6.9 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2229Orbit1End System1687Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 618.9 days = 36.6 periods f(M) = 0.00105 +/- 0.00013 solar masses a1 sin i = 1.961 +/- 0.083 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1687Orbit2End System2230Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6986.9 days = 0.8 periods f(M) = 0.059 +/- 0.013 solar masses a1 sin i = 476. +/- 53. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2230Orbit1End System2231Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2741.3 days = 13.3 periods f(M) = 0.0343 +/- 0.0016 solar masses a1 sin i = 33.22 +/- 0.53 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2231Orbit1End System2232Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5420.1 days = 0.8 periods f(M) = 0.0100 +/- 0.0032 solar masses a1 sin i = 228. +/- 37. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2232Orbit1End System2233Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5434.1 days = 0.8 periods f(M) = 0.0531 +/- 0.0050 solar masses a1 sin i = 405. +/- 43. x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2233Orbit1End System2234Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3949.3 days = 1.4 periods f(M) = 0.0131 +/- 0.0017 solar masses a1 sin i = 134.7 +/- 6.1 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2234Orbit1End System2235Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5434.1 days = 0.4 periods f(M) = 0.0133 +/- 0.0036 solar masses a1 sin i = 405. +/- 187. x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2235Orbit1End System2236Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 892.7 days = 27.6 periods f(M) = 0.0044 +/- 0.0012 solar masses a1 sin i = 4.89 +/- 0.45 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2236Orbit1End System1245Orbit2Begin Time span of observations = 2653 days M1 (sin i)**3 = 0.721 +/- 0.052 solar masses M2 (sin i)**3 = 0.607 +/- 0.024 solar masses q = 0.84 +/- 0.03 a sin i = 47.81 +/- 0.92 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 12 km/s System1245Orbit2End System2237Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1793.0 days = 85.4 periods f(M) = 0.001286 +/- 0.000059 solar masses a1 sin i = 2.424 +/- 0.037 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2237Orbit1End System2238Orbit1Begin Time span of observations = 3013 days M1 (sin i)**3 = 0.682 +/- 0.032 solar masses M2 (sin i)**3 = 0.580 +/- 0.020 solar masses q = 0.85 +/- 0.02 a sin i = 73.70 +/- 0.98 x 10**6 km Light ratio L2/L1 = 0.30 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 8 km/s System2238Orbit1End System2239Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1895.8 days = 6.0 periods f(M) = 0.0578 +/- 0.0080 solar masses a1 sin i = 52.8 +/- 2.4 x 10**6 km Rotational velocity v sin i = 10 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2239Orbit1End System2240Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1865.8 days = 1.6 periods f(M) = 0.0430 +/- 0.0079 solar masses a1 sin i = 112.8 +/- 6.9 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2240Orbit1End System2241Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 888.9 days = 18.0 periods f(M) = 0.00515 +/- 0.00052 solar masses a1 sin i = 6.81 +/- 0.23 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2241Orbit1End System2242Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6698.8 days = 0.7 periods f(M) = 0.057 +/- 0.011 solar masses a1 sin i = 511. +/- 79. x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2242Orbit1End System2243Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5178.7 days = 98.1 periods f(M) = 0.00504 +/- 0.00013 solar masses a1 sin i = 7.062 +/- 0.060 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2243Orbit1End System2244Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1353.3 days = 1.5 periods f(M) = 0.0262 +/- 0.0038 solar masses a1 sin i = 81.3 +/- 4.4 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2244Orbit1End System1678Orbit2Begin Time span of observations = 1975 days M1 (sin i)**3 = 0.647 +/- 0.011 solar masses M2 (sin i)**3 = 0.5396 +/- 0.0074 solar masses q = 0.83 +/- 0.02 a sin i = 72.97 +/- 0.35 x 10**6 km Light ratio L2/L1 = 0.10 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System1678Orbit2End System2245Orbit1Begin Time span of observations = 5858 days M1 (sin i)**3 = 1.09 +/- 0.21 solar masses M2 (sin i)**3 = 0.84 +/- 0.14 solar masses q = 0.77 +/- 0.06 a sin i = 962 +/- 64 x 10**6 km Light ratio L2/L1 = 0.25 Rotational velocities: v1 sin i = 2 km/s v2 sin i = 4 km/s System2245Orbit1End System2246Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3662.9 days = 2.1 periods f(M) = 0.0764 +/- 0.0036 solar masses a1 sin i = 179.1 +/- 2.9 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2246Orbit1End System2247Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1510.8 days = 3.8 periods f(M) = 0.0293 +/- 0.0017 solar masses a1 sin i = 48.84 +/- 0.90 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2247Orbit1End System2248Orbit1Begin Time span of observations = 2244 days M1 (sin i)**3 = 0.432 +/- 0.018 solar masses M2 (sin i)**3 = 0.400 +/- 0.011 solar masses q = 0.92 +/- 0.02 a sin i = 84.21 +/- 0.98 x 10**6 km Light ratio L2/L1 = 0.40 Rotational velocities: v1 sin i = 2 km/s v2 sin i = 2 km/s System2248Orbit1End System2249Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3446.6 days = 5.6 periods f(M) = 0.0101 +/- 0.0041 solar masses a1 sin i = 45.8 +/- 6.1 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2249Orbit1End System2250Orbit1Begin Time span of observations = 1118 days M1 (sin i)**3 = 0.0740 +/- 0.0038 solar masses M2 (sin i)**3 = 0.0686 +/- 0.0025 solar masses q = 0.93 +/- 0.03 a sin i = 13.66 +/- 0.19 x 10**6 km Light ratio L2/L1 = 0.50 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 10 km/s System2250Orbit1End System2251Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 986.1 days = 2.1 periods f(M) = 0.00078 +/- 0.00018 solar masses a1 sin i = 16.2 +/- 1.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2251Orbit1End System2252Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5075.2 days = 1.5 periods f(M) = 0.060 +/- 0.017 solar masses a1 sin i = 262. +/- 25. x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2252Orbit1End System2253Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3298.0 days = 1.5 periods f(M) = 0.0179 +/- 0.0048 solar masses a1 sin i = 131. +/- 15. x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2253Orbit1End System2254Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4790.9 days = 1.2 periods f(M) = 0.0232 +/- 0.0014 solar masses a1 sin i = 205.0 +/- 5.5 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2254Orbit1End System2255Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5525.0 days = 1.2 periods f(M) = 0.0090 +/- 0.0011 solar masses a1 sin i = 167.3 +/- 7.0 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2255Orbit1End System2256Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1247.8 days = 46.6 periods f(M) = 0.03088 +/- 0.00031 solar masses a1 sin i = 8.219 +/- 0.027 x 10**6 km Rotational velocity v sin i = 23 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2256Orbit1End System2257Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5230.0 days = 1.2 periods f(M) = 0.00374 +/- 0.00099 solar masses a1 sin i = 119. +/- 11. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2257Orbit1End System1680Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 360.0 days = 47.8 periods f(M) = 0.002936 +/- 0.000087 solar masses a1 sin i = 1.612 +/- 0.016 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1680Orbit2End System2258Orbit1Begin Time span of observations = 4988 days M1 (sin i)**3 = 0.454 +/- 0.037 solar masses M2 (sin i)**3 = 0.422 +/- 0.024 solar masses q = 0.93 +/- 0.04 a sin i = 663 +/- 16 x 10**6 km Light ratio L2/L1 = 0.40 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System2258Orbit1End System2259Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4608.3 days = 1.1 periods f(M) = 0.0296 +/- 0.0030 solar masses a1 sin i = 230.8 +/- 8.7 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2259Orbit1End System2260Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 353.0 days = 7.2 periods f(M) = 0.01405 +/- 0.00060 solar masses a1 sin i = 9.45 +/- 0.14 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2260Orbit1End System2261Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5076.9 days = 2.1 periods f(M) = 0.00428 +/- 0.00091 solar masses a1 sin i = 86.0 +/- 6.3 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2261Orbit1End System1689Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1421.0 days = 6.0 periods f(M) = 0.0064 +/- 0.0015 solar masses a1 sin i = 20.9 +/- 1.6 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1689Orbit2End System1690Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1326.6 days = 68.4 periods f(M) = 0.00213 +/- 0.00016 solar masses a1 sin i = 2.720 +/- 0.067 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1690Orbit2End System2262Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 7300.9 days = 1.1 periods f(M) = 0.0108 +/- 0.0030 solar masses a1 sin i = 223. +/- 26. x 10**6 km Rotational velocity v sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2262Orbit1End System2263Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4046.9 days = 2.5 periods f(M) = 0.00414 +/- 0.00099 solar masses a1 sin i = 64.9 +/- 5.3 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2263Orbit1End System2264Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4037.9 days = 9.2 periods f(M) = 0.0962 +/- 0.0044 solar masses a1 sin i = 77.6 +/- 1.2 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2264Orbit1End System2265Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4833.8 days = 1.8 periods f(M) = 0.00643 +/- 0.00098 solar masses a1 sin i = 104.6 +/- 5.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2265Orbit1End System2266Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1394.0 days = 29.3 periods f(M) = 0.01619 +/- 0.00050 solar masses a1 sin i = 9.725 +/- 0.099 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2266Orbit1End System2267Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1538.4 days = 2.3 periods f(M) = 0.00307 +/- 0.00024 solar masses a1 sin i = 33.00 +/- 0.83 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2267Orbit1End System2268Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1524.8 days = 18.8 periods f(M) = 0.0794 +/- 0.0049 solar masses a1 sin i = 23.60 +/- 0.48 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2268Orbit1End System1700Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1898.7 days = 35.9 periods f(M) = 0.00201 +/- 0.00021 solar masses a1 sin i = 5.21 +/- 0.18 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1700Orbit2End System2269Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 658.0 days = 9.2 periods f(M) = 0.0171 +/- 0.0012 solar masses a1 sin i = 13.00 +/- 0.30 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2269Orbit1End System2270Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4494.8 days = 1.5 periods f(M) = 0.086 +/- 0.017 solar masses a1 sin i = 270. +/- 19. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2270Orbit1End System1706Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 7029.8 days = 3.1 periods f(M) = 0.0048 +/- 0.0020 solar masses a1 sin i = 85. +/- 12. x 10**6 km Rotational velocity v sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1706Orbit2End System2271Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 185.6 days = 9.0 periods f(M) = 0.00918 +/- 0.00015 solar masses a1 sin i = 4.623 +/- 0.025 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2271Orbit1End System2272Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5198.1 days = 1.1 periods f(M) = 0.041 +/- 0.010 solar masses a1 sin i = 285. +/- 43. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2272Orbit1End System1671Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3460.7 days = 10.0 periods f(M) = 0.215 +/- 0.011 solar masses a1 sin i = 86.6 +/- 1.4 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1671Orbit2End System2273Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1614.6 days = 5.9 periods f(M) = 0.00728 +/- 0.00025 solar masses a1 sin i = 23.96 +/- 0.28 x 10**6 km Rotational velocity v sin i = 6 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2273Orbit1End System2274Orbit1Begin Time span of observations = 1111 days M1 (sin i)**3 = 0.741 +/- 0.028 solar masses M2 (sin i)**3 = 0.581 +/- 0.013 solar masses q = 0.78 +/- 0.01 a sin i = 27.61 +/- 0.28 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System2274Orbit1End System2275Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2934.9 days = 24.2 periods f(M) = 0.0100 +/- 0.0053 solar masses a1 sin i = 15.5 +/- 2.7 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2275Orbit1End System2276Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5176.9 days = 0.8 periods f(M) = 0.0055 +/- 0.0014 solar masses a1 sin i = 173. +/- 30. x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2276Orbit1End System1677Orbit2Begin Time span of observations = 159 days M1 (sin i)**3 = 0.861 +/- 0.011 solar masses M2 (sin i)**3 = 0.7631 +/- 0.0063 solar masses q = 0.886 +/- 0.006 a sin i = 32.43 +/- 0.11 x 10**6 km Light ratio L2/L1 = 0.30 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System1677Orbit2End System2277Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3214.2 days = 1.8 periods f(M) = 0.063 +/- 0.020 solar masses a1 sin i = 173. +/- 19. x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2277Orbit1End System2278Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3680.0 days = 9.2 periods f(M) = 0.0369 +/- 0.0041 solar masses a1 sin i = 52.7 +/- 2.0 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2278Orbit1End System1686Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 381.9 days = 6.3 periods f(M) = 0.00268 +/- 0.00022 solar masses a1 sin i = 6.28 +/- 0.17 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1686Orbit2End System1536Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5280.3 days = 1.5 periods f(M) = 0.00071 +/- 0.00018 solar masses a1 sin i = 60.0 +/- 5.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1536Orbit2End System2279Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 554.7 days = 7.3 periods f(M) = 0.00377 +/- 0.00014 solar masses a1 sin i = 8.17 +/- 0.10 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2279Orbit1End System2280Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3242.0 days = 4.4 periods f(M) = 0.00470 +/- 0.00043 solar masses a1 sin i = 39.9 +/- 1.2 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2280Orbit1End System2281Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2165.0 days = 11.2 periods f(M) = 0.00208 +/- 0.00038 solar masses a1 sin i = 12.52 +/- 0.78 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2281Orbit1End System2282Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5438.1 days = 6.8 periods f(M) = 0.00043 +/- 0.00036 solar masses a1 sin i = 18.9 +/- 5.3 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2282Orbit1End System2283Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2605.8 days = 1.4 periods f(M) = 0.0228 +/- 0.0038 solar masses a1 sin i = 124.7 +/- 9.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2283Orbit1End System2284Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3006.0 days = 1.5 periods f(M) = 0.0201 +/- 0.0068 solar masses a1 sin i = 125. +/- 14. x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2284Orbit1End System584Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 879.8 days = 259.5 periods f(M) = 0.01408 +/- 0.00018 solar masses a1 sin i = 1.5954 +/- 0.0069 x 10**6 km Rotational velocity v sin i = 9 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System584Orbit2End System2285Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1188.8 days = 52.6 periods f(M) = 0.0351 +/- 0.0033 solar masses a1 sin i = 7.66 +/- 0.24 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2285Orbit1End System2286Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5229.7 days = 1.0 periods f(M) = 0.0212 +/- 0.0035 solar masses a1 sin i = 239. +/- 14. x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2286Orbit1End System2287Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4518.8 days = 1.5 periods f(M) = 0.00882 +/- 0.00051 solar masses a1 sin i = 128.3 +/- 2.5 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2287Orbit1End System1688Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6893.0 days = 5.5 periods f(M) = 0.00116 +/- 0.00054 solar masses a1 sin i = 35.6 +/- 5.7 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1688Orbit2End System2288Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5410.0 days = 0.9 periods f(M) = 0.0222 +/- 0.0090 solar masses a1 sin i = 274. +/- 84. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2288Orbit1End System2289Orbit1Begin Radial velocities in original publication were omitted by mistake. They have been included here. Time span of observations = 4032 days M1 (sin i)**3 = 0.684 +/- 0.095 solar masses M2 (sin i)**3 = 0.673 +/- 0.063 solar masses q = 0.98 +/- 0.07 a sin i = 398 +/- 15 x 10**6 km Light ratio L2/L1 = 0.50 Rotational velocities: v1 sin i = 7 km/s v2 sin i = 10 km/s System2289Orbit1End System2290Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3142.3 days = 1.8 periods f(M) = 0.070 +/- 0.010 solar masses a1 sin i = 176.8 +/- 9.0 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2290Orbit1End System2291Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3419.7 days = 1.2 periods f(M) = 0.0058 +/- 0.0016 solar masses a1 sin i = 104.7 +/- 10.0 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2291Orbit1End System1693Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1857.9 days = 31.0 periods f(M) = 0.0116 +/- 0.0014 solar masses a1 sin i = 10.15 +/- 0.40 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1693Orbit2End System1694Orbit2Begin Time span of observations = 1930 days M1 (sin i)**3 = 0.0683 +/- 0.0016 solar masses M2 (sin i)**3 = 0.0618 +/- 0.0012 solar masses q = 0.91 +/- 0.01 a sin i = 14.64 +/- 0.10 x 10**6 km Light ratio L2/L1 = 0.40 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 6 km/s System1694Orbit2End System2292Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2705.8 days = 1.1 periods f(M) = 0.0263 +/- 0.0027 solar masses a1 sin i = 159.8 +/- 6.6 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2292Orbit1End System180Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2013.7 days = 1043.4 periods f(M) = 0.0955 +/- 0.0016 solar masses a1 sin i = 2.075 +/- 0.012 x 10**6 km Rotational velocity v sin i = 37 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System180Orbit2End System1679Orbit2Begin Time span of observations = 1854 days M1 (sin i)**3 = 0.4920 +/- 0.0052 solar masses M2 (sin i)**3 = 0.4738 +/- 0.0039 solar masses q = 0.963 +/- 0.005 a sin i = 12.187 +/- 0.037 x 10**6 km Light ratio L2/L1 = 0.70 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 6 km/s System1679Orbit2End System2293Orbit1Begin Time span of observations = 2978 days M1 (sin i)**3 = 0.231 +/- 0.018 solar masses M2 (sin i)**3 = 0.212 +/- 0.017 solar masses q = 0.92 +/- 0.04 a sin i = 100.3 +/- 2.5 x 10**6 km Light ratio L2/L1 = 0.65 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System2293Orbit1End System2294Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2110.1 days = 2.0 periods f(M) = 0.0252 +/- 0.0019 solar masses a1 sin i = 88.3 +/- 2.2 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2294Orbit1End System2295Orbit1Begin Time span of observations = 4465 days M1 (sin i)**3 = 0.554 +/- 0.017 solar masses M2 (sin i)**3 = 0.519 +/- 0.014 solar masses q = 0.94 +/- 0.02 a sin i = 264.7 +/- 2.5 x 10**6 km Light ratio L2/L1 = 0.60 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 2 km/s System2295Orbit1End System2296Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5360.1 days = 2.3 periods f(M) = 0.0168 +/- 0.0029 solar masses a1 sin i = 131.1 +/- 7.5 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2296Orbit1End System2297Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4046.8 days = 13.3 periods f(M) = 0.000127 +/- 0.000041 solar masses a1 sin i = 6.67 +/- 0.72 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2297Orbit1End System1695Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2221.9 days = 23.3 periods f(M) = 0.0186 +/- 0.0025 solar masses a1 sin i = 16.19 +/- 0.73 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1695Orbit2End System2298Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5821.0 days = 4.9 periods f(M) = 0.00173 +/- 0.00021 solar masses a1 sin i = 39.4 +/- 1.6 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2298Orbit1End System2299Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1858.9 days = 40.0 periods f(M) = 0.00175 +/- 0.00024 solar masses a1 sin i = 4.55 +/- 0.21 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2299Orbit1End System2300Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1209.6 days = 83.4 periods f(M) = 0.04422 +/- 0.00033 solar masses a1 sin i = 6.155 +/- 0.015 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2300Orbit1End System2301Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4766.1 days = 1.5 periods f(M) = 0.0410 +/- 0.0036 solar masses a1 sin i = 218.5 +/- 7.0 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2301Orbit1End System2302Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5117.0 days = 273.1 periods f(M) = 0.00533 +/- 0.00045 solar masses a1 sin i = 3.61 +/- 0.10 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2302Orbit1End System2303Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6610.9 days = 43.8 periods f(M) = 0.000109 +/- 0.000036 solar masses a1 sin i = 3.96 +/- 0.44 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2303Orbit1End System2304Orbit1Begin Time span of observations = 3330 days M1 (sin i)**3 = 0.859 +/- 0.044 solar masses M2 (sin i)**3 = 0.831 +/- 0.040 solar masses q = 0.97 +/- 0.03 a sin i = 646 +/- 10 x 10**6 km Light ratio L2/L1 = 0.90 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 4 km/s System2304Orbit1End System1697Orbit2Begin Time span of observations = 1226 days M1 (sin i)**3 = 0.456 +/- 0.010 solar masses M2 (sin i)**3 = 0.4223 +/- 0.0071 solar masses q = 0.93 +/- 0.01 a sin i = 13.634 +/- 0.087 x 10**6 km Light ratio L2/L1 = 0.70 Rotational velocities: v1 sin i = 5 km/s v2 sin i = 10 km/s System1697Orbit2End System2305Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2845.0 days = 14.1 periods f(M) = 0.000136 +/- 0.000046 solar masses a1 sin i = 5.18 +/- 0.58 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2305Orbit1End System2306Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1977.8 days = 1.2 periods f(M) = 0.0373 +/- 0.0019 solar masses a1 sin i = 135.1 +/- 2.5 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2306Orbit1End System2307Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3737.9 days = 2.1 periods f(M) = 0.0135 +/- 0.0010 solar masses a1 sin i = 103.4 +/- 2.8 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2307Orbit1End System2308Orbit1Begin Original velocities published by Mazeh et al. (1995), (1995ApJ...449..909M) Time span of observations = 3396 days M1 (sin i)**3 = 0.478 +/- 0.036 solar masses M2 (sin i)**3 = 0.447 +/- 0.034 solar masses q = 0.93 +/- 0.02 a sin i = 472. +/- 12. x 10**6 km Light ratio L2/L1 = 0.60 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 4 km/s System2308Orbit1End System1513Orbit2Begin Time span of observations = 4856 days M1 (sin i)**3 = 0.579 +/- 0.026 solar masses M2 (sin i)**3 = 0.467 +/- 0.017 solar masses q = 0.82 +/- 0.02 a sin i = 32.38 +/- 0.43 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 2 km/s System1513Orbit2End System2309Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4866.7 days = 1.2 periods f(M) = 0.0510 +/- 0.0046 solar masses a1 sin i = 274.8 +/- 8.9 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2309Orbit1End System2310Orbit1Begin Preliminary orbit Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 6683.8 days = 1.0 periods f(M) = 0.5 +/- 6.1 solar masses a1 sin i = 840. +/- 3103. x 10**6 km Rotational velocity v sin i = 9 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2310Orbit1End System2311Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5091.0 days = 3.4 periods f(M) = 0.0653 +/- 0.0048 solar masses a1 sin i = 155.3 +/- 4.0 x 10**6 km Rotational velocity v sin i = 4 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2311Orbit1End System1674Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 484.8 days = 2.3 periods f(M) = 0.00531 +/- 0.00053 solar masses a1 sin i = 17.94 +/- 0.61 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1674Orbit2End System1675Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2625.0 days = 29.9 periods f(M) = 0.0314 +/- 0.0028 solar masses a1 sin i = 18.24 +/- 0.54 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1675Orbit2End System2312Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4540.6 days = 1.3 periods f(M) = 0.0904 +/- 0.0047 solar masses a1 sin i = 308.6 +/- 6.1 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2312Orbit1End System2313Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1471.0 days = 8.2 periods f(M) = 0.00778 +/- 0.00093 solar masses a1 sin i = 18.43 +/- 0.74 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2313Orbit1End System2314Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4434.9 days = 24.2 periods f(M) = 0.00145 +/- 0.00020 solar masses a1 sin i = 10.69 +/- 0.48 x 10**6 km Rotational velocity v sin i = 3 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2314Orbit1End System2315Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1218.9 days = 1.9 periods f(M) = 0.00779 +/- 0.00089 solar masses a1 sin i = 43.0 +/- 1.8 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2315Orbit1End System2316Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 4578.7 days = 1.2 periods f(M) = 0.0809 +/- 0.0079 solar masses a1 sin i = 314. +/- 11. x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2316Orbit1End System276Orbit3Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3003.9 days = 66.1 periods f(M) = 0.01013 +/- 0.00051 solar masses a1 sin i = 8.07 +/- 0.14 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System276Orbit3End System1681Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 156.9 days = 18.1 periods f(M) = 0.0311 +/- 0.0011 solar masses a1 sin i = 3.885 +/- 0.047 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1681Orbit2End System1682Orbit2Begin Time span of observations = 1559 days M1 (sin i)**3 = 0.250 +/- 0.012 solar masses M2 (sin i)**3 = 0.2296 +/- 0.0083 solar masses q = 0.92 +/- 0.02 a sin i = 52.01 +/- 0.72 x 10**6 km Light ratio L2/L1 = 0.60 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 6 km/s System1682Orbit2End System1684Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1618.7 days = 19.0 periods f(M) = 0.0943 +/- 0.0036 solar masses a1 sin i = 25.80 +/- 0.33 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1684Orbit2End System2317Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2684.8 days = 1.9 periods f(M) = 0.0809 +/- 0.0050 solar masses a1 sin i = 159.4 +/- 4.1 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2317Orbit1End System2318Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2328.6 days = 169.6 periods f(M) = 0.05873 +/- 0.00089 solar masses a1 sin i = 6.526 +/- 0.033 x 10**6 km Rotational velocity v sin i = 7 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2318Orbit1End System2319Orbit1Begin Time span of observations = 999 days M1 (sin i)**3 = 0.499 +/- 0.070 solar masses M2 (sin i)**3 = 0.351 +/- 0.028 solar masses q = 0.70 +/- 0.05 a sin i = 20.85 +/- 0.80 x 10**6 km Light ratio L2/L1 = 0.15 Rotational velocities: v1 sin i = 6 km/s v2 sin i = 15 km/s System2319Orbit1End System2320Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 3094.8 days = 8.8 periods f(M) = 0.00414 +/- 0.00045 solar masses a1 sin i = 23.46 +/- 0.83 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2320Orbit1End System2321Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2252.0 days = 2.6 periods f(M) = 0.00341 +/- 0.00059 solar masses a1 sin i = 40.4 +/- 2.4 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2321Orbit1End System2322Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1153.9 days = 6.1 periods f(M) = 0.0173 +/- 0.0018 solar masses a1 sin i = 25.09 +/- 0.88 x 10**6 km Rotational velocity v sin i = 5 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2322Orbit1End System2323Orbit1Begin Time span of observations = 4719 days M1 (sin i)**3 = 0.648 +/- 0.061 solar masses M2 (sin i)**3 = 0.567 +/- 0.036 solar masses q = 0.88 +/- 0.04 a sin i = 316.0 +/- 8.3 x 10**6 km Light ratio L2/L1 = 0.30 Rotational velocities: v1 sin i = 0 km/s v2 sin i = 0 km/s System2323Orbit1End System2324Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1281.3 days = 10.6 periods f(M) = 0.000085 +/- 0.000017 solar masses a1 sin i = 3.14 +/- 0.21 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2324Orbit1End System2325Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 771.9 days = 7.3 periods f(M) = 0.0540 +/- 0.0028 solar masses a1 sin i = 24.74 +/- 0.43 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2325Orbit1End System2326Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 5171.8 days = 106.3 periods f(M) = 0.002198 +/- 0.000066 solar masses a1 sin i = 5.073 +/- 0.051 x 10**6 km Rotational velocity v sin i = 0 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2326Orbit1End System2327Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2276.8 days = 9.9 periods f(M) = 0.0115 +/- 0.0016 solar masses a1 sin i = 24.8 +/- 1.2 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2327Orbit1End System2328Orbit1Begin Time span of observations = 4563 days M1 (sin i)**3 = 0.609 +/- 0.039 solar masses M2 (sin i)**3 = 0.547 +/- 0.028 solar masses q = 0.90 +/- 0.03 a sin i = 153.2 +/- 2.8 x 10**6 km Light ratio L2/L1 = 0.60 Rotational velocities: v1 sin i = 4 km/s v2 sin i = 2 km/s System2328Orbit1End System1683Orbit2Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 1586.7 days = 2.8 periods f(M) = 0.0261 +/- 0.0052 solar masses a1 sin i = 58.9 +/- 3.9 x 10**6 km Rotational velocity v sin i = 2 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1683Orbit2End System2329Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 2895.1 days = 7.2 periods f(M) = 0.0053 +/- 0.0025 solar masses a1 sin i = 27.8 +/- 4.4 x 10**6 km Rotational velocity v sin i = 8 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2329Orbit1End System2330Orbit1Begin Telescope flags (tel): W = Wyeth reflector T = Tillinghast reflector M = MMT Time span of observations = 448.7 days = 17.3 periods f(M) = 0.00114 +/- 0.00014 solar masses a1 sin i = 2.68 +/- 0.11 x 10**6 km Rotational velocity v sin i = 1 km/s Radial velocities are on the native CfA system (+0.14 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2330Orbit1End System231Orbit2Begin System231Orbit2End System2331Orbit1Begin System2331Orbit1End System2332Orbit1Begin System2332Orbit1End System2333Orbit1Begin System2333Orbit1End System2334Orbit1Begin System2334Orbit1End System2335Orbit1Begin System2335Orbit1End System2336Orbit1Begin System2336Orbit1End System2337Orbit1Begin System2337Orbit1End System2338Orbit1Begin System2338Orbit1End System2339Orbit1Begin System2339Orbit1End System2340Orbit1Begin System2340Orbit1End System2341Orbit1Begin System2341Orbit1End System2342Orbit1Begin System2342Orbit1End System2343Orbit1Begin System2343Orbit1End System2344Orbit1Begin System2344Orbit1End System2345Orbit1Begin System2345Orbit1End System2346Orbit1Begin System2346Orbit1End System2347Orbit1Begin System2347Orbit1End System2348Orbit1Begin System2348Orbit1End System2349Orbit1Begin System2349Orbit1End System2350Orbit1Begin System2350Orbit1End System2351Orbit1Begin System2351Orbit1End System2352Orbit1Begin System2352Orbit1End System2353Orbit1Begin System2353Orbit1End System2354Orbit1Begin System2354Orbit1End System2355Orbit1Begin System2355Orbit1End System2356Orbit1Begin System2356Orbit1End System2357Orbit1Begin System2357Orbit1End System2358Orbit1Begin System2358Orbit1End System2359Orbit1Begin System2359Orbit1End System2360Orbit1Begin System2360Orbit1End System2361Orbit1Begin System2361Orbit1End System2362Orbit1Begin System2362Orbit1End System2363Orbit1Begin System2363Orbit1End System2364Orbit1Begin System2364Orbit1End System2365Orbit1Begin System2365Orbit1End System2366Orbit1Begin System2366Orbit1End System2367Orbit1Begin System2367Orbit1End System2368Orbit1Begin System2368Orbit1End System265Orbit2Begin System265Orbit2End System2369Orbit1Begin M1 (sin i)**3 = 0.531 +/- 0.011 Msun M2 (sin i)**3 = 0.524 +/- 0.012 Msun q = M2/M1 = 0.987 +/- 0.014 a1 sin i = 12.14 +/- 0.13 x 10**6 km a2 sin i = 12.30 +/- 0.11 x 10**6 km a sin i = 35.12 +/- 0.25 Rsun Rotational velocity of primary = 28 km/s Rotational velocity of secondary = 22 km/s System2369Orbit1End System2370Orbit1Begin MWO = Mt. Wilson Observatory DDO = David Dunlap Observatory KPNO = Kitt Peak National Observatory The period was determined from all the radial velocities, but the other elements were determined only with the KPNO velocities. The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. The primary is a chromospherically active star. The secondary is probably an M dwarf. a1 sin i = 1104000 +/- 6000 km f(m) = 0.0118 +/- 0.002 solar masses System2370Orbit1End System2371Orbit1Begin DDO = David Dunlap Observatory KPNO = Kitt Peak National Observatory The period was determined from all radial velocities, but the other elements were determined only from the KPNO velocities. The velocity of HJD 2445784 was give zero weight because of its 3 sigma residual. Three typographical errors were found in this data set and have been corrected, the velocity residual for HJD 2434111.846 and the velocity and its residual for HJD 2447244.882. The primary is a chromospherically active star. a1 sin i = 5600000 +/- 73000 km f(m) = 0.0202 +/- 0.0008 solar masses System2371Orbit1End System2372Orbit1Begin This system is a chromospherically active binary and a BY Draconis variable. a1 sin i = 5430000 +/- 20000 km a2 sin i = 5450000 +/- 30000 km M1 (sin)3 i = 0.547 +/- 0.005 solar masses M2 (sin)3 i = 0.545 +/- 0.004 solar masses System2372Orbit1End System68Orbit2Begin MO = McDonald Obseratory FO = Fick Observatory KPNO = Kitt Peak National Observatory The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. The primary is a chromospherically active star, while the secondary is a DA white dwarf that was detected at ultraviolet wavelengths by Simon, Fekel, and Gibson (1985, ApJ, 295, 153). a1 sin i = 5570000 +/- 100000 km f(m) = 0.0021 +/- 0.0001 solar masses System68Orbit2End System1164Orbit2Begin MO = McDonald Observatory FO = Fick Observatory KPNO = Kitt Peak National Observaotry The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. As shown in Figure 2 of the paper by Fekel et al., the center of mass velocity listed in Table V should be negative rather positive. In addition, the velocity for JD 2445242 should be positive rather than negative. The primary is a chromospherically active star. a1 sin i = 22620000 +/- 240000 km f(m) = 0.287 +/- 0.009 solar masses System1164Orbit2End System2373Orbit1Begin Chromospherically active binary. The four blended velocities of the primary and secondary have been given zero weight. a1 sin i = 21060000 +/- 80000 km a2 sin i = 23430000 +/- 100000 km m1 sin(3) i = 0.9865 +/- 0.0094 solar masses m2 sin(3) i = 0.8866 +/- 0.0076 solar masses System2373Orbit1End System1092Orbit2Begin Radial velocities in this table are referred to the center of mass of the binary system, with V = -18 km/s. V0_true = -15.7 km/s. Orbital elements are given according Table II from Skul'skii (1993AstL...19..160S) because some errors were made in present paper. Oribital elements of secondary component are following: T0 = 48136.6(+-1.0), V0 = -0.6(+-0.8) km/s, V0_true = -18.6(+-0.8) km/s, e = 0.07(+-0.03), w = 261(+-2) System1092Orbit2End System1092Orbit3Begin Radial velocities in this table are referred to the center of mass of the binary system, with V = -18 km/s. V0_true = -15.8 km/s. Oribital elements of secondary component are following: T0 = 48395.7(+-0.6), V0 = -0.9(+-0.5) km/s, V0_true = -18.9(+-0.5) km/s, e = 0.04(+-0.08), w = 273(+-1) Orbital parameters for both components were calculated from data of the two seasons: 1991 published by Skul'skii (1992SvAL...18..287S) and 1992 (this paper). Orbital elements calculated from data of 1992 only are following: P = 12.9377, T01 = 48743.5(+-0.6), T02 = 48745.1(+-0.6), V01 = 1.0(+-0.7) km/s, V02 = -0.9(+-0.5) km/s, V01_true = -17.0(+-0.7) km/s, V02_true = -18.9(+-0.5) km/s, K1 = 189.7(+-1.0) km/s, K2 = 43.3(+-0.6) km/s, e1 = 0.02(+-0.01), e2 = 0.04(+-0.09), w1 = 54(+-1), w2 = 277(+-1), rms1 = 0.73, rms2 = 0.49 System1092Orbit3End System2374Orbit1Begin Authors have combined their observations with observations of Campbell (1928) and Frost et al. (1926). Every coathors used differnt telescope and spectrometer , but the velocity offset found for each data set is 1 km/s or less. System2374Orbit1End System2375Orbit1Begin In the paper T0 = 51000.066 : it is a time when observed velocity equals systemic velocity. System2375Orbit1End System2376Orbit1Begin The parameters of a circular orbit fit to the radial velocities measured from both spectral lines: H_alpha and He I 6678. In the paper T0 = 51240.855 : it is a time when observed velocity equals systemic velocity. System2376Orbit1End System2377Orbit1Begin Authors measured radial velocities from 49 spectra of H_alpha line. They did not publish these velocities. V0 measured for the second component equals to -1.4 km/s. T0 is a time when the observed velocity equals systemic velocity. System2377Orbit1End System2378Orbit1Begin The value of P was taken from Billeres et al. (2000, ApJ 530, 441) The time T0 corresponds to the point in the orbit when the sdB star (a visible companion) is closest to the observer. The value of V0 =-13.9 is obtained from H_alpha line, there is another value of V0 = -12.2 (with err 3.7) obtained from HeI 6678 line. Authors measured radial velocities from 25 spectra obtained. They did not publish these velocities. System2378Orbit1End System2379Orbit1Begin P, e and w were taken from Lacy (1993, AJ 105, 637). V0 measured for the second component equals to -23.7 km/s with the error of 1.9 km/s. System2379Orbit1End System2380Orbit1Begin P, e and w were taken from Lacy (1993, AJ, 105, 1096). V0 of secondary component equals to -10.6 km/s with the error of 1.6 km/s. System2380Orbit1End System1955Orbit3Begin V0 measured for the second component equals to -15.8 km/s with the error of 0.5 km/s. Author did not publish the value of T0. System1955Orbit3End System436Orbit2Begin T, w, e were adopted from the photometric solution. V0 measured for the second component equals to 44.9 km/s with the error of 0.6 km/s P was taken from Ziegler (1965, Mitt. Ver. Sterne, 2, 185) System436Orbit2End System2381Orbit1Begin V0 measured for the second component equals to -25.4 km/s with the error of 0.7 km/s P was taken from Gulmen et al.(1988, AApS 73, 255) Author assumed that the third component exist from analysis of photometric observations. System2381Orbit1End System2382Orbit1Begin Authors measured radial velocities using 103 spectrograms; they did not publish these velocities. In the paper w equals to -0.066 rad. T0 is the time when the observed velocity equals to the systemic velocity. System2382Orbit1End System2383Orbit1Begin System2383Orbit1End System1402Orbit2Begin Crimea means that the observations have been made at 2.6 m telescope of the Crimean Astrophysical Observatory. SOFIN means that the observations have been made with the SOFIN echelle spectrograph at 2.56 m Nordic Optical Telescope, La Palma In the paper T0=50342.883 corresponds to the conjuction with the primary in the back. System1402Orbit2End System2384Orbit1Begin T, e, w were taken from the photometric orbit. P was taken from ephemeris curve solution. The value of V0 for the secondary component is -15.0+- 1.0 km/s. System2384Orbit1End System2385Orbit1Begin From analysis of the H_alpha line profiles, authors find antiphased radial velocity variations of the emission component and the photospheric absorption. They asssumed that absortion-line spectrum is associated with a more massive primary, while the travelling emission component originates in a region around a less massive secondary. Orbital elements derived for secondary component are following: V0=-1.6+-0.1 km/s; P=84.135+-0.004. System2385Orbit1End System4Orbit3Begin Orbital elements were calculated by combining measurements from this paper with those from Abt & Snowden (1973, ApJS 25, 137), Aikman (1976, Publ. Dominion Astrophys. Obs. 14, 379), and Tomkin et al. (1995, AJ 109, 780). The authors weighted 53 their values according to estimated uncertaintes for the primary (2 km/s) and the secondary (5 km/s). System4Orbit3End System155Orbit2Begin Radial-velocity curves were constructed from 52 spectrograms. Author did not published the values of Vr. The orbital elements were calculated in two models: a circular orbit and an elliptical orbit. There are another set of elements of primary component derived from FeI (V0=-10.0 km/s; K=29.5 km/s) and from Ca, Sc, Cr (V0=-2.2 km/s; K=31.5 km/s) separately. V0 derived for secondary component is -5.7+-0.3 km/s. System155Orbit2End System155Orbit3Begin Radial-velocity curves were constructed from 52 spectrograms. Author did not published the values of Vr. The orbital elements were calculated in two models: a circular orbit and an elliptical orbit. There are another set of elements of primary component derived from FeI (V0=-7.7 km/s; K=29.8 km/s; e=0.191; w=179.1) and from Ca, Sc, Cr (V0=-0.2 km/s; K=33.1 km/s; e=0.155; w=57.2) separately. Orbital elements derived for secondary component are following: V0=-6.0+-0.3 km/s; e=0.097+-0.02; w=260.1+-2.5. The high eccentricity of primary's orbit is the result of the absence of observations near phi_orb=0.9 to 0.0. System155Orbit3End System1921Orbit1Begin The system is a visual binary, and its primary star is a chromospherically active, single-lined binary, making the system triple. The unseen secondary of the short-period binary is likely an M dwarf, while the visual binary secondary is probably a K3 dwarf. a1 sin i = 4356000 +/- 15000 km f(m) = 0.01018 +/- 0.00011 solar masses System1921Orbit1End System811Orbit2Begin No RV published. System811Orbit2End System856Orbit2Begin System856Orbit2End System2386Orbit1Begin System2386Orbit1End System2387Orbit1Begin System2387Orbit1End System2060Orbit2Begin M1 (sin i)**3 = 2.481 +/- 0.023 Msun M2 (sin i)**3 = 0.515 +/- 0.011 Msun q = M2/M1 = 0.2076 +/- 0.0032 a1 sin i = 5.148 +/- 0.079 x 10**6 km a2 sin i = 24.799 +/- 0.079 x 10**6 km a sin i = 43.03 +/- 0.15 Rsun Orbit and radial velocities superseded by results in 2003AJ....125.3237T. System2060Orbit2End System2060Orbit3Begin M1 (sin i)**3 = 2.486 +/- 0.028 Msun M2 (sin i)**3 = 0.516 +/- 0.010 Msun q = M2/M1 = 0.2076 +/- 0.0031 a1 sin i = 5.151 +/- 0.074 x 10**6 km a2 sin i = 24.814 +/- 0.094 x 10**6 km a sin i = 43.05 +/- 0.17 Rsun Due to an oversight the elements and derived quantities reported for the circular orbit in the original publication (Table 2, last column) are incorrect, and should be replaced by these. Orbit and radial velocities superseded by results in 2003AJ....125.3237T. System2060Orbit3End System2388Orbit1Begin Orbital parameters for the absorption lines. NV emission line gives K = 157 km/s and V0 = 219 ks/sec with considerably larger scatter. System2388Orbit1End System2389Orbit1Begin Calculations based in 73 photographic spectrograms. Orbital elements are for HeI 3888 absorption. CIV and NV emissions give smaller velocity amplitudes with larger scatter and systemic velocities of 65 and 135 km/s, respectively. Longer periods of 55 and 64 days are also possible, giving eccentric orbits. System2389Orbit1End System2390Orbit1Begin Circular elements for CIII-IV emission lines. HeII, NV and NIV emissions give slightly different solutions. System2390Orbit1End System476Orbit3Begin Primary elements from HeII absorption lines; secondary from OIV emission. Minimum masses of 7 and 5 solar masses, respectively. Systemic velocity of OIV emission is -371 km/s. System476Orbit3End System2391Orbit1Begin Primary elements from absorption line spectrum; secondary from NV 4603-19 emission (systemic velocity 9 km/s). Minimum masses of 4 and 2 solar masses, respectively. Orbital parameters for HeII emission similar to those of NV. System2391Orbit1End System2392Orbit1Begin Orbital elements for HeII 4686 emission. NV 4603-19 emission gives larger semiamplitude (320 km/s) and different systemic velocity (204 km/s). System2392Orbit1End System2393Orbit1Begin Orbital parameters for NIV 4058 emission. O-C values are given as errors. T is the time of conjunction with the WR star in front of the system. Minimum masses derived from this solution and the O-type absorptions are 36 and 26 solar masses, respectively. System2393Orbit1End System2393Orbit2Begin Orbital parameters for the NIV 5203 absorption line. O-C values from the orbital fit given as errors. T is the time of conjunction with the WR star in front of the system. Minimum masses derived from this solution and the O-type absorptions are 40 and 33 solar masses, respectively. System2393Orbit2End System2393Orbit3Begin Orbital parameters for the HeII 4686 emission line. O-C values from the orbital fit given as errors. T is the time of conjunction with the WR star in front of the system. Minimum masses derived from this solution and the O-type absorptions are 28 and 14 solar masses, respectively. System2393Orbit3End System2393Orbit4Begin Orbital parameters for the NV 4604 PCyg absorption. O-C values from the orbital fit given as errors. T is the time of conjunction with the WR star in front of the system. Minimum masses derived from this solution and the O-type absorptions are 34 and 44 solar masses, respectively. System2393Orbit4End System2393Orbit5Begin Orbital parameters for the average of the O-type Hydrogen absorption lines. O-C values from the orbital fit given as errors. T is the time of conjunction with the WR star in front of the system. System2393Orbit5End System2394Orbit1Begin Radial velocities and orbital parameters for the NIV 4058 emission line. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. System2394Orbit1End System2394Orbit2Begin Radial velocities and orbital parameters for the NV 4604 absorption line. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. System2394Orbit2End System2394Orbit3Begin Radial velocities and orbital parameters for the average of H absorption lines. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. System2394Orbit3End System2394Orbit4Begin Radial velocities and orbital parameters for the HeII 4686 emission line. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. System2394Orbit4End System2394Orbit5Begin Radial velocities and orbital parameters for the average of HeII absorption lines. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. System2394Orbit5End System2461Orbit1Begin Radial velocities and orbital parameters for the average of HeI absorption lines probably originated in a close visual companion, also of binary nature. T is the time of passage through the systemic velocity V0 from positive to negative radial velocity. Multiple system with at least four stars. SB9 note: Typo corrected in K1. System2461Orbit1End System2395Orbit1Begin Radial velocities and orbital parameters for the HeII 4686 emission line. A phase lag of approximately 1 day is observed between this radial velocity orbit and that derived from the average of the O6 component absorptions. System2395Orbit1End System2395Orbit2Begin Radial velocities and orbital parameters for the average of the He absorpion lines in the O6 spectrum. A phase lag of approximately 1 day is observed between this radial velocity orbit and that derived from the HeII 4686 WN emission. System2395Orbit2End System801Orbit2Begin The period and epoch are adopted from Andersen et al. (1984) [1984A&A...137..281A], and are based on eclipse timings. M1 (sin i)**3 = 1.454 +/- 0.008 Msun M2 (sin i)**3 = 1.448 +/- 0.008 Msun q = M2/M1 = 0.9955 +/- 0.0035 a sin i = 16.763 +/- 0.029 Rsun System801Orbit2End System987Orbit2Begin T is the time of maximum radial velocity. O-C values from the orbital fit are given as radial velocity errors. Orbital solution coincident with previous determinations by Abt et al.(1972ApJ...171..259A) and Crampton et al. (1976ApJ...204..502C). System987Orbit2End System2396Orbit1Begin O-C values from the orbital fit are given as radial velocity errors. System2396Orbit1End System989Orbit2Begin O-C values from the orbital fit are given as radial velocity errors. SB9 comment: omega should be read 164 instead of 16 as in the paper. System989Orbit2End System2397Orbit1Begin O-C values from the orbital fit are given as radial velocity errors. System2397Orbit1End System2398Orbit1Begin O-C values from the orbital fit are given as radial velocity errors. SB9 comment: T0 was changed in order to match the observations System2398Orbit1End System170Orbit2Begin O-C values from the orbital fit are given as radial velocity errors. System170Orbit2End System2399Orbit1Begin SB9 comment: T0 was changed in order to match the observations. System2399Orbit1End System2400Orbit1Begin O-C values from the orbital fit given as errors. System2400Orbit1End System2401Orbit1Begin O-C from the orbital fit given as errors. System2401Orbit1End System2402Orbit1Begin O-C from orbital fit given as errors. System2402Orbit1End System2200Orbit2Begin System2200Orbit2End System760Orbit3Begin System760Orbit3End System882Orbit2Begin System882Orbit2End System180Orbit3Begin H56 = Heard 1956, PDDO, 2, 107 C79 = Carquillat, Nadal, Ginestet, & Pedoussaut 1979, A&A, 74, 113 SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. Element uncertainties listed in the original paper for this system are roughly a factor of 5 too large. Correct uncertainties are now listed. The primary is a G2 V chromospherically active star. Stockton and Fekel estimated a spectral type of about K5 V for the secondary from the mass of the primary and the mass ratio. They also determined vsini = 31 km/s for the primary. System180Orbit3End System275Orbit2Begin SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 Harper's (1932, PDAO, 7, 1) earlier radial velocities were used only to improve the orbital period. The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. The primary is an Am star. Abt and Morrell (1995, ApJS, 135, 172) classified it as A7/F0/F2 based on its Ca II K line, hydrogen lines, and metal lines, respectively. Stockton and Fekel have estimated a spectral type of about F6 V for the secondary from the expected mass of the primary and the mass ratio. They also determined vsini = 10 km/s for the primary. System275Orbit2End System368Orbit2Begin SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 The radial velocities of Abt and Levy (1985, ApJS, 59, 232) were used only to improve the orbital period. The primary is an Am star. Abt and Morrell (1995, ApJS, 135, 172) classified it as A4/A5/A7 based on its Ca II K line, hydrogen lines, and metal lines, respectively. Stockton and Fekel have estimated a spectral type of about F1 V for the secondary from the expected mass of the primary and the mass ratio. The vsini value of 48 km/s given by Abt and Morrell is much larger than the value of 9 km/s determined by Stockton and Fekel. System368Orbit2End System1075Orbit2Begin SB85 = Salzer & Beavers 1985, PASP, 97, 637 Aetal85 = Andersen et al. 1985, A&A, 59, 15 SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 Element uncertainties listed in the original paper for this system are roughly a factor of 4 too large. Correct uncertainties are now listed. The vsini of the primary is 8 km/s System1075Orbit2End System1299Orbit2Begin P22 = Plaskett 1922, PDAO, 1, 113 MM87 = Mayor & Mazeh 1987, A&A, 171, 157 BE86 = Beavers & Eitter 1986, ApJS, 62, 147 SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. Element uncertainties listed in the original paper for this system are roughly a factor of 2 too large. Correct uncertainties are now listed. The primary is an F8 V chromospherically active binary. Stockton and Fekel estimated a spectral type of about K6 V for the secondary from the mass of the primary and the mass ratio. They also determined vsini = 15 km/s for the primary. System1299Orbit2End System1453Orbit2Begin H56 = Heard 1956 PDDO, 2, 107 I69 = Imbert 1969, A&A, 3, 272 BE86 = Beavers & Eitter 1986, ApJS, 62, 147 SF92 = This paper = Stockton & Fekel 1992, MNRAS, 256, 575 The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. Element uncertainties listed in the original paper for this system are roughly a factor of 4 too large. Correct uncertainties are now listed. The primary is a G5 V chromospherically active binary. Stockton and Fekel estimated a spectral type of about K6 V for the secondary from the mass of the primary and the mass ratio. They also determined vsini = 8 km/s for the primary. System1453Orbit2End System75Orbit2Begin Wright and Pugh (1954, Publ. Dom. Astrophys. Obs. 9, 407) got P = 5.42906. System75Orbit2End System87Orbit2Begin K variations have been detected relative to Sanford's (1921, ApJ 53, 201) elements. The system has a faint companion. System87Orbit2End System228Orbit2Begin Comparison with Lucy and Sweeney (1971, AJ 76, 544) work indicates a possible K1 variation. System228Orbit2End System236Orbit2Begin The value for the period was derived by combining the authors' elements with T0 of Northcott and Wright (1952, J. Roy. Astron. Soc. Canada 46, 11). System236Orbit2End System392Orbit2Begin The authors derived the value for the period P by combining their elements with T0 of Lucy and Sweeney (1971, AJ 76, 544), based on Harper's (1925, Publ. Dom. Astrophys. Obs. 3, 189) measurements. System392Orbit2End System585Orbit2Begin The authors got e = 0.002 +-0.005 and adopted a circular orbit. According to detection of K variation the presence of third component is possible. System585Orbit2End System647Orbit2Begin HD 95638 is a member of the quadruple system. Petrie (1959, Publ. Dom. Astrophys. Obs. 6, 365) got e=0.087+-0.027. The authors got e=-0.004+-0.011 and adopted a circular orbit. The old orbit elements were recalculated using Petrie's measurements, assuming e=0. Then the value for the period P was calculated by combining derived T0 for the 1959 epoch and the authors' elements. System647Orbit2End System675Orbit2Begin This is a spectroscopically triple system. Comparison with the measurements of Petrie and Laidler (1952, Publ. Dom. Astrophys. Obs. 9, 181) indicates possible K and e variations. System675Orbit2End System721Orbit2Begin The value for the period was derived by combining the authors' elements and Sanford's observations (1924, ApJ 59, 356). T0 was recalculated by authors for his radial velocities assuming e=0. System721Orbit2End System27Orbit2Begin VRcorr means that observed radial velocities have been corrected of the V0 variations to allow the determination of orbital elements at the epoch T0. System27Orbit2End System730Orbit2Begin Comparision with Petrie's work (1937, Publ. Dom. Astrophys. Obs. 6, 365) indicates a possible K variation. The eccentricity has been changed as Petrie got e = 0.213+-0.016. System730Orbit2End System737Orbit2Begin McKellar and Reeves (1953 Publ. Dom. Astrophys. Obs. 9, 399) got e = 0.034 +- 0.008. The authors recalculated T0 for radial velocities of McKellar and Reeves assuming e = 0. Then the value for the period P was calculated by combining derived T0 and the authors' elements. System737Orbit2End System773Orbit2Begin The value for the period was derived by using also T0 of Lucy and Sweeney (1971, AJ 76, 544) which is based on Harper's (1938, Publ. Dom. Astrophys. Obs. 7, 141) observations. System773Orbit2End System805Orbit2Begin The value for the period was derived by using also Duncan's (1921, ApJ 54, 226) T0. System805Orbit2End System821Orbit2Begin The value for the period was derived by using also Heard's (1966, J. Roy. Astron. Soc. Canada 60, 128) T0. The authors suggest that V0 velocity is changing, so HD 131861 is probably a spectroscopic triple system. The given V0 is for JD = 2444500. VRcorr means that the observed radial velocities have been corrected of the V0 variation to allow the determination of orbital elements at the epoch T0. System821Orbit2End System829Orbit2Begin K variation has been detected. There are two measurements of the faint visual component (HD 134646 B): JD Vr Err 45433.630 -1.71 0.57 45436.578 -1.95 0.51 System829Orbit2End System882Orbit3Begin K variation has been detected. System882Orbit3End System885Orbit2Begin K variation has been detected. The authors suggest that HD 144515 includes two close spectroscopic binaries: HD 144515A with a period of about 4 days and the new HD 144515B (see SB9) with a period of about 11 days. They are physically connected as their V0 velocity differs by about 1 km/s. System885Orbit2End System2403Orbit1Begin The authors suggest that HD 144515 includes two close spectroscopic binaries: HD 144515A with a period of about 4 days (see SB9) and the new HD 144515B with a period of about 11 days. They are physically connected as their V0 velocity differs by about 1 km/s. System2403Orbit1End System916Orbit2Begin The value of P was derived by combining T0 of Sanford (1926, ApJ 64, 172) with the authors' elements. System916Orbit2End System981Orbit2Begin The value of P was derived by combining the authors' elements with T0 of Luyten (1936, ApJ 84, 85), based on Turner's (1907, Lick Obs. Bull. 4, 163) observations. System981Orbit2End System1126Orbit2Begin The value of P was derived by combining the authors' elements with T0 of Harper (1925, Publ. Dom. Astrophys. Obs. 3, 189). System1126Orbit2End System1141Orbit2Begin The value of P was derived by combining the authors' elements with T0 of Lucy and Sweeney (1971, AJ 76, 544), based on Northcott's (1947, Pub. David Dunlop Obs. 1, 369) observations. System1141Orbit2End System1299Orbit3Begin The value of P was derived by combining the authors' results with T0 of Lucy and Sweeney (1971, AJ 76, 544), based on Plaskett's (1919 Pub. Dom. Astrophys. Obs 1, 113) observations. System1299Orbit3End System1329Orbit2Begin V0 was found to vary. The value of V0 is given for T0. VRcorr means that the observed radial velocities have been corrected of the V0 variation to allow the determination of orbital elements at the epoch T0. System1329Orbit2End System1336Orbit2Begin The value of P was derived by using the value of Lucy and Sweeney (1971, AJ 76, 544) for T0, based on observations of McKellar and Patten (1940, Publ. Dom. Astrophys. Obs. 7, 239). System1336Orbit2End System497Orbit2Begin SZ Lyncis is an ultrashort-period, 0.12 day, pulsating variable. The authors measured 69 radial velocities; then they used velocity curves from Bardin and Imbert (1981, AAp 98, 198 ) as master curves to determine the mean velocities for seven epochs. To determine the orbital elements authors used the photometric and spectroscopic data in a combined iterative solution. System497Orbit2End System1454Orbit2Begin The giant primary star in the system is a Mira variable. The value of period, 44 years, was assumed and fixed; T0 and w were fixed in calculation. To calculate orbital elements authors used their observations and thirteen previously published velocities from Merrill (1950, ApJ 112, 314 ), Jacobsen and Wallerstein (1975, PASP 87, 269), Wallerstein (1986, PASP 92, 275 ). System1454Orbit2End System389Orbit2Begin Radial-velocity measurements were made with cross-correlation techniques or by manually measuring individual line shifts ("line by line") System389Orbit2End System2404Orbit1Begin Radial-velocity measurements were made with cross-correlation techniques or by manually measuring individual line shifts ("line by line") The eccentricity was found to be within two standart deviations of zero and was taken to be zero. System2404Orbit1End System2405Orbit1Begin Authors used following published data to calculate orbital elements: Fekel et al. (1986, ApJS 60, 551), Balona (1987, SAAO Circ. 11, 1), Bopp (1983, private comm.). Authors assumed the value of "e" to be equal zero. T0 and w were taken from Balona (1987). System2405Orbit1End System410Orbit3Begin The radial velocities were measured at the McDonald Observatory (McDonald) with the 2.7 m or 2.1 m telescope and coude spectrograph, or at the Kitt Peak National Observatory (KPNO) with a coude feed telescope. Authors also made a combined solution with their data and velocities measured at the David Dunlap Observatory and Lick Observatory (Kamper and Beardsley 1987, AJ 94, 1302). Orbital elements are following: P = 4614.0 +- 0.7; T0 = 39382.7 +- 1.6; V0 = -12.23 +- 0.08 km/s; e = 0.893 +- 0.002; w = 312.6 +- 0.9; K1 = 12.1 +- 0.1 km/s. System410Orbit3End System248Orbit2Begin McD means that the observations were made on a 2.7 m telescope at McDonald Observatory. All other observations were made on a 1.5 m telescope at Palomar Observatory. The preliminary period was determined from solution of primary velocities from this paper and the published primary velocities combined. This period was then fixed in the solution for orbital elements. K2 must be regarded as provisional, not final, because of possible underestimation of the real error in K2. System248Orbit2End System4Orbit4Begin The preliminary period was determined from solution of primary velocities from this paper and the published primary velocities combined. This period was then fixed in the solution for orbital elements. K2 must be regarded as provisional, not final, because of possible underestimation of the real error in K2. Orbital elements obtained by using secondary velocities only are following: V0 = -9.2(+-3.9) km/s, K2 = 66.5(+-3.9) km/s. System4Orbit4End System2308Orbit2Begin System2308Orbit2End System675Orbit3Begin This is a spectroscopically triple system. Comment column contains the radial velocities of the tertiary. System675Orbit3End System2406Orbit1Begin This IAU radial velocity standard star is a spectroscopic binary with a low-mass companion. System2406Orbit1End System1537Orbit2Begin This IAU radial velocity standard star is a spectroscopic binary with a low-mass companion. System1537Orbit2End System2407Orbit1Begin This is IAU radial velocity standard star. Authors consider their orbital solution to be preliminary. System2407Orbit1End System680Orbit2Begin To calculate the orbital elements authors combined 3 new velocities with 29 old primary velocities published by Duquennoy et al. (1991, AApS 88, 281). System680Orbit2End System2213Orbit2Begin To calculate the orbital elements authors combined 3 new velocities with 35 old primary velocities published by Mayor and Turon (1982, AAp 110, 241). System2213Orbit2End System1863Orbit2Begin The relative orbital elements were calculated via a simultaneous fit to the relative astrometric and primary radial velocity data. The authors did not publish the radial velocity data. System1863Orbit2End System2200Orbit3Begin Authors combined the new radial velocities of the primary and the secondary with the primary measurements published by Latham et al. (2002, AJ 124, 1144) to solve the orbital parameters. They did not publish the radial velocity data. System2200Orbit3End System760Orbit4Begin Authors combined the new radial velocities of the primary and the secondary with the primary measurements published by Latham et al. (2002, AJ 124, 1144) to solve the orbital parameters. They did not publish the radial velocity data. System760Orbit4End System882Orbit4Begin Authors combined the new radial velocities of the primary and the secondary with the primary measurements published by Duquennoy and Mayor (1991, AAp 248, 485) to solve the orbital parameters. They did not publish the radial velocity data. System882Orbit4End System2179Orbit2Begin Authors combined the new radial velocities of the primary and the secondary with the primary measurements published by Duquennoy and Mayor (1991, AAp 248, 485) to solve the orbital parameters. They did not publish the radial velocity data. Authors consider their results to be preliminary. System2179Orbit2End System1419Orbit2Begin The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values, but are best taken as relative. The value of eccentricity was fixed. There are the separate single-component solutions. For primary: P=2.7290(fixed), T0=48603.566(+-0.004), e=0.0293(fixed), w= 351.0(fixed), K1=210.7(+-1.3) km/s, V0=-2.9(+-1.1) km/s, rms1=4.4 km/s For secondary: P=2.7290(fixed), T0=48603.562(+-0.003), e=0.0293(fixed), w=171.0(fixed), K2=230.8(+-1.2) km/s, V0=-4.5(+-1.1) km/s, rms2=4.0 km/s System1419Orbit2End System922Orbit2Begin There is a separate solution for the primary star alone: P=1.446262(+-0.000011), T0=48102.622(+-0.119), e=0.037(+-0.015), w=151.4(+-29.1), K1=158.2(+-2.2) km/s, V0=-8.1(+-1.9) km/s, rms1=6.0 km/s The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values, but are best taken as relative. System922Orbit2End System832Orbit2Begin There is a separate solution for the primary star alone: P=3.902456(fixed), T0=48883.874(+-0.058), e=0.063(+-0.004), w=237.2(+-5.1), K1=147.8(+-0.7) km/s, V0=-15.5(+-0.5) km/s, rms1=2.3 km/s The radial velocities were taken from the archive of IUE observations. The velocities are relative but the zero point has been adjusted to bring them close to absolute values. System832Orbit2End System325Orbit2Begin There are the separate solutions. For primary: P=4.002439(fixed), T0=49302.832(+-0.012), K1=154.6(+-2.1) km/s, V0=4.9(+-1.4) km/s, rms1=7.1 km/s For secondary: P=4.002439(fixed), T0=49300.789(+-0.008), K2=289.7(+-2.3) km/s, V0=4.9(+-1.6) km/s, rms2=7.2 km/s The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values, but are best taken as relative. System325Orbit2End System662Orbit2Begin There are the separate single-component solutions. For primary: P=3.4142765(fixed), T0=48259.329(+-0.006), K1=232.7(+-1.9) km/s, V0=-12.1(+-1.5) km/s, rms1=4.8 km/s For secondary: P=3.4142765(fixed), T0=48261.043(+-0.005), K2=256.5(+-1.8) km/s, V0=-10.2(+-1.4) km/s, rms2=4.6 km/s The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values. System662Orbit2End System552Orbit2Begin The value of K2 was adopted. There is the solution in which P, e, w, and T0 have been set at the values obtained from the X-ray timing analysis (Deeter et al. 1987, ApJ 314, 634) P=8.964353(fixed), T0=43957.89(fixed), e=0.090(fixed), w= 332.8(fixed), K1=17.1(+-1.5) km/s, V0=-3.4(+-1.0) km/s, rms1=6.6 km/s There is the solution of using velocities measured when the small-aperture spectrum of the standard was employed. P=8.964353(fixed), T0=43957.89(fixed), e=0.090(fixed), w=332.8(fixed), K1=18.7(+-1.9) km/s, V0=0.5(+-1.2) km/s, rms1=8.3 km/s The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values. System552Orbit2End System1321Orbit3Begin HD 206267 A is a spectroscopic triple system. Measurements of the very weak secondary are not certain enough to be used in the determination of the orbital elements. The radial velocities were taken from the archive of IUE observations. System1321Orbit3End System932Orbit2Begin The radial velocities were taken from the archive of IUE observations. The zero-point of radial velocities is arbitrary, but approximately equal to zero. These radial velocites have been used also to solve for the elements of a circular orbit: P=7.84826(fixed); T0=43874.768(+-0.047); K1=77.1(+-3.4) km/s; V0=-40.5(+-2.2) km/s System932Orbit2End System943Orbit2Begin The radial velocities were taken from the archive of IUE observations. In the orbital elements derived by authors V0 is "arbitrary". The radial velocites for 1985 only have been used to solve for the elements of a circular orbit: P=3.4118(fixed); T0=46165.438(+-0.023); K1=5.05(+-0.25) km/s; V0=arbitrary System943Orbit2End System634Orbit5Begin The radial velocities were taken from the archive of IUE observations. The secondary velocities have been given weights of 0.4 for those data close to periastron, 0.2 for those around phase 0.3, and 0.1 for those close to phase 0.7, while all of the primary data have been given weights of 1.0. There is a separate solution for the primary star alone: P=6.08209(+-0.00038), T0=44113.817(+-0.026), e=0.46(+-0.02), w=15.4(+-2.1), K1=144.5(+-3.3) km/s, V0=28.8(+-1.8) km/s, rms1=6.5 km/s System634Orbit5End System331Orbit2Begin The radial velocities were taken from the archive of IUE observations. They all have been adjusted to the adopted systemic velocity, V0, taken from Curtiss R.H. (1914, Publ. Michigan Obs. 1, 118) The authors also analysed all published data and calculated the following orbital elements: P=5.732824(+-0.000050), T0=30802.02(+-0.09), K1=97.9(+-0.9) km/s, e=0.087(+-0.009), w=49.9(+-5.5), V0=20.3(adopted) km/s System331Orbit2End System354Orbit2Begin Since even at the higher dispersions and at times of maximum or minimum velocity, signatures of the secondary component were not obvious, the lines were measured as though they were single using parabola fitting. To improve the data set the authors used four lines only in final solution that appeared to behave well consistently: HI at 4101 A and 4340 A, He I at 4388 A and 4471 A. All available archival material has also been reexaminated. System354Orbit2End System2408Orbit1Begin The comment means: NSO - the observations were obtained at National Solar Observatory; KPNO - the observations were obtained at Kitt Peak National Observatory; Fleming - the observations were taken from Fleming et al. (1989AJ.....98..692F); Latham -the observations were taken from Latham et al. (1988AJ.....96..567L) This is the spectroscopic triple star with two (short and long) periods and orbits. The standard error of an observation of unit weight is 1.0 km/s. System2408Orbit1End System2409Orbit1Begin The comment means: NSO - the observations were obtained at National Solar Observatory; KPNO - the observations were obtained at Kitt Peak National Observatory; Fleming - the observations were taken from Fleming et al. (1989AJ.....98..692F); Latham -the observations were taken from Latham et al. (1988AJ.....96..567L). This is the spectroscopic triple star with two (short and long) periods and orbits. The standard error of an observation of unit weight is 1.0 km/s. A time of conjunction with the primary behind the secondary is HJD 2446348.080. System2409Orbit1End System45Orbit2Begin The comment means: NSO - the observations were obtained at National Solar Observatory; KT2 - the observations were obtained at Kitt Peak National Observatory. The standard error of an observation of unit weight is 0.6 km/s. System45Orbit2End System2410Orbit1Begin The comment means: KT2 - the observations were obtained at Kitt Peak National Observatory using 800x800 TI CCD; KF - the observations were obtained at Kitt Peak National Observatory using 3096x1024 F3KB CCD. The standard error of an observation of unit weight is 0.15 km/s. A time of conjunction with the primary behind the secondary is HJD 2449311.371. System2410Orbit1End System569Orbit2Begin The comment means: NSO - the observations were obtained at National Solar Observatory; KR, KT2, KFA - the observations were obtained at Kitt Peak National Observatory using different detectors; MR - the observations were obtained at McDonald Observatory of the University of Texas; Dadonas - the observations were taken from Dadonas (1994, private comm.); Donati -the observations were taken from Donati et al. (1997MNRAS.291..658D). The standard error of an observation of unit weight for the primary is 0.7 km/s. System569Orbit2End System2411Orbit1Begin The comment means: KFA, KF, KR, KT1, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; NSO - the observations were obtained at National Solar Observatory; MR - the observations were obtained at McDonald Observatory of the University of Texas. This is the spectroscopic triple star with two (short and long) periods and orbits, but only one component shows both long- and short-period orbital motion. The standard error of an observation of unit weight is 1.3 km/s. System2411Orbit1End System2412Orbit1Begin The comment means: KFA, KF, KR, KT1, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; NSO - the observations were obtained at National Solar Observatory; MR - the observations were obtained at McDonald Observatory of the University of Texas. This is the spectroscopic triple star with two (short and long) periods and orbits, but only one component shows both long- and short-period orbital motion. The standard error of an observation of unit weight is 1.3 km/s. A time of conjunction in the short-period orbit with the primary behind the secondary is HJD 2450195.909. System2412Orbit1End System2371Orbit2Begin The comment means: KF, KT1, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; NSO - the observations were obtained at National Solar Observatory. Authors combined 18 new velocities with those published by Fekel et al. (1989, AJ 97, 202) The standard error of an observation of unit weight is 1.2 km/s. A time of conjunction with the primary behind the secondary is HD 2447312.447. System2371Orbit2End System848Orbit2Begin The comment means: KF, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; ESO - the observations were obtained at European Southern Observatory, La Silla The period was fixed from circular solution received using new observations and data from the literature. The standard error of an observation of unit weight is 3.0 km/s. System848Orbit2End System2413Orbit1Begin The comment means: KF, KT1, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; ESO - the observations were obtained at European Southern Observatory, La Silla The standard error of an observation of unit weight is 0.6 km/s. A time of conjunction with the primary behind the secondary is HD 2448226.377. System2413Orbit1End System2414Orbit1Begin The comment means: KF, KT2 - the observations were obtained at Kitt Peak National Observatory using different detectors; NSO - the observations were obtained at National Solar Observatory. The standard error of an observation of unit weight is 0.6 km/s. System2414Orbit1End System1402Orbit3Begin The comment means: NSO - the observations were obtained at National Solar Observatory; Harper - the observations were taken from Harper (1920, Publ. Dominion Astroph. Obs. 1, 203) and Harper (1935, Publ. Dominion Astroph. Obs. 6, 207); Olah - the observations were taken from Olah et al. (1998, A&Ap 330,559). The standard error of an observation of unit weight is 0.9 km/s. System1402Orbit3End System500Orbit2Begin The radial velocities were taken from the archive of IUE observations. All velocities were adjusted to give adopted systemic velosity of -18 km/s. There are the separate single-component solutions. The period has been fixed at 78.519 for all solutions. a) For O9I star using six lines:T=43606.7(+-4.9), e=0.29(+-0.10), w=258(+-23), V0=-11.0(+-13.1) km/s, K=42.9(+-4.7) km/s, rms=17.0 km/s b) For O9I star using two NIII lines:T=43599.3(+-3.1), e=0.50(+-0.16), w=235(+-23), V0=-18.0(+-4.3) km/s, K=37.1(+-6.6) km/s, rms=22.8 km/s c) For WR star using ten lines:T=43597.6(+-0.8), e=0.59(+-0.03), w=43(+-7), V0=-18.0(fixed) km/s, K=121.1(+-5.5) km/s, rms=20.1 km/s System500Orbit2End System1266Orbit3Begin The radial velocities were taken from the archive of IUE observations. The measured velocities are close to absolute values, probably to an accuracy of about 2 km/s. There are the separate single-component solutions. For primary: P=2.9963(fixed), T0=48040.665(+-0.062), e=0.072(+-0.009), w=146.6(+-7.9), K1=237.8(+-1.8) km/s, V0=-70.2(+-1.4) km/s, rms1=4.2 km/s For secondary: P=2.9963(fixed), T0=48040.904(+-0.035), e=0.129(+-0.009) w=356.6(+-4.8), K2=233.7(+-2.0) km/s, V0=-61.9(+-1.4) km/s, rms2=4.4 km/s System1266Orbit3End System2415Orbit1Begin This star is component A of the close visual binary ADS 16800 AB. Component C, V = 9.5 mag, is separated from AB by about 19 arcsec. The velocities were obtained when the visual system, which has a period of 49 years, was near apastron. Many velocities of the primary and secondary have been given zero weight in the final orbital solution because of blending problems with the lines of component B, which is also a double lined binary. The weights of the velocities were not included in the published paper. All velocities are shown in the current orbital plot. System2415Orbit1End System2416Orbit1Begin The star is component B of the close visual binary ADS 16800 AB. Component C, V = 9.5 mag, is separated from AB by about 19 arcsec. The velocities were obtained when the visual system, which has a period of 49 years, was near apastron. Many velocities of the primary and secondary have been given zero weight in the final orbital solution because of blending problems with the lines of component A, which is also a double lined binary. The weights of the paper were not included in the published paper. All velocities are shown in the current orbital plot. System2416Orbit1End System2405Orbit2Begin SAAO = Balona, 1987, SAAO Circ., 11, 1 McD = McDonald Observatory, this paper KPNO = Kitt Peak National Observatory, this paper Because of their large residuals three velocities have been given zero weight in the solution, one from McD and two from SAAO. The velocities from the SAAO obtained on JD 2444235 and 2444639 have extremely large residuals, and so it is likely that those observations contain typographical errors in the original publication or should be attributed to another star. The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. The primary is a chromospherically active star. System2405Orbit2End System2417Orbit1Begin McD = McDonald Observatory KPNO = Kitt Peak National Observatory Velocities of JD 2,444,180 and 2,444,894 had 3-sigma residuals and were given zero weight in the final solution. The tests of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the eccentric-orbit solution is to be prefered. The primary is a chromospherically active star. System2417Orbit1End System2418Orbit1Begin Coravel = DeMedeiros and Udry, 1999, A&A, 346, 532) McD = McDonald Observatory, this paper KPNO = Kitt Peak National Observatory, this paper The primary is a chromospherically active star. System2418Orbit1End System2419Orbit1Begin - T0: apparent emission-line inferior conjunction given in the paper, change to periastron - epsilon= (P_sh - P_orb)/P_orb = 0.0332 0.0006, where P_sh= superhump period; P_orb= orbital period. System2419Orbit1End System2420Orbit1Begin The superhump period excess implied by this choice is epsilon=0.049 +- 0.003, while the mean relationship from Thorstensen et al. (1996, PASP,108,73) predicts epsilon=0.033 at this P. System2420Orbit1End System2421Orbit1Begin The detection of the secondary is suggests that the period is fairly long. Consistent with this expectation, the velocity periodogram shows that the orbital period cannot be of the gap; the leading candidate period is 0.2391 +- 0.0004. Bad observational conditions left this period determination slightly ambigous. System2421Orbit1End System2421Orbit2Begin System2421Orbit2End System2422Orbit1Begin - Period obtained from photometry. - Orbital elements obtained from H-alpha emission System2422Orbit1End System2422Orbit2Begin - Period obtained from photometry. - Orbital elements obtained from H-alpha emission (binned) System2422Orbit2End System2422Orbit3Begin - Period obtained from photometry. - To expedite readout, the data were binned on chip to 2x2 pixels and a region of 512x512 (binned) pixels was read. - Orbital elements obtained from H-alpha emission (binned) - V0_2= 38 +- 11, for secondary component (Absortion; binned) - From H-alpha emission: K1=116+-5, V0=18+-4, rms=19 System2422Orbit3End System2423Orbit1Begin - Orbital elements using H-alpha lines of all observing runs. - Because the velocity curve departs substantially from the sinusoid assumed in the period search, the contrast between the best candidate frequencies and their aliases is not as strong as one might expect from the time distribution of the data. The non-sinusoidal shape of the velocity curve also varied noticeably from one observing run to the other, inducing extra scatter when all three were combined and further reducing the selectivity of the global period search. The best frequencies selected by the velocities are near 9.5 or 10.5 1/day. The modulation seen in the photometry gives an independent ephemeris constraint. The interval between the deeper minima seen in the March and June runs was 80.889 +- 0.004 (estimated uncertainty) System2423Orbit1End System2423Orbit2Begin -Orbital elements obtained using H-alpha line observed in March 2001 System2423Orbit2End System2423Orbit3Begin -Orbital elements obtained using H-alpha line observed in May 2001 System2423Orbit3End System2423Orbit4Begin -Orbital elements obtained using H-alpha line observed in June 2001 System2423Orbit4End System2423Orbit5Begin -Orbital elements obtained using absortion line. System2423Orbit5End System2424Orbit1Begin -Simbad coordinates: 19 10 53.3 +28 56 22 (2000) - Our spectra are from two observing runs. The discovery on 1994 May 1 UT occurred on the penultimate night of the first run; on the final night (May 2) we obtained seventeen 600-s spectra, spanning 3.2 hours. We returned to the object 1997 June 29 July 2, and obtained 35 more exposures using the 2.4 m telescope, modular spectrograph, and a SITe 20482 CCD detector. While the uncertainty in P should be realistic, we caution that V0 and (especially) K1 in cases where they can be checked, are often serious mis-estimates of the systemic velocity and radial velocity amplitude of the white dwarf, so they should be viewed only as fitting parameters. A fit to the 1994 data alone with the period fixed at 0.1429 d yielded K1 = 114 +- 9 km/s, V0 = -48 +-6 km/s, and rms1 = 23 km/s. The improved rms1 probably reflects the somewhat brighter state of the star during the 1994 observations. The time interval between the 1994 and 1997 data sets is so long that there is no unique choice of cycle count between them, but if one assumes phase coherence, the two runs constrain the period to P = (1155.745+- 0.003 d)/N; where N = 8090+-55 is an integer. The uncertainty in N keeps P within +- 3 standard deviations of the value above. System2424Orbit1End System510Orbit2Begin -T0 is the epoch of apparent inferior conjunction of the line source. - The study by Kraft, R. P., Krzeminski, W., and Mumford, G. S., 1969, ApJ, 158, 589 (KKM) did define a phase tied to the red star in the system; this red-star phase should have a more direct physical interpretation than the emission-line phase. KKM noted that the emission lines are not precisely 180 degrees out of phase with the absorption (presumed to represent the red star), but rather lag by an additional 0.017 d (some 20 degrees of phase). The ephemeris quoted in KKM's equation (1) is for the inferior conjunction of the red star; if we assume that the 0.017 d offset still holds, we find for an updated red-star ephemeris: Red_star_inferior_conjunction = JD_{sun} 2448546.855 + 0.2898406(2) E, where E is the integer cycle count. For completeness we give here Emission-line inferior conjunction = JD{sun} 2448547.0174 + 0.2898406(2) E. System510Orbit2End System510Orbit3Begin -Orbital elements from re-fit the H{alpha} velocities from Robinson (1973,ApJ, 186, 347) -The good agreement between the K and V0 velocities in the two studies gives us confidence that our phases may be compared directly. System510Orbit3End System2425Orbit1Begin - Data from 1989 Nov. - Our period is consistent with Ratering et al., 1993,A&A,268,694 (RDB) period 0.1633 (11) d, and our smaller uncertainty reflects our longer time base. System2425Orbit1End System2425Orbit2Begin - Data from Oct + Nov 1989. - Individual observing runs were pre-adjusted to V0=0. The fits to combined runs depart only slightly from this. - RDB's 1989 October observations were reasonably near in time to ours (43 days) so we were able to place constraints on the precise period by combining period by combining the RBD 1989 october H-beta and H-alpha velocities with our 1989 November data, after adjusting all to a common V0=0 using fits to the individual observing runs. - The best fit is found at P=0.16264 (2) d, ~1.9 sigma longer than the period derived from our November data. System2425Orbit2End System2425Orbit3Begin - Data from Oct + Nov 1989. - Individual observing runs were pre-adjusted to V0=0. The fits to combined runs depart only slightly from this. - This is a another choice of cycle count gives a poorer fit at P=0.16184 (2) d , formally 8 sigma shorter than the period derived from our November data. System2425Orbit3End System2425Orbit4Begin - Data from 1990 Feb. System2425Orbit4End System2425Orbit5Begin - Although KT Per was in outburst in 1990 February, the H-alpha emissioni was reasonably strong (as RBD found in their 1986 data), so we again measured radial velocities. The periodicity manifested itself once again. The outburst data (JD 2447927 and 2447928) were taken 75 75 days after the last observations in quiescence, so we should in principle have been able to extrapolate the ephemeris derived from the 43-day October-November baseline with fair accuracy. We therefore attempted to combine the outburst velocities coherently with the quiescent velocities, but found that the two data sets did not fit together gracefully. A period search of the combined data sets yielded two cadidate periods, 0.162711 (Case 1) and 0.161817 d (Case 3). - Case 1: The high-state velocities are in phase with the low-state velocities, the period is 0.162711 days, and the low-state data have conspired to mislead us about uncertainty in the low-state period. - Individual observing runs were pre-adjusted to V0=0. The fits to combined runs depart only slightly from this. System2425Orbit5End System2425Orbit6Begin - Case 3: The low-state data have misled us as to the correct choice of cycle count on the October-November baseline, and all data phase together. - This is an alternate choice of cycle count. - Individual observing runs were pre-adjusted to V0=0. The fits to combined runs depart only slightly from this. System2425Orbit6End System2426Orbit1Begin -There appears to be modulation at a period slightly different from P_orb, but there is heavy aliasing at ~1 cycle d^-1 intervals because the photometric observations covered a small range of hour angle, so we cannot unambigously determina the photometric period. Also, in view of the small redundancy of the data, we cannot be certain of the modulation's reality, and the nonrandom nature of the underlying noise process makes simple quantitative confidence estimaes unrealiable System2426Orbit1End System2427Orbit1Begin - Combining our revised period with the superhump period changes 'epsilon' from 0.0141 +- 0.0023 to 0.0204 +- 0.0015. The mean epsilon - P_orb relation from Thorstensen et al. (1996, PASP, 108, 73) predicts epsilon = 0.0234. The revised period is therefore more consistent with that expected from the superhump period. System2427Orbit1End System2428Orbit1Begin -While our 100.10+-0.07 min period appears secure, with a (one-sided) discriminatory power of 972/1000 and a correctness likehood again indistiguishable from unity, we were unable to find a superhumps period in the literature for comparison. System2428Orbit1End System2429Orbit1Begin - T0: Apparent emission-line inferior conjunction, HJD 2,450,000. System2429Orbit1End System2430Orbit1Begin - T0: Apparent emission-line inferior conjunction, HJD 2,450,000. System2430Orbit1End System2431Orbit1Begin - To search the period, we used a least-squares periodogram technique (Thorstensen et al. 1996,PASP, 108,39). -While the uncertainty in P should be realistic, we caution that V0 and (especially) K in cases where they can be checked, rarely indicate the systemic velocity and radial-velocity semiamplitude of the white dwarf. Thus listed values should not be used in dynamical solutions of the system. - T0: apparent inferior conjunction of the emission-line source, which in any case may not trace the white-dwarf motion accurately. Corrected to "periastron". System2431Orbit1End System2432Orbit1Begin - To search the period we used a least-squares periodogram technique (Thorstensen et al. 1996,PASP, 108,39) -A search for a precise period by analyzing all our emission-line velocities together with the velocities used by Jablonski & Cieslinski, 1992, A&A, 259, 198 (JC). The period search showed fine structure in the 16.08 d^-1 peak arising from the cycle count in the ~1900 d interval between JC's observations and ours. A Monte-Carlo simulation showed that this time series has a discriminatory power of 985/1000 on this interval, so the best period is strongly preferred but not stablished absolutely. System2432Orbit1End System2433Orbit1Begin -We searched for periods in the radial velocities by creating a dense grid of evenly spaced trial frequencies and fitting least-squares sinusoids at each frequency. We then plotted 1/sigma^2, where sigma is the standard deviation of the fit, as a function of trial frequency. At periods selected by this method we fit least-squares sinusoids. - The periodogram shows a preferred frequency near 6 cycles day^-1. In 1000 Monte-Carlo simulations, the best-fit period was chosen all 1000 times. The alias choice is therefore secure, especially since our period is consistent (within 1.7 sigma) with that of Shafter, Veal, Robinson, 1995, ApJ, 440.(SVR) System2433Orbit1End System2434Orbit1Begin - We searched for periods in the radial velocities by creating a dense grid of evenly spaced trial frequencies and fitting least-squares sinusoids at each frequency. We then plotted 1/sigma^2, where sigma is the standard deviation of the fit, as a function of trial frequency. At periods selected by this method we fit least-squares sinusoids. - The orbital period is most likely 0.16490 +- 0.00001 days (3.96 hr), but periods of 0.16551 +- 0.00001 days (3.97 hr) and 0.16431 +- 0.00001 days (3.94 hr) are not excluded. Those periods have been found using Monte Carlo simulations. System2434Orbit1End System2435Orbit1Begin -We searched for periods in the radial velocities by creating a dense grid of evenly spaced trial frequencies and fitting least-squares sinusoids at each frequency. We then plotted 1/sigma^2, where sigma is the standard deviation of the fit, as a function of trial frequency. At periods selected by this method we fit least-squares sinusoids. - The periodogram shows a frequency of roughly 6.5 cycles d^-1. In the Monte Carlo simulations, the best-fit period was chosen all 1000 times. The spectrum is unremarkable for a dwarf nova. System2435Orbit1End System2436Orbit1Begin - The emission lines move with P = 0.115063(1) days, which is presumably the underlying orbital period of the binary. Photometry reveals a different period, namely, 0.12228(1) days. The presence of this wave in a short-period cataclysmic variable, and the value of the period excess at 6.3%, suggests identification as a permanent superhump. After subtraction of this large signal, the residual time series appears to contain a weak feature at 0.11193(5) days. The star evidently shows positive and negative superhumps simultaneously. Its binary period puts it among a modest number of nonmagnetic cataclysmic variables occupying the 2-3 hr period "gap'. System2436Orbit1End System2437Orbit1Begin - From velocities of Ha emission lines, we determine an orbital period of 0.174774 +- 0.000003 days (=4.1946 hr), which agrees with Szkody's value of approximately 4.2 hr. No stable photometric signal was found at the orbital period. A noncoherent quasi-periodic photometric signal was seen at a period of minutes. 20.750.3 System2437Orbit1End System1086Orbit2Begin - Radial velocities from H + He II lines. - The photometric data described in Patterson et al. (1993, ApJS, 86, 235) prove that both the short-period signal and the long-period signal wander significantly in period. Neither agrees with the spectrocopic period. While there is no proof that P_spec = P_orb, the fact remains that the photometric periods are known to be untable, which certainly disqualifies them as candidates to be P_orb. Thus it seems likely that the conventional view (P_orb = P_spec) is correct, in which case the two photometric signals satisfy the defining criterion for superhumps: slightly unstable periodic features slightly displaced (+6.5% and -3.1%) from P_orb. System1086Orbit2End System1086Orbit3Begin - Radial velocities from He I line. System1086Orbit3End System2438Orbit1Begin - Because most of the "velocity" amplitude apparently comes from variations in the line profile, K is not a reliable indicator of the motion of either star. - Although the interval between 1998 January and March is too long to derive an unambiguous cycle count, we can use the phases at the two epochs to restrict the period to P = (52.32950.009)/N days, where is an integer. The uncertainty of N is chosen to yield periods within +-2 standard deviations of the fit to the March data alone. System2438Orbit1End System2439Orbit1Begin - Orbital elements from He I line. 3.2. Those lines were fairly weak and not always measurable, but they proved to be the most useful features for orbital period determination. - The radial velocities indicate an underlying binary period of 0.1445(2) day; the long-term cycle count is not firmly decided, but the best choice implies a period of 0.144464(1) day. The star shows a moderately low excitation spectrum with transient P Cygni absorption suggestive of a wind origin, occasionally seen in cataclysmic variables accreting at a high rate. Curiously, the P Cygni absorption appears correlated with binary phase in our two most extensive data sets. A photometric wave with day, slightly shorter than , rumbles P = 0.1394(1) slightly shorter than P_orb, rumbles through the light curve, as well as a low-frequency wiggle at 3.94(6) days. System2439Orbit1End System2439Orbit2Begin - Orbital elements from H-beta line. This emission-line peaks also gave a discernible orbital signal, but with a lower amplitude than the He I lines. System2439Orbit2End System2439Orbit3Begin - Orbital elements adopted. The 0.144464 day period is the strongest in both sets of velocities and lies only about 1 standard deviation from the photometric prediction. We therefore adopt it as a fiducial period but emphasize its nonuniqueness. System2439Orbit3End System848Orbit3Begin - V magnitude extracted from the paper. V Mag. from SIMBAD = 9.11. - We obtained 12 velocities and use them in combination with Boopp et al.'s (1984,ApJ,285,202) KPNO CCD data from 1983 and Grewing et al.'s (1989,A&A,223,172) data from 1986, to recompute the orbital elements. All observations were given equal weight. Final orbital elements were derived with the differential-correction program of Barker et al. (1967,ROB,No, 130). A first run with the preliminary elements of Bopp et al. converged at an eccentricity so close to zero that a formal zero-eccentricity solution was adopted. Some residuals are as large as 9 km s^-1. System848Orbit3End System2459Orbit1Begin - 'e' and 'w' adopted. - Bopp et al. (1993,AJ 106, 2502) presented a first zero-eccentricity SB1 orbit and found a period of 23.9729 +- 0.0022 days from 44 radial velocities taken between 1985 and 1992. We add our 14 velocities to refine the orbital elements. The adopted velocities for our cross-correlation stars were 3.2 km s^-11 for beta Gem (K0III), -14.5 km s^-11 for alpha Ari (K2III), and +54.3 km s^-1 for HR 8551 (K0III-IV) (Scarfe et al. 1990,Publ. Dom. Astron. Obs.Victoria 18, 21). No systematic velocity differences were evident, but two of the velocities from Bopp et al. (1993) were given zero weight. System2459Orbit1End System2440Orbit1Begin - We obtained 43 radial velocities from our red-wavelength spectra and find the star to be a single-lined spectroscopic binary. One additional velocity of 19: km s^-1 was obtained by Osten & Saar (1998,MNRAS 295, 257) under the assumption that the star has no composite spectrum. This velocity deviates by 15 km s^-1 from our smallest value (-4 km s^-1) and is therefore not used in the orbit computation. A single velocity from a blue-wavelength Ca II H&K spectrum from April 1998 (Strassmeier et al. 2000,A&AS 142, 275) was only used for the period search but not in the orbit determination. Initially, all velocities were given equal weight for a preliminary orbital solution. Final orbital elements were derived with the differential-correction program of Barker et al. (1967,ROB No. 130) as described in the update by Fekel et al. (1999,A&AS,137, 369). The solution with preliminary elements converged at an eccentricity of 0.001 +- 0.01 so that a formal zero-eccentricity solution was adopted. The standard error of an observation of unit weightwas 1.5 km s^-1 but two O-C residuals were as large as 4-5 km s^-1 and were given half weight in the final solution. System2440Orbit1End System181Orbit2Begin - (*): Nights where no radial-velocity standards were observed. These velocities rely on a zero-point from the Th-Ar comparison lamp. Nightly zero-point corrections were applied from the measurements of the radial-velocity standard alpha Ari whenever possible. - Assuming zero orbital eccentricity (Fekel 1983,ApJ 268, 274; Donati et al. 1992,A&A 265, 682), we redetermine the orbit. - We keep orbital period fixed to the value originally determined by Fekel (1983, ApJ 268, 274) and obtain the phase shift of the superior conjunction, HJD_sup.conj. = 2442766.080 + 2.83774xE where the zero point is a time of superior conjunction (primary in front) and the period is the orbital period. - The tertiary is a fainter K3V star 6" away. - Throughout this paper, errors quoted are always the standard deviations computed from the combined line-profile and light-curve fits and the data; a weight of 0.2 was assigned to the photometry. - Our radial velocities from the NSO McMath-Pierce stellar spectrograph sometimes show arbitrary shifts of up to 5 km s^-1, most likely due to mechanical motion of the spectrograph components. Such shifts were also noted in the 1988/89 NSO data of Donati et al. (1992) attributed to the same effect and, consequently, our orbital elements are of large external uncertainty. The O-C's are nevertheless comparable to Fekel's original orbit from data taken between 1975 and 1981. Despite the velocity shifts, the velocity differences between the two stellar components should not be affected. System181Orbit2End System2441Orbit1Begin - Comments: central wavelength in angstrom of the line used to measure the radial velocity. In parethesis the year when data was taken. - The orbital period is estimated by eye to be ~10 yrs based on a systemic velocity of around -19 km s^-1 and a time of periastron passage in late 1994, and remains fixed throughout the iterative solution for the orbital elements. The formally best solution gives a standard error of an observation of unit weight of 1.7 km s^-1, thus comparable to our observational uncertainties, but the O-C residuals for the eight velocities from 1991-1993 are systematically too high (by 1.2-3.2 km s^-1). Thus, we emphasize that our orbit is just preliminary and based on a rough estimate of the period. System2441Orbit1End System2442Orbit1Begin - Mag1 from SIMBAD = 10.70. - The rms for each component give the upper limits of the measurement uncertainties, because they contain the deviations of the component velocities from the simplified model of circular orbits without any proximity effects (i.e. without allowance for non-coinciding photometric and dynamic centres of the components). - The individual observations, as well as the observed minus calculated (O-C) deviations from the sine-curve fitting to radial velocities of individual components. In order to find appropriate fitting parameters we assumed only the value of the period, following Odell (1996,MNRAS, 282, 373), and determined the mean velocity V0, the two amplitudes K1 and K2, as well as the moment of the primary minimum T0. System2442Orbit1End System2443Orbit1Begin - As expected, the moment of the primary minimum is considerably different from predictions based on the existing ephemerides. As was shown by Herczeg & Drechsel (1985,Ap&SS,114,1), the rate of the period change is not constant in SV Cen. Drechsel provided us a new ephemeris resulting from a combination of the Drechsel and Herczeg data with the new moment of the primary minimum JD_hel(pri)= 2443332.9756(18) + 1.6585318(45)E-4.1(2)x10^-8E^2 with the standard deviation of 0.0039 day. It should be noted that the quadratic term corresponds to an e-folding time of the orbital period change of 55000 yr. -Drechsel et al. on the basis of colours guessed them to be B1V and B6.5III). System2443Orbit1End System2444Orbit1Begin - tel1: Data obtained with the 1.2m telescope and its 32121 coude spectrograph which gave a dispersion of 10 angstroms/mm and the coverage of only 100 angstroms with the FORD CCD detector at the Dominion Astrophysical Observatory. - tel2: Data obtained with the 1.8m telescope and the 21121 spectrograph which gave a dispersion of 15 angstroms/mm and wavelength of 150 and 240 angstroms with the FORD and RCA CCD respectively at the Dominion Astrophysical Observatory. - (*)= half weight were given for this data. - Circular orbit was adopted. - Orbital solution was made using the "Bootstrap" (Efron, 1979, Rietz Lecture, Ann. Statistics,7,1) method. One thousand samples of ramdomly drawn data points (with repetitions) from the velocities listed led to one thousand solutions for each component. By analyzing the mean values and dispersions of such distributions of solutions, the following elements were obtained: the systemic velocities V0_1= +43.5 +- 1.8 km/s and V0_2=+44.7 +- 2.7 km/s and the semi-amplitudes K1=109.7 +- 2.1 km/s and K2=185.7 +- 2.7 km/s. This method, however, helped to establish the rms errors of the solutions for parameters above. - A linear solution for the light elements was tried, giving the ephemeris as follows: HJD min I = 2425918.3597(16) +0.71181663(7)E In the solution, twenty times higher weights were given to the minima determined by photometry than to those obtained by visual photographic means. System2444Orbit1End System2445Orbit1Begin - The period 0.3449094 by Cereda et al. (1988,A&AS,76,255) was adopted and fixed. The time T0 of deeper mideclipse by a quarter of period, was not fixed because the period of the system seems not precisely determined or may be variable. - A circular orbit was adopted. System2445Orbit1End System713Orbit2Begin - BF Circular: radial velocities processed using the newly developed method of Broading Function (BF) by Rucinski 1992,AJ,104,1968. - (*)= Blue spectrum centered at the G-Band. - Three sets of orbital elements were obtained from the separate solutions of the velocities from the BF and CCF profiles using the traditional approach. First, we used a Gaussian fit to the component simple circular orbit. As the program finds the time T of the positive maximum velocity of the primary star, we added one quarter of the period to obtain the photometric initial epoch. The period was set equal to the recently derived value of 0.40752779 (Demircan et al.,1991,AJ,101,201). Two solutions based on the BF and CCF profiles with Gaussian fittings. We found that our determination of the initial epoch, T0, differed slightly from the most recent time of light minimum HJD 2447569.36214 (Demircan et al.,1991,AJ,101,201) for the BF and CCF solutions. System713Orbit2End System2446Orbit1Begin System2446Orbit1End System2447Orbit1Begin The observations obtained on JD 2450578 and 2450927 showed that the lines of the components were partially blended and so the velocities from those observations were given zero weight in the final solution. The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Given the spectral types of the two components, both the primary and secondary are presumably chromospherically active stars. System2447Orbit1End System1473Orbit2Begin The elements listed correspond to a joint astrometric-spectroscopic solution that combines radial velocities with visual and speckle measurements of the relative position (angular separation and position angle) of the components. The remaining elements of the combined solution are: Semimajor axis of relative orbit = 0.1005 +/- 0.0019 arc seconds Position angle of ascending node (J2000) = 216.58 +/- 0.82 degrees Inclination angle = 124.97 +/- 0.92 degrees Derived quantities: Orbital parallax = 21.44 +/- 0.67 milli arc seconds Linear semimajor axis = 4.688 +/- 0.086 AU M1 = 1.363 +/- 0.073 solar masses M2 = 1.253 +/- 0.075 solar masses q = M2/M1 = 0.919 +/- 0.027 Time span of observations = 37.1 yr System1473Orbit2End System1245Orbit3Begin The elements listed correspond to a joint astrometric-spectroscopic solution that combines radial velocities with interferometric visibilities. The remaining elements of the combined solution are: Semimajor axis of relative orbit = 15.378 +/- 0.027 milli arc seconds Position angle of ascending node (J2000) = 334.960 +/- 0.070 degrees Inclination angle = 99.364 +/- 0.080 degrees Magnitude difference in K (CIT system) = 1.056 +/- 0.013 Magnitude difference in H (CIT system) = 1.154 +/- 0.065 Derived quantities: Orbital parallax = 46.08 +/- 0.27 milli arc seconds M1 = 0.844 +/- 0.018 solar masses M2 = 0.6650 +/- 0.0079 solar masses Magnitude difference in V = 2.4 +/- 0.2 mag System1245Orbit3End System2448Orbit1Begin Photometric variability detected in the Hipparcos observations, presumably corresponding to ellipsoidal variability. The primary minimum is only 0.05 mag deep in the Hp band. Derived quantities: M1 (sin i)**3 = 0.05571 +/- 0.00190 Msun M2 (sin i)**3 = 0.01191 +/- 0.00037 Msun q = M2/M1 = 0.2138 +/- 0.0045 a1 sin i = 0.1587 +/- 0.0027 x 10**6 km a2 sin i = 0.7422 +/- 0.0094 x 10**6 km Time span of observations (days) = 4435 The unpublished radial velocities reported here, on which the orbit is based, are preliminary. System2448Orbit1End System2449Orbit1Begin Derived quantities: f(M) = 0.00576 +/- 0.00051 MSun M2 (sin i) = 0.179 (M1+M2)**(2/3) MSun a1 (sin i) = 21.48 +/- 0.67 x 10**6 km Time span = 1601 days System2449Orbit1End System2450Orbit1Begin Derived quantities: Light ratio L(sec)/L(prim) = 0.3 at 5187 Angstroms M1 (sin i)**3 = 0.528 +/- 0.033 Msun M2 (sin i)**3 = 0.440 +/- 0.024 Msun q = M2/M1 = 0.834 +/- 0.024 a1 sin i = 61.0 +/- 1.2 x 10**6 km a2 sin i = 73.2 +/- 1.9 x 10**6 km Time span = 1601 days System2450Orbit1End System585Orbit3Begin Projected rotational velocity (v sin i) of primary = 22 km/s Projected rotational velocity (v sin i) of secondary = 22 km/s Light ratio at 5187 Angstroms: L(sec)/L(prim) = 0.66 +/- 0.02 Derived quantities: M1 (sin i)**3 = 1.1998 +/- 0.0044 Msun M2 (sin i)**3 = 1.1338 +/- 0.0035 Msun q = M2/M1 = 0.9450 +/- 0.0020 a1 sin i = 3.9722 +/- 0.0051 x 10**6 km a2 sin i = 4.2032 +/- 0.0072 x 10**6 km a sin i = 11.746 +/- 0.013 Rsun Time span of observations (days) = 5816 Changes in the orbital elements reported by other authors are not confirmed by these observations. System585Orbit3End System2451Orbit1Begin The companion of OGLE-TR-113 is a transiting planet. The period and transit epoch were fixed in the spectroscopic solution to the values determined from the transit light curve solution: P = 1.4324758 +/- 0.0000046 days T = 2452325.79823 +/- 0.00082 (HJD) Derived quantities: M2 (sin i) = 1.21 +/- 0.31 x 10**(-3) (M1+M2)**(2/3) MSun System2451Orbit1End System2451Orbit2Begin The companion of OGLE-TR-113 is a transiting planet. The orbital period and transit epoch were adopted from Udalski et al. (2002): 2002AcA....52..317U System2451Orbit2End System2452Orbit1Begin The companion of OGLE-TR-56 is a transiting planet. The period and transit epoch were fixed in the spectroscopic solution to the values determined from the transit light curve solution: P = 1.2119189 +/- 0.0000059 days T = 2452075.1046 +/- 0.0017 (HJD) Derived quantities: M2 (sin i) = 1.33 +/- 0.21 x 10**(-3) (M1+M2)**(2/3) MSun An offset of -0.192 km/s has been applied to the observations obtained in 2003 in order to refer them to the same reference frame as those from the preceding year. This offset was determined along with the orbital elements of OGLE-TR-56 in a simultaneous solution involving also observations of two radial-velocity standard stars (HD 179949 and HD 209458). System2452Orbit1End System2453Orbit1Begin Derived quantities: M1 (sin i)**3 = 0.2396 +/- 0.0027 Msun M2 (sin i)**3 = 0.2220 +/- 0.0025 Msun q = M2/M1 = 0.9265 +/- 0.0063 a1 sin i = 4.191 +/- 0.021 x 10**6 km a2 sin i = 4.523 +/- 0.022 x 10**6 km System2453Orbit1End System2453Orbit2Begin The orbital period is listed incorrectly in the original publication. It has been corrected here. Derived quantities: M1 (sin i)**3 = 0.24069 +/- 0.00091 Msun M2 (sin i)**3 = 0.22535 +/- 0.00082 Msun q = M2/M1 = 0.936 +/- 0.003 a1 sin i = 4.2234 +/- 0.0063 x 10**6 km a2 sin i = 4.5110 +/- 0.0082 x 10**6 km v sin i for primary = 6 km/s v sin i for primary = 5 km/s System2453Orbit2End System2454Orbit1Begin Projected rotational velocity (v sin i) = 34 km/s Derived quantities: f(M) = 0.0041 +/- 0.0034 Msun M2 (sin i) = 0.1603 * (M1+M2)**(2/3) MSun a1 sin i = 0.58 +/- 0.16 x 10**6 km Time span of observations (days) = 1209 System2454Orbit1End System2455Orbit1Begin Projected rotational velocity (v sin i) of primary = 25 km/s Projected rotational velocity (v sin i) of secondary = 10 km/s (approx.) Light ratio at 5187 Angstroms: L(sec)/L(prim) = 0.14 +/- 0.02 Derived quantities: M1 (sin i)**3 = 1.12 +/- 0.12 Msun M2 (sin i)**3 = 0.831 +/- 0.049 Msun q = M2/M1 = 0.743 +/- 0.037 a1 sin i = 2.661 +/- 0.024 x 10**6 km a2 sin i = 3.58 +/- 0.18 x 10**6 km a sin i = 8.97 +/- 0.25 Rsun Time span of observations (days) = 740 System2455Orbit1End System1472Orbit2Begin The elements listed correspond to a joint astrometric-spectroscopic solution that combines radial velocities with visual micrometer measurements and one photographic measurement of the relative position (angular separation and position angle) of the two components. The remaining elements of the combined solution are: Semimajor axis of relative orbit = 0.924 +/- 0.021 arc seconds Position angle of ascending node (J2000) = 156.4 +/- 5.2 degrees Inclination angle = 146.9 +/- 4.7 degrees Derived quantities: Orbital parallax = 16.6 +/- 2.1 milli arc seconds M1 = 1.09 +/- 0.41 solar masses M2 = 0.69 +/- 0.29 solar masses M1 + M2 = 1.78 +/- 0.58 solar masses q = M2/M1 = 0.63 +/- 0.29 System1472Orbit2End System2456Orbit1Begin The system is triple. Derived quantities for inner (double-lined) orbit: M1 (sin i)**3 = 2.558 +/- 0.012 Msun M2 (sin i)**3 = 2.488 +/- 0.011 Msun q = M2/M1 = 0.9729 +/- 0.0029 a1 sin i = 14.669 +/- 0.030 x 10**6 km a2 sin i = 15.077 +/- 0.031 x 10**6 km a sin i = 42.739 +/- 0.062 Rsun The inclination angle "i" is that of the inner orbit. Derived quantities for outer orbit (comprising the inner double-lined binary and a more distant unseen companion): a12 sin i = 49.8 +/- 1.3 x 10**6 km f(M) = 0.01070 +/- 0.00079 Msun M3 sin i = 0.2203 (M1 + M2 + M3)**(2/3) Msun The inclination angle "i" is that of the outer orbit. M3 is the mass of the third distant companion, and a12 is the semimajor axis of the orbit of the inner binary. System2456Orbit1End System2457Orbit1Begin Projected rotational velocity (v sin i) of primary = 19 km/s Projected rotational velocity (v sin i) of secondary = 15 km/s Light ratio at 5187 Angstroms: L(sec)/L(prim) = 0.39 +/- 0.02 Derived quantities: M1 (sin i)**3 = 0.3168 +/- 0.0061 Msun M2 (sin i)**3 = 0.2825 +/- 0.0046 Msun q = M2/M1 = 0.8917 +/- 0.0099 a1 sin i = 1.746 +/- 0.012 x 10**6 km a2 sin i = 1.958 +/- 0.017 x 10**6 km a sin i = 5.323 +/- 0.030 Rsun Time span of observations (days) = 1157 System2457Orbit1End System2042Orbit2Begin Period and epoch of primary minimum fixed from linear ephemeris based on times of eclipse. Radial velocities were computed with the two-dimensional cross-correlation technique TODCOR, using synthetic templates with rotational broadening corresponding to v sin i = 10 km/s for both components. Templates with rotational velocities of v sin i = 20 km/s lead to very similar orbital elements, with only slightly larger uncertainties. Derived quantities: M1 (sin i)**3 = 1.268 +/- 0.005 Msun M2 (sin i)**3 = 1.250 +/- 0.004 Msun q = M2/M1 = 0.985 +/- 0.002 a1 sin i = 5.163 +/- 0.008 x 10**6 km a2 sin i = 5.242 +/- 0.008 x 10**6 km System2042Orbit2End System2458Orbit1Begin The system is triple. Derived quantities for inner (double-lined) orbit: M1 (sin i)**3 = 2.558 +/- 0.012 Msun M2 (sin i)**3 = 2.488 +/- 0.011 Msun q = M2/M1 = 0.9729 +/- 0.0029 a1 sin i = 14.669 +/- 0.030 x 10**6 km a2 sin i = 15.077 +/- 0.031 x 10**6 km a sin i = 42.739 +/- 0.062 Rsun The inclination angle "i" is that of the inner orbit. Derived quantities for outer orbit (comprising the inner double-lined binary and a more distant unseen companion): a12 sin i = 49.8 +/- 1.3 x 10**6 km f(M) = 0.01070 +/- 0.00079 Msun M3 sin i = 0.2203 (M1 + M2 + M3)**(2/3) Msun The inclination angle "i" is that of the outer orbit. M3 is the mass of the third distant companion, and a12 is the semimajor axis of the orbit of the inner binary. System2458Orbit1End System2462Orbit1Begin This star is the primary component of a close triple system. It has both delta Scuti type pulsations and ellipsoidal light variations. Narrow lines from a second star are also visible in the spectrum, but the velocities of that star do not correspond to the secondary of the 1.47-day system. Rather the narrow-lined star is a third component. New velocities not included in the paper indicate that the third component has an orbital period of almost exactly 2 years. Because of velocity variations in the long period orbit, only 6 velocities were used in the short-period orbital solution. The period from the ellipticity effect was increased by a factor of two and adopted as the orbital period. Since a circular orbit was also adopted, the element T is not a time of periastron passage, but is T_0, a time of maximum velocity. Note that the center of mass velocity of the short-period orbital solution is for the mean epoch of the observations and is not that of the triple system. System2462Orbit1End System1028Orbit2Begin System1028Orbit2End System2463Orbit1Begin System2463Orbit1End System169Orbit2Begin SB9: The period was changed from 6.4372703 to 6.4378703 days. The radial velocities are not adjusted according to the suggested change on the systemic velocity along with time. The weight column actually lists the factor by which the inverse of the standard deviation is multiplied to derive the real weight. System169Orbit2End System2464Orbit1Begin The radial velocities are the mean gamma velocities of the inner orbit. System2464Orbit1End System2464Orbit2Begin The radial velocities are the mean gamma velocities of the inner orbit. System2464Orbit2End System2465Orbit1Begin System2465Orbit1End System2466Orbit1Begin SB9: P is given with a few more decimals than in the original paper. System2466Orbit1End System2467Orbit1Begin System2467Orbit1End System2468Orbit1Begin SB9: P is given with a few more decimals than in the original paper. System2468Orbit1End System2469Orbit1Begin SB9: P is given with a few more decimals than in the original paper. System2469Orbit1End System2470Orbit1Begin System2470Orbit1End System2471Orbit1Begin System2471Orbit1End System2472Orbit1Begin SB9: T0 is given with a few more decimals than in the original paper and also ajusted to have omega=0.. System2472Orbit1End System120Orbit2Begin System120Orbit2End System2473Orbit1Begin System2473Orbit1End System2474Orbit1Begin System2474Orbit1End System2475Orbit1Begin System2475Orbit1End System2475Orbit2Begin System2475Orbit2End System2476Orbit1Begin The very same orbit with the same radial velocities appears in two consecutive papers. System2476Orbit1End System2476Orbit2Begin The very same orbit with the same radial velocities appears in two consecutive papers. System2476Orbit2End System2477Orbit1Begin System2477Orbit1End System2478Orbit1Begin System2478Orbit1End System2479Orbit1Begin System2479Orbit1End System1925Orbit2Begin System1925Orbit2End System2480Orbit1Begin System2480Orbit1End System2481Orbit1Begin System2481Orbit1End System2482Orbit1Begin System2482Orbit1End System2483Orbit1Begin System2483Orbit1End System2484Orbit1Begin System2484Orbit1End System2485Orbit1Begin System2485Orbit1End System2486Orbit1Begin System2486Orbit1End System2487Orbit1Begin The listed coordinates are those of the cluster. System2487Orbit1End System2488Orbit1Begin The listed coordinates are those of the cluster + 5" in dec to make it two distinct entries in SB9. System2488Orbit1End System2488Orbit2Begin The listed coordinates are those of the cluster + 5" in dec to make it two distinct entries in SB9. System2488Orbit2End System2489Orbit1Begin System2489Orbit1End System2490Orbit1Begin System2490Orbit1End System2491Orbit1Begin The listed coordinates are those of the cluster. System2491Orbit1End System2492Orbit1Begin The listed coordinates are those of the cluster + 5" in dec to make it two distinct entries in SB9. System2492Orbit1End System2493Orbit1Begin System2493Orbit1End System2494Orbit1Begin System2494Orbit1End System2495Orbit1Begin System2495Orbit1End System2496Orbit1Begin System2496Orbit1End System2497Orbit1Begin System2497Orbit1End System2498Orbit1Begin System2498Orbit1End System2499Orbit1Begin System2499Orbit1End System2500Orbit1Begin System2500Orbit1End System2501Orbit1Begin System2501Orbit1End System2502Orbit1Begin System2502Orbit1End System2503Orbit1Begin The listed coordinates are those of the cluster. System2503Orbit1End System2504Orbit1Begin System2504Orbit1End System2505Orbit1Begin System2505Orbit1End System2506Orbit1Begin The listed coordinates are those of the cluster + 5" in dec in order to make two distinct entries in SB9. System2506Orbit1End System2507Orbit1Begin The listed coordinates are those of the cluster - 5" in dec in order to make two distinct entries in SB9. System2507Orbit1End System2508Orbit1Begin System2508Orbit1End System2509Orbit1Begin System2509Orbit1End System1976Orbit2Begin System1976Orbit2End System1972Orbit2Begin System1972Orbit2End System1975Orbit2Begin System1975Orbit2End System1974Orbit2Begin System1974Orbit2End System1973Orbit2Begin System1973Orbit2End System2510Orbit1Begin System2510Orbit1End System2511Orbit1Begin System2511Orbit1End System2512Orbit1Begin System2512Orbit1End System2513Orbit1Begin System2513Orbit1End System2514Orbit1Begin System2514Orbit1End System2515Orbit1Begin System2515Orbit1End System2516Orbit1Begin System2516Orbit1End System2517Orbit1Begin System2517Orbit1End System2518Orbit1Begin System2518Orbit1End System2519Orbit1Begin System2519Orbit1End System2520Orbit1Begin System2520Orbit1End System2521Orbit1Begin System2521Orbit1End System2522Orbit1Begin System2522Orbit1End System2523Orbit1Begin System2523Orbit1End System2524Orbit1Begin System2524Orbit1End System2525Orbit1Begin System2525Orbit1End System2526Orbit1Begin System2526Orbit1End System2527Orbit1Begin System2527Orbit1End System2528Orbit1Begin System2528Orbit1End System2529Orbit1Begin System2529Orbit1End System2530Orbit1Begin 4" subtracted from dec in order to make two distincts entries in SB9. System2530Orbit1End System2531Orbit1Begin System2531Orbit1End System2532Orbit1Begin System2532Orbit1End System2533Orbit1Begin System2533Orbit1End System2534Orbit1Begin System2534Orbit1End System2535Orbit1Begin System2535Orbit1End System690Orbit3Begin System690Orbit3End System636Orbit3Begin The systemic radial velocity of the secondary is listed as -5.4+/-4.5 km/s in the paper. For the plot, an offset of 9.4km/s was added to all RV of the secondary. System636Orbit3End System2536Orbit1Begin System2536Orbit1End System2537Orbit1Begin System2537Orbit1End System2538Orbit1Begin System2538Orbit1End System2539Orbit1Begin System2539Orbit1End System2540Orbit1Begin System2540Orbit1End System2541Orbit1Begin System2541Orbit1End System2542Orbit1Begin System2542Orbit1End System2543Orbit1Begin System2543Orbit1End System910Orbit2Begin The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positve velocity. The primary is rotating substantially slower than its synchronous velocity, while the secondary may be synchronously rotating. The system has at least two and perhaps three types of light variations. >From their ground-based photometry the authors confirm the ellipsoidal light variation previously noted in the Hipparcos photometry. Also detected in the new photometry are periods of 0.076 and 0.059 days, indicating that the primary is a delta Scuti variable. The photometry also suggests the possibility of extremely shallow grazing eclipses. System910Orbit2End System372Orbit3Begin This is visual primary in a spectroscopic visual quadruple system. The comment means: Instrument code DAO - DAO photograhic observation MR - McDonald Reticon detector KF - KPNO Fairchild CCD KR - KPNO RCA CCD KT - KPNO Texas Instruments CCD w - value for component Aa The value for omega was revised for SB9. The original value was w : 289+/-19 System372Orbit3End System373Orbit2Begin This is visual secondary in a spectroscopic visual quadruple system. The radial velocities were obtained at McDonald Observatory and KPNO. System373Orbit2End System2544Orbit1Begin This is a spectroscopic visual quadruple system: each visual component is a short-period spectroscopic binary. w - value for component B System2544Orbit1End System2005Orbit2Begin Observations have been made at KPNO using the Coude-fed telescope with CCD detectors. The original orbital period of 27.55 +- 0.05 (Bloomer et al., 1983, ApJ 270, L79) was refined to 27.5384 +- 0.0045 by finding the O-C residuals for the orbital phase of mid-primary eclipse as a function of cycle number. Oribital elements of secondary component are following: V0 = 13.21 +- 0.53 T0 = 2445462.48 +- 0.05 System2005Orbit2End System27Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System27Orbit3End System2545Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) The value of eccentricity was fixed. Preliminary orbit. System2545Orbit1End System1470Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) The values of T0 and e have been fixed. Preliminary orbit. System1470Orbit2End System46Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System46Orbit2End System57Orbit2Begin The values of T0 and e have been fixed. PI - The radial velocities were taken from Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Other measurements have been published by Jasniewicz and Mayor (1988A&A...203..329J) Preliminary orbit. System57Orbit2End System2546Orbit1Begin The values of T0 and e have been fixed. The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. System2546Orbit1End System2547Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2547Orbit1End System136Orbit4Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Early velocities by Colacevich (1941PUFir..59.....A) have been used to get a more precise determination of period. It has been fixed in solution. System136Orbit4End System2548Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2548Orbit1End System169Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) The values of e and w have been fixed. System169Orbit3End System1535Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) P was fixed to its value in the astrometric orbit. 12 additional values of radial velocity were taken from Campbell et al. (1988ApJ...331..902C) to calculate orbital elements. Preliminary orbit. System1535Orbit2End System2179Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2179Orbit3End System523Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) For a precise determination of the period authors used early measurements of Joy and Abetti (1919ApJ....50..391J). The other elements were obtained with fixed P. System523Orbit2End System2549Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. System2549Orbit1End System2550Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2550Orbit1End System680Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System680Orbit3End System2551Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. Three solutions with fixed P=3000, 4000, 5000d give respectively e = 0.04, 0.17, 0.26. Authors adopted the second solution as mean preliminary orbit. System2551Orbit1End System2552Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2552Orbit1End System799Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) 10 additional measurements by Kamper (1987AJ.....93..683K) were used around periastron for calculations of orbital elements. System799Orbit3End System2553Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit with arbitrary fixed period. System2553Orbit1End System2554Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. Other solutions with P = 6850 or 10050d are less credible. The adopted solution is the best fit using early Lick observations (PLO 16,216,1928) and one measurement made with CORAVEL on March, 21, 1990 (RV = -27.2 km/s). System2554Orbit1End System2555Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Three additional velocities from Fick observatory (Beavers & Eitter, 1986ApJS...62..147B) have been used. System2555Orbit1End System842Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. System842Orbit3End System882Orbit5Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Other 15 measurements were taken from Mayor and Mazeh(1987A&A...171..157M) to calculate the orbital elements. The values of e and w have been fixed. System882Orbit5End System2556Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System2556Orbit1End System894Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System894Orbit2End System2213Orbit3Begin PI - The radial velocity was taken from Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Other measurements were taken from Mayor and Turon(1982A&A...110..241M) System2213Orbit3End System969Orbit4Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary SB2 orbit was derived using West data (1966AJ.....71Q.186W). The values e and w have been fixed. System969Orbit4End System2557Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) T0, V0 and e have been fixed. Preliminary orbit. System2557Orbit1End System2558Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary SB1 orbit, using 6 early velocities (LOB 6,140,1911). System2558Orbit1End System1058Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System1058Orbit3End System2559Orbit1Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. T0, e and w have been fixed. System2559Orbit1End System1122Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System1122Orbit2End System1478Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Authors obtained preliminary SB2 orbit with fixed visual elements: T0, e, w. System1478Orbit2End System1438Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) System1438Orbit2End System1468Orbit2Begin PI - the radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Other measurements were taken from Jasniewicz and Mayor (1988A&A...203..329J). Preliminary orbit. T0, e and w have been fixed. System1468Orbit2End System1477Orbit2Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281) Preliminary orbit. SB2 solution with fixed values of T0 and eccentricity. System1477Orbit2End System1477Orbit3Begin The radial velocities have been published in Paper I (Duquennoy A., Mayor M. and Halbwaschs J.-L., 1991, AApS 88, 281). SB1 solution. System1477Orbit3End System2560Orbit1Begin The system HD 111980 includes a third faint component. System2560Orbit1End System2213Orbit4Begin The spectroscopic binary HD 149414 has a faint visual companion, with common proper motion. The first two measurements of Rv are from Sandage (1969, ApJ 158, 1115). They were only used to improve the period. For the determination of the orbital parameters only the new photoelectric measurements were taken into consideration. System2213Orbit4End System2561Orbit1Begin System2561Orbit1End System2562Orbit1Begin System2562Orbit1End System2563Orbit1Begin System2563Orbit1End System2564Orbit1Begin System2564Orbit1End System2565Orbit1Begin System2565Orbit1End System2566Orbit1Begin System2566Orbit1End System2567Orbit1Begin System2567Orbit1End System2568Orbit1Begin System2568Orbit1End System2569Orbit1Begin System2569Orbit1End System2570Orbit1Begin System2570Orbit1End System2571Orbit1Begin System2571Orbit1End System2572Orbit1Begin System2572Orbit1End System2573Orbit1Begin System2573Orbit1End System2574Orbit1Begin System2574Orbit1End System2575Orbit1Begin System2575Orbit1End System2576Orbit1Begin System2576Orbit1End System2577Orbit1Begin System2577Orbit1End System2578Orbit1Begin System2578Orbit1End System2579Orbit1Begin System2579Orbit1End System2580Orbit1Begin System2580Orbit1End System2581Orbit1Begin System2581Orbit1End System2582Orbit1Begin System2582Orbit1End System2583Orbit1Begin System2583Orbit1End System2584Orbit1Begin System2584Orbit1End System2585Orbit1Begin System2585Orbit1End System2586Orbit1Begin System2586Orbit1End System2587Orbit1Begin System2587Orbit1End System2588Orbit1Begin System2588Orbit1End System2110Orbit2Begin System2110Orbit2End System2589Orbit1Begin System2589Orbit1End System2590Orbit1Begin System2590Orbit1End System2591Orbit1Begin System2591Orbit1End System2592Orbit1Begin System2592Orbit1End System2593Orbit1Begin System2593Orbit1End System2594Orbit1Begin System2594Orbit1End System1034Orbit2Begin The observations were carried out with the 1.4m Coude Auxiliary Telescope at ESO's La Silla Observatory in Chile. The value of period was taken from Brunch et al. (1994, A&A, 287, 829) A least squares fit gives the eccentricity equals to 0.04, but a circular orbit provides a better description of the data. System1034Orbit2End System926Orbit3Begin The value of period was calculated using all published data. System926Orbit3End System2595Orbit1Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. Preliminary orbit. System2595Orbit1End System928Orbit2Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. System928Orbit2End System925Orbit3Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. All RVs are commented because the published orbital elements do not match them well. Comment means which component was measured. System925Orbit3End System2596Orbit1Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. Preliminary orbit. System2596Orbit1End System927Orbit3Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. This star is an eclipsing binary and has a third companion with a period estimated to 150 yr. System927Orbit3End System2597Orbit1Begin The orbital elements were calculated using the combination of the literature radial velocities and new observations. Preliminary orbit. System2597Orbit1End System1852Orbit2Begin The radial velocities have been obtained for HeI 4471. V0 of secondary star equals to -46.4+-11.5 km/s. System1852Orbit2End System1852Orbit3Begin The radial velocities have been obtained by a correlation with a synthetic mask. V0 of secondary star equals to -41.6+-3.5 km/s. System1852Orbit3End System927Orbit4Begin The radial velocities have been obtained for He I 4471 absorption lines. The radial velocities for the primary and secondary stars are given in the "zero systemic velocity" reference frame, that is why we put V0 to equal to zero instead of -30.3 km/s to receive the correct figure. V0 of the secondary star equals to -28.7+-4.3 km/s. The spectra was obtained : -with the Boller & Chivens spectrograph fed by the ESO 1.5 m telescope (ESO_1.5+B&C), -with ESO' 1.4 m Coude Auxiliary Telescope using the Coude Echelle Spectrometer equipped with the Long Camera (CAT+CES+LC), -with the Fiber-fed Extended Range Optical Spectrograph attached to the ESO 1.5 m telescope at La Silla (ESO_1.5+FEROS), -with the Bench-Mounted Echelle Spectrograph (BME) attached to the 1.5 m CTIO telescope (CTIO_1.5+BME) System927Orbit4End System927Orbit5Begin In order to combine the RVs obtained from the different lines, the authors had to refer all the RV measurements to a "zero systemic velocity" reference frame: they subtracted the corresponding weighted mean between V0 of primary and V0 of secondary star from the individual RVs of the considered line. Then they computed a weighted RV mean from all RV data obtained at the same observing time. These mean RVs are listed in the table. To receive the correct figure we put V0 to equal to zero instead of 0.2 km/s. V0 of the secondary star equals to 2.6+-3.4 km/s. The spectra was obtained : -with the Boller & Chivens spectrograph fed by the ESO 1.5 m telescope (ESO_1.5+B&C), -with ESO' 1.4 m Coude Auxiliary Telescope using the Coude Echelle Spectrometer equipped with the Long Camera (CAT+CES+LC), -with the Fiber-fed Extended Range Optical Spectrograph attached to the ESO 1.5 m telescope at La Silla (ESO_1.5+FEROS), -with the Bench-Mounted Echelle Spectrograph (BME) attached to the 1.5 m CTIO telescope (CTIO_1.5+BME) System927Orbit5End System2598Orbit1Begin P, T0 and V0 were received from photometric solution of Hipparcos light curve. IUE velocities (JD=2444487.4713 RV1=+101 RV2=-155) give K1 and K2. System2598Orbit1End System1784Orbit2Begin LM means revised radial velocity from spectra by Levato H., Malaroda S. et al. (1991, ApJS 75, 869) System1784Orbit2End System2599Orbit1Begin 1WGA J1958.2+3232 is Intermediate polar (magnetic cataclysmic variable with an asynchronously rotating magnetic white dwarf). The orbital elements were determined by radial velocity curve for the emission line of H_beta. System2599Orbit1End System2599Orbit2Begin 1WGA J1958.2+3232 is Intermediate polar (magnetic cataclysmic variable with an asynchronously rotating magnetic white dwarf). The orbital elements were determined by radial velocity curve for the emission line of HeII 4686. System2599Orbit2End System1409Orbit2Begin An analysis of 1236 new spectra of the eclipsing binary EN Lac and of 994 published radial velocities has allowed authors to disentangle the RV variations due to orbital motion and due to pulsations of the star. New accurate orbital elements as well as precise values of the three pulsation periods (P1, P2, P3) were derived. P1=0.16916703d , P2=0.17085554d, P3=0.18173256d. System1409Orbit2End System1348Orbit3Begin Radial velocities were determined from high-resolution IUE spectra. Velocities are given with respect to an arbitrary zero point (which is within 10 km/s of zero). P has been obtained from unweighted orbit solution to all data: both IUE and published DAO (Petrie R.M., PDAO, 12(3), 111, 1962; Hilditch R.W., M.N., 169, 323, 1974) System1348Orbit3End System2600Orbit1Begin System2600Orbit1End System448Orbit2Begin Eclipsing system in a semidetached configuration, which is a member of the rare class of "cool Algols". The radial velocities for both stars were solved simultaneously with the UBV light curves using the Wilson-Devinney model. Two solutions of very nearly the same quality were obtained, one with and the other without accounting for light from a possible third component. The solution with third light is the preferred one not only because it is marginally better, but because the light ratios derived from the photometry are in better agreement with the spectroscopy (L2/L1 = 1.15 +/- 0.04 at a wavelength close to V) and the predicted synchronous rotational velocities are also in better agreement with the spectroscopically determined values of v1 sin i = 20 +/- 2 km/s v2 sin i = 34 +/- 2 km/s The stellar parameters derived from this solution are also in better agreement with stellar evolution models. The mass ratio is q = 0.2987 +/- 0.0022, and there is an apparent change in period in the amount of dP/dt = (-0.75 +/- 0.30) x 10**(-7). The velocity amplitudes are not reported in the original publication, and have been added here solely for the purpose of allowing a graphical representation of the measurements. System448Orbit2End System2601Orbit1Begin Astrometric-spectroscopic solution that includes lunar occultation measurements and speckle interferometry measurements along with the radial velocities from three sources, aside from CfA: G = Griffin & Gunn (1977), BE = Beavers & Eitter (1986), D = Detweiler et al. (1984). The velocities from Griffin & Gunn listed here are the original values, but an adjustment of -1.0 km/s was applied in the orbital solution to bring them onto the same system as the other measurements. The primary star is one of the giants in the Hyades. The masses of the components were derived by adopting the distance of the nearby binary Theta2 Tau, and are 2.91 +/- 0.88 solar masses for the primary and 1.31 +/- 0.14 solar masses for the secondary. The secondary is 3.5 magnitudes fainter than the primary in V. Other elements of the astrometric-spectroscopic solution are: Semimajor axis of relative orbit = 0.2178 +/- 0.0054 arcsec P.A. of the ascending node (J2000) = 355.54 +/- 0.26 deg The time span of observations (days) = 25.8 yr System2601Orbit1End System2602Orbit1Begin Triple system in which only two stars are visible (star 1 and star 2). They orbit each other with a period of 133 days (outer orbit). The fainter star is itself a single-lined spectroscopic binary with a period of 1.76 days. The companion (star 3) is unseen. Derived quantities in outer orbit: a1 sin i = 31.08 +/- 0.52 million km (a2+a3) sin i = 20.98 +/- 0.66 million km M1 sin**3 i = 0.1271 +/- 0.0079 solar masses (M2+M3) sin**3 i = 0.1883 +/- 0.0088 solar masses q = (M2+M3)/M1 = 1.481 +/- 0.051 Derived quantities in inner orbit: a2 sin i = 0.9605 +/- 0.0087 million km f(M) = 0.01138 +/- 0.00031 solar masses M3 sin i = 0.2249 (M2+M3)**(2/3) Physical parameters are derived as follows: Effective temperature of star 1 = 7000 +/- 150 K Effective temperature of star 2 = 6650 +/- 150 K Projected rotational velocity (v sin i) of star 1 = 19 +/- 2 km/s Projected rotational velocity (v sin i) of star 2 = 17 +/- 2 km/s Time span of observations = 882 days System2602Orbit1End System2603Orbit1Begin Triple system in which only two stars are visible (star 1 and star 2). They orbit each other with a period of 133 days (outer orbit). The fainter star is itself a single-lined spectroscopic binary with a period of 1.76 days. The companion (star 3) is unseen. Derived quantities in outer orbit: a1 sin i = 31.08 +/- 0.52 million km (a2+a3) sin i = 20.98 +/- 0.66 million km M1 sin**3 i = 0.1271 +/- 0.0079 solar masses (M2+M3) sin**3 i = 0.1883 +/- 0.0088 solar masses q = (M2+M3)/M1 = 1.481 +/- 0.051 Derived quantities in inner orbit: a2 sin i = 0.9605 +/- 0.0087 million km f(M) = 0.01138 +/- 0.00031 solar masses M3 sin i = 0.2249 (M2+M3)**(2/3) Physical parameters are derived as follows: Effective temperature of star 1 = 7000 +/- 150 K Effective temperature of star 2 = 6650 +/- 150 K Projected rotational velocity (v sin i) of star 1 = 19 +/- 2 km/s Projected rotational velocity (v sin i) of star 2 = 17 +/- 2 km/s Time span of observations = 882 days System2603Orbit1End System248Orbit3Begin A member of the Hyades cluster. Radial velocities for the secondary component were not derived directly, but the authors were able to determine the velocity amplitude spectroscopically by applying a two-dimensional cross-correlation procedure (see Zucker & Mazeh 1994) and seeking the best match of their spectra to a combination of two templates. In this way they derived K2 and also the projected rotational velocity of the secondary, v2 sin i = 110 +/- 4 km/s. The rotational velocity of the primary is v1 sin i = 70 km/s, and the brightness difference with the secondary is 1.10 mag in V from lunar occultation observations. The combination of these spectroscopic elements with the astrometric elements reported by Pan et al. (1992) yields the masses of the two stars, as well as the orbital parallax: M1 = 2.42 +/- 0.30 solar masses M2 = 2.11 +/- 0.17 solar masses Orbital parallax = 21.22 +/- 0.79 mas Distance = 47.1 +/- 1.7 pc System248Orbit3End System2604Orbit1Begin The system is triple. Derived quantities for inner (double-lined) orbit: M1 (sin i)**3 = 0.6719 +/- 0.0034 Msun M2 (sin i)**3 = 0.6041 +/- 0.0026 Msun q = M2/M1 = 0.8991 +/- 0.0027 a1 sin i = 4.6721 +/- 0.0084 x 10**6 km a2 sin i = 5.1965 +/- 0.0122 x 10**6 km The inclination angle "i" is that of the inner orbit. The center of mass listed corresponds to that of the system as a whole. Derived quantitis for outer orbit (comprising the inner double-lined binary and a more distant third companion): M12 (sin i)**3 = 1.0862 +/- 0.0114 Msun M3 (sin i)**3 = 0.5352 +/- 0.0058 Msun a12 sin i = 27.70 +/- 0.15 x 10**6 km a3 sin i = 56.23 +/- 0.24 x 10**6 km where M12 represents the sum of the two stars in the inner pair. The inclination angle "i" here is that of the outer orbit. Changes in the orbital elements are seen and are due to the three-body interactions. System2604Orbit1End System2605Orbit1Begin The system is triple. Derived quantities for inner (double-lined) orbit: M1 (sin i)**3 = 0.6719 +/- 0.0034 Msun M2 (sin i)**3 = 0.6041 +/- 0.0026 Msun q = M2/M1 = 0.8991 +/- 0.0027 a1 sin i = 4.6721 +/- 0.0084 x 10**6 km a2 sin i = 5.1965 +/- 0.0122 x 10**6 km The inclination angle "i" is that of the inner orbit. The center of mass listed corresponds to that of the system as a whole. Derived quantitis for outer orbit (comprising the inner double-lined binary and a more distant third companion): M12 (sin i)**3 = 1.0862 +/- 0.0114 Msun M3 (sin i)**3 = 0.5352 +/- 0.0058 Msun a12 sin i = 27.70 +/- 0.15 x 10**6 km a3 sin i = 56.23 +/- 0.24 x 10**6 km where M12 represents the sum of the two stars in the inner pair. The inclination angle "i" here is that of the outer orbit. Changes in the orbital elements are seen and are due to the three-body interactions. System2605Orbit1End System14Orbit2Begin Secondary Phase = Primary phase - 0.051 Weights=0 for Vr on HJD 51419.951 and 51491.730. System14Orbit2End System2606Orbit1Begin Triple-lined system in which the inner binary is eclipsing and has been assumed to have a circular orbit. Radial velocities for the three stars were derived using a three-dimensional extension of TODCOR (Zucker & Mazeh 1994). The projected rotational velocities are 36 +/- 2 km/s and 20 +/- 3 km/s for the eclipsing pair, and 2 +/- 3 km/s for the third star. The fraction of the total light contributed by each star is 0.75 for the primary, 0.09 for the secondary, and 0.16 for the tertiary, with estimated uncertainties of 0.01. The inner and outer orbits were solved simultaneously incorporating also times of eclipse as well as measurements from the Hipparcos satellite (intermediate astrometric data). Additional elements depending on the astrometry that were derived from the combined fit are: Inclination angle of outer orbit = 112.0 +/- 4.9 degrees P.A. of the ascending node (J2000) = 27 +/- 44 degrees Semimajor axis of relative orbit = 55.3 +/- 1.8 mas The mass ratio of the inner pair is q = 0.7266 +/- 0.0042. System2606Orbit1End System2607Orbit1Begin Triple-lined system in which the inner binary is eclipsing and has been assumed to have a circular orbit. Radial velocities for the three stars were derived using a three-dimensional extension of TODCOR (Zucker & Mazeh 1994). The projected rotational velocities are 36 +/- 2 km/s and 20 +/- 3 km/s for the eclipsing pair, and 2 +/- 3 km/s for the third star. The fraction of the total light contributed by each star is 0.75 for the primary, 0.09 for the secondary, and 0.16 for the tertiary, with estimated uncertainties of 0.01. The inner and outer orbits were solved simultaneously incorporating also times of eclipse as well as measurements from the Hipparcos satellite (intermediate astrometric data). Additional elements depending on the astrometry that were derived from the combined fit are: Inclination angle of outer orbit = 112.0 +/- 4.9 deg P.A. of the ascending node (J2000) = 27 +/- 44 deg Semimajor axis of relative orbit = 55.3 +/- 1.8 mas The mass ratio of the inner pair is q = 0.7266 +/- 0.0042. System2607Orbit1End System2608Orbit1Begin Eclipsing system. Other spectroscopically derived quantities are: Light ratio L(sec)/L(prim) = 0.528 +/- 0.010 at 5188.5 Angstroms M1 (sin i)**3 = 0.928 +/- 0.006 Msun M2 (sin i)**3 = 0.869 +/- 0.004 Msun q = M2/M1 = 0.9375 +/- 0.0035 Time span = 2.43 years System2608Orbit1End System804Orbit2Begin Radial velocities were obtained using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The system has been spatially resolved with the Palomar Testbed Interferometer (PTI). The orbital elements are the result of a simultaneous fit to the radial velocities and the interferometric visibilities in two passbands (H and K). The simultaneous fit yields the following astrometric parameters: Relative semimajor axis = 3.451 +/- 0.018 mas Inclination angle of the orbit = 107.990 +/- 0.077 degrees P.A. of the ascending node (J2000) = 80.291 +/- 0.079 degrees The light ratio inferred from the spectra is L2/L1 = 0.64 +/- 0.02 at the mean wavelength 5188.5 A. Projected rotational velocities are 14 +/- 1 km/s for the primary and 12 +/- 1 km/s for the secondary. System804Orbit2End System2609Orbit1Begin Eclipsing system most likely in a semidetached configuration, which is probably a member of the rare class of "cool Algols". The radial velocities were obtained with the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The velocities for both stars were solved simultaneously with the BVRI light curves using the Wilson-Devinney model. Two solutions of very nearly the same quality were obtained, one slightly detached and the other semidetached. The projected rotational velocities determined spectroscopically are v1 sin i = 35 +/- 1 km/s v2 sin i = 56 +/- 3 km/s and the spectroscopic light ratio is L2/L1 = 0.25 +/- 0.05 at the mean wavelength of the observations (5188.5 A). An analysis of the existing times of eclipse suggests the period may be changing at a rate of (+0.95 +/- 0.30) 10**(-6) days per year, but this needs to be confirmed. System2609Orbit1End System2274Orbit2Begin Radial velocities were obtained with the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The system has been spatially resolved with the Palomar Testbed Interferometer (PTI). In addition to the velocities, the orbital fit includes interferometric visibilities obtained at two wavelengths (H and K). The simultaneous fit yields the following astrometric parameters: Relative semimajor axis = 4.944 +/- 0.018 mas Inclination angle of the orbit = 61.56 +/- 0.25 degrees P.A. of the ascending node (J2000) = 262.29 +/- 0.20 degrees The light ratio inferred from the spectra is L2/L1 = 0.16 +/- 0.03 at the mean wavelength 5188.5 A. System2274Orbit2End System2610Orbit1Begin In addition to the radial velocities, the orbital solution incorporates intermediate astrometric data (abscissa residuals) from the Hipparcos mission as well as the proper motions from the Tycho-2 catalog. The joint solution yields the following astrometric parameters: Semimajor axis of the photocenter = 14.9 +/- 1.3 mas Inclination angle of the orbit = 83 +/- 15 degrees P.A. of the ascending node (J2000) = 179 +/- 10 degrees A significant correction to the original Hipparcos parallax is also found from this fit, yielding the revised value of 20.6 +/- 1.9 mas. The unseen companion is found to be overmassive (about 20% larger than the primary), and is most likely a closer binary composed of M dwarfs. This is supported by the infrared excess displayed by the system. System2610Orbit1End System2450Orbit2Begin In addition to the radial velocities, the orbital fit includes interferometric visibilities obtained with the Keck Interferometer in the K band. The radial velocities listed here are the same as those reported by Torres et al. (1995) [1995ApJ...452..870T]. The joint astrometric-spectroscopic solution yields the following astrometric parameters: Semimajor axis of the relative orbit = 23.3 +/- 2.5 mas Inclination angle of the orbit = 66.8 +/- 3.2 degrees P.A. of the ascending node (J2000) = 337.6 +/- 2.4 degrees Individual dynamical masses for the components are determined for the first time. The orbital parallax of the system is 23.7 +/- 2.6 mas, and the brightness difference in the K band is determined to be 0.612 +/- 0.046 mag. System2450Orbit2End System253Orbit2Begin Radial velocities were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Other derived quantities of the fit: a1 sin i = 0.984 +/- 0.019 x 10**6 km a2 sin i = 0.988 +/- 0.026 x 10**6 km M1 (sin i)**3 = 0.01013 +/- 0.00057 solar masses M2 (sin i)**3 = 0.01009 +/- 0.00048 solar masses The time span of the observations is 4082 days. System253Orbit2End System1863Orbit3Begin Other derived quantities of the fit: a1 sin i = 232.3 +/- 7.1 x 10**6 km f(M) = 0.0778 +/- 0.0070 solar masses The time span of the observations is 5149 days. System1863Orbit3End System1859Orbit2Begin Other derived quantities of the fit: a1 sin i = 28.9 +/- 3.7 x 10**6 km f(M) = 0.046 +/- 0.017 solar masses The time span of the observations is 1181 days. System1859Orbit2End System1860Orbit2Begin Other derived quantities of the fit: a1 sin i = 2.10 +/- 0.23 x 10**6 km f(M) = 0.0034 +/- 0.0011 solar masses The time span of the observations is 825 days. System1860Orbit2End System2611Orbit1Begin This symbiotic star system is very unusual since the companion of the M5 III is a neutron star rather than a white dwarf. Thus, the system is also an X-ray binary with the X-ray source being known as GX 1+4. The spectroscopic orbit, obtained from velocities of infrared spectra, is for the M giant. The orbital period of 1161 days or 3.2 years is by far the longest of any known X-ray binary. Adopting a mass of 1.35 solar masses for the neutron star, the M giant has a mass of 1.22 solar masses, and so is the less massive component. The M giant does not fill its Roche lobe and has near solar abundances. System2611Orbit1End System2612Orbit1Begin Eclipsing system presenting a hint of apsidal motion from an analysis of available times of eclipse. The negative value of the apsidal motion (corresponding to an apsidal period of perhaps 75 +/- 22 years) would suggest the presence of a third body. This is supported by the non-negligible value of third light derived from the light curve analysis. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second (KPNO) data set were derived with standard one-dimensional cross-correlation techniques. A significant velocity offset ( = -2.98 +/- 0.62 km/s) was found between the two data sets. Other spectroscopically derived quantities: a1 sin i = 2.9848 +/- 0.0069 x 10**6 km a2 sin i = 3.683 +/- 0.015 x 10**6 km (a1+a2) sin i = 9.583 +/- 0.023 solar radii M1 (sin i)**3 = 1.733 +/- 0.015 solar masses M2 (sin i)**3 = 1.404 +/- 0.009 solar masses q = M2/M1 = 0.8105 +/- 0.0037 Both components appear to be metallic-lined. The projected rotational velocities measured are 45.4 +/- 0.9 km/s for the primary and 40.5 +/- 1.4 km/s for the secondary (average of two determinations). System2612Orbit1End System2613Orbit1Begin Eclipsing system. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set (KPNO) were derived with standard one-dimensional cross-correlation techniques. An insignificant velocity offset ( = +0.16 +/- 0.78 km/s) was found between the two data sets. The orbital solution accounts for this, and includes also available times of eclipse simultaneously with the velocities. Other spectroscopically derived quantities: M1 (sin i)**3 = 1.627 +/- 0.012 solar masses M2 (sin i)**3 = 1.458 +/- 0.010 solar masses q = M2/M1 = 0.8959 +/- 0.0042 The projected rotational velocities measured are 52 +/- 2 km/s for the primary and 43 +/- 3 km/s for the secondary (average of two determinations). System2613Orbit1End System2614Orbit1Begin Eclipsing system with an eccentric orbit. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set (KPNO) were derived with standard one-dimensional cross-correlation techniques. An insignificant velocity offset ( = -0.06 +/- 0.36 km/s) was found between the two data sets. The orbital solution accounts for this, and includes also available times of eclipse simultaneously with the velocities. Other spectroscopically derived quantities: a1 sin i = 8.634 +/- 0.0028 x 10**6 km a2 sin i = 8.650 +/- 0.0026 x 10**6 km M1 (sin i)**3 = 2.341 +/- 0.016 solar masses M2 (sin i)**3 = 2.337 +/- 0.017 solar masses q = M2/M1 = 0.9982 +/- 0.0044 Time of periastron passage = 2,449,718.0448 +/- 0.0078 (HJD) The orbital fit indicates a somewhat significant apsidal motion in the amount of dw/dt = 0.00061 +/- 0.00025 degrees per cycle. The corresponding apsidal period is U = 10700 +/- 4500 years. System2614Orbit1End System1313Orbit2Begin Eclipsing system. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The second data consists of the velocities published by Popper (1971). The velocity offset between these two data sets was included as an adjustable parameter in the solution, and was found to be significant: = -0.94 +/- 0.18 km/s. The fit includes also available times of eclipse simultaneously with the velocities. Other spectroscopically derived quantities: a1 sin i = 9.403 +/- 0.0015 x 10**6 km a2 sin i = 8.917 +/- 0.0015 x 10**6 km M1 (sin i)**3 = 1.6742 +/- 0.0062 solar masses M2 (sin i)**3 = 1.7654 +/- 0.0066 solar masses q = M1/M2 = 1.0544 +/- 0.0024 The time of eclipse listed with the other elements is a time of secondary minimum. System1313Orbit2End System2615Orbit1Begin Eclipsing system with a slightly eccentric orbit. Radial velocities for the first data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set (KPNO) were derived with standard one-dimensional cross-correlation techniques. The velocity offset between these two data sets was included as an adjustable parameter in the solution, and was found to be insignificant: = -0.15 +/- 0.38 km/s. Other spectroscopically derived quantities: a1 sin i = 3.897 +/- 0.0019 x 10**6 km a2 sin i = 3.995 +/- 0.0010 x 10**6 km M1 (sin i)**3 = 1.917 +/- 0.013 solar masses M2 (sin i)**3 = 1.870 +/- 0.018 solar masses q = M2/M1 = 0.9755 +/- 0.0053 Time of periastron passage = 2,451,946.949 +/- 0.076 (HJD) Time span of the observations = 17 years. System2615Orbit1End System2616Orbit1Begin Eclipsing system with an eccentric orbit and a small apsidal motion. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set were derived with standard one-dimensional cross-correlation techniques. The velocity offset between these two data sets was included as an adjustable parameter in the solution, and was found to be small: = -0.74 +/- 0.37 km/s. The orbital solution incorporates also the available times of eclipse simultaneously with the velocities. The apsidal motion is found to be dw/dt = 0.00250 +/- 0.00033 degrees per cycle, corresponding to an apsidal period of U = 2810 +/- 360 years. Other spectroscopically derived quantities: a1 sin i = 9.148 +/- 0.0049 x 10**6 km a2 sin i = 9.298 +/- 0.0049 x 10**6 km a sin i = 26.502 +/- 0.074 solar radii M1 (sin i)**3 = 2.332 +/- 0.015 solar masses M2 (sin i)**3 = 2.295 +/- 0.025 solar masses q = M2/M1 = 0.9838 +/- 0.0054 Time of periastron passage = 2,449,947.3607+/- 0.0075 (HJD) The time of eclipse listed with the other elements is a time of secondary minimum. The time span of the combined data sets is 19.2 years. Projected rotational velocities for the components are found to be 45 +/- 1 km/s and 15 +/- 1 km/s for the primary and secondary, respectively. System2616Orbit1End System609Orbit2Begin Eclipsing system with a third, unseen component. Radial velocities were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The orbital solution combines these CfA data with velocities reported by Popper (1971), and solves simultaneously for the inner and outer orbital elements as well as for an offset between the two velocity data sets. This offset is found to be small: = -1.06 +/- 0.72 km/s. Other spectroscopically derived properties: a sin i = 7.656 +/- 0.014 solar radii M1 (sin i)**3 = 1.2439 +/- 0.0077 solar masses M2 (sin i)**3 = 1.2077 +/- 0.0069 solar masses q = M2/M1 = 0.9709 +/- 0.0038 Mass function of outer orbit f(M) = 0.0151 +/- 0.0014 solar masses The projected rotational velocities are measured to be 42 and 41 km/s for the primary and secondary, respectively, with estimated errors of 2-3 km/s. These are consistent with synchronous rotation. Although the third object is not directly detected spectroscopically, its signature is revealed in the light curves in the form of third light. It is most likely an M0 dwarf with an estimated minimum mass of about 0.51 solar masses. System609Orbit2End System2617Orbit1Begin Eclipsing system with a third, unseen component. Radial velocities were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The orbital solution combines these CfA data with velocities reported by Popper (1971), and solves simultaneously for the inner and outer orbital elements as well as for an offset between the two velocity data sets. This offset is found to be small: = -1.06 +/- 0.72 km/s. Other spectroscopically derived properties: a sin i = 7.656 +/- 0.014 solar radii M1 (sin i)**3 = 1.2439 +/- 0.0077 solar masses M2 (sin i)**3 = 1.2077 +/- 0.0069 solar masses q = M2/M1 = 0.9709 +/- 0.0038 Mass function of outer orbit f(M) = 0.0151 +/- 0.0014 solar masses The projected rotational velocities are measured to be 42 and 41 km/s for the primary and secondary, respectively, with estimated errors of 2-3 km/s. These are consistent with synchronous rotation. Although the third object is not directly detected spectroscopically, its signature is revealed in the light curves in the form of third light. It is most likely an M0 dwarf with an estimated minimum mass of about 0.51 solar masses. System2617Orbit1End System232Orbit3Begin Member of the Hyades cluster with a history of spectroscopic and astrometric observations. Velocities for the primary component have been notoriously difficult to measure. New radial velocities from CfA for both stars were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Additionally published velocities by Deutsch et al. (1971) for the secondary component were used. The elements listed correspond to a joint astrometric-spectroscopic orbital solution that combines radial velocities with speckle interferometric measurements. A velocity offset between the two radial-velocity data sets was included as an adjustable parameter in the solution, and was found to be very small: = -0.43 +/- 0.26 km/s. The remaining elements of the combined solution are: Semimajor axis of relative orbit = 0.13393 +/- 0.00096 arc seconds Position angle of ascending node (J2000) = 350.77 +/- 0.45 degrees Inclination angle = 125.08 +/- 0.50 degrees Derived quantities: Orbital parallax = 17.92 +/- 0.58 milli arc seconds M1 = 1.80 +/- 0.13 solar masses M2 = 1.46 +/- 0.18 solar masses The time span of the combined data sets is 44.2 years. System232Orbit3End System2618Orbit1Begin Eclipsing system with a slightly eccentric orbit. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set (CHSL) were derived with standard one-dimensional cross-correlation techniques. The velocity offset between these two sets was included as an adjustable parameter in the solution, and was found to be insignificant: = +0.5 +/- 0.7 km/s. Other spectroscopically derived quantities: a1 sin i = 0.03352 +/- 0.00009 AU a2 sin i = 0.03359 +/- 0.00009 AU M1 (sin i)**3 = 1.329 +/- 0.010 solar masses M2 (sin i)**3 = 1.327 +/- 0.008 solar masses q = M2/M1 = 0.998 +/- 0.004 Previous reports of Delta Scuti variations are not confirmed. There is a hint of apsidal motion in the system, but it is very poorly determined with the data available. System2618Orbit1End System2619Orbit1Begin Eclipsing system with an eccentric orbit. Radial velocities for the first and more numerous data set (CfA) were derived using the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). Those for the second data set (KPNO) were derived with standard one-dimensional cross-correlation techniques. The velocity offset between these two sets was included as an adjustable parameter in the solution, and was found to be insignificant: = -0.40 +/- 0.48 km/s. Times of eclipse were also included in the solution. Other quantities derived from the orbital solution: a sin i = 24.29 +/- 0.06 solar radii M1 (sin i)**3 = 1.526 +/- 0.009 solar masses M2 (sin i)**3 = 1.502 +/- 0.014 solar masses q = M2/M1 = 0.9839 +/- 0.0049 Time of periastron passage = 2,450,322.9770 +/- 0.0018 (HJD) Time of primary eclipse = 2,452,339.60834 +/- 0.00010 (HJD) Time of secondary eclipse = 2,452,342.76452 +/- 0.00017 (HJD) System2619Orbit1End System2620Orbit1Begin System2620Orbit1End System2621Orbit1Begin System2621Orbit1End System2622Orbit1Begin System2622Orbit1End System2623Orbit1Begin System2623Orbit1End System2624Orbit1Begin System2624Orbit1End System2625Orbit1Begin System2625Orbit1End System2626Orbit1Begin System2626Orbit1End System2627Orbit1Begin System2627Orbit1End System2628Orbit1Begin System2628Orbit1End System2629Orbit1Begin System2629Orbit1End System2295Orbit2Begin System2295Orbit2End System2630Orbit1Begin System2630Orbit1End System2631Orbit1Begin System2631Orbit1End System2632Orbit1Begin System2632Orbit1End System2633Orbit1Begin System2633Orbit1End System2634Orbit1Begin System2634Orbit1End System2635Orbit1Begin Epochs in HMJD System2635Orbit1End System2636Orbit1Begin Epochs in HMJD System2636Orbit1End System2637Orbit1Begin Epochs in HMJD System2637Orbit1End System2638Orbit1Begin Epochs in HMJD System2638Orbit1End System2639Orbit1Begin System2639Orbit1End System2640Orbit1Begin System2640Orbit1End System2641Orbit1Begin System2641Orbit1End System2642Orbit1Begin System2642Orbit1End System2643Orbit1Begin System2643Orbit1End System2644Orbit1Begin System2644Orbit1End System2645Orbit1Begin System2645Orbit1End System2646Orbit1Begin System2646Orbit1End System292Orbit2Begin System292Orbit2End System2647Orbit1Begin System2647Orbit1End System2648Orbit1Begin System2648Orbit1End System2649Orbit1Begin System2649Orbit1End System2650Orbit1Begin System2650Orbit1End System1468Orbit3Begin System1468Orbit3End System2651Orbit1Begin System2651Orbit1End System2652Orbit1Begin System2652Orbit1End System2653Orbit1Begin The gamma velocity is given at MJD 50000. It rises by 0.580+/-0.021 km/s per 1000 days, so at (MJD) time t, V0=-25.79+(0.580+/-0.021)((t-50000)/10000) km/s. That correction is not included in the radial velocities but applied on the fly when the plot is generated. System2653Orbit1End System2654Orbit1Begin System2654Orbit1End System2655Orbit1Begin System2655Orbit1End System2656Orbit1Begin System2656Orbit1End System2657Orbit1Begin System2657Orbit1End System2658Orbit1Begin System2658Orbit1End System2659Orbit1Begin System2659Orbit1End System2660Orbit1Begin System2660Orbit1End System2661Orbit1Begin System2661Orbit1End System2662Orbit1Begin System2662Orbit1End System2663Orbit1Begin System2663Orbit1End System2664Orbit1Begin System2664Orbit1End System2665Orbit1Begin System2665Orbit1End System2635Orbit2Begin System2635Orbit2End System2666Orbit1Begin System2666Orbit1End System2667Orbit1Begin System2667Orbit1End System2625Orbit2Begin System2625Orbit2End System2668Orbit1Begin System2668Orbit1End System2669Orbit1Begin System2669Orbit1End System2636Orbit2Begin System2636Orbit2End System2670Orbit1Begin System2670Orbit1End System2671Orbit1Begin System2671Orbit1End System2672Orbit1Begin System2672Orbit1End System2673Orbit1Begin System2673Orbit1End System2674Orbit1Begin System2674Orbit1End System2675Orbit1Begin System2675Orbit1End System2637Orbit2Begin System2637Orbit2End System2676Orbit1Begin System2676Orbit1End System2677Orbit1Begin System2677Orbit1End System2626Orbit2Begin System2626Orbit2End System2678Orbit1Begin System2678Orbit1End System2638Orbit2Begin System2638Orbit2End System2679Orbit1Begin System2679Orbit1End System2680Orbit1Begin System2680Orbit1End System2628Orbit2Begin System2628Orbit2End System2681Orbit1Begin System2681Orbit1End System1658Orbit2Begin System1658Orbit2End System1659Orbit2Begin Although the orbit appears in that paper, it essentially dupplicates what was published in 2001Obs...121..315G. The radial velocities are taken from the latter. In the paper, V0 is given as 16.34 which is the systemic velocity of the triple star. System1659Orbit2End System2682Orbit1Begin No radial velocity published yet for this suspected triple star. System2682Orbit1End System2339Orbit2Begin System2339Orbit2End System1662Orbit2Begin Although the orbit appears in that paper, it essentially dupplicates what was published in 2001Obs...121...55G. The radial velocities are taken from the latter. System1662Orbit2End System2683Orbit1Begin Triple system composed of M dwarfs, in which all three stars are visible in the spectra. Two sets of velocities were derived from the same spectra using somewhat different procedures and different implementations of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The velocities and elements presented here are from the Tel Aviv analysis. The final elements adopted for the system are the average of the elements from the separate Tel Aviv and CfA analyses, and are: Outer orbit P = 625.8 +/- 1.3 days gamma = +15.10 +/- 0.21 km/s K1 = 4.60 +/- 0.22 km/s K2 = 2.95 +/- 0.28 km/s e = 0.053 +/- 0.028 w = 298 +/- 27 deg T = 2,447,208 +/- 45 (HJD) Inner orbit P = 2.965522 +/- 0.000014 days K1 = 17.01 +/- 0.20 km/s K2 = 18.77 +/- 0.23 km/s e = 0.026 +/- 0.007 w = 166 +/- 16 deg T = 2,447,337.30 +/- 0.14 (HJD) Spectroscopic light ratios (mean wavelength = 5187 Angstroms): L(Ba)/L(A) = 0.566 +/- 0.034 L(Bb)/L(A) = 0.358 +/- 0.024 System2683Orbit1End System2683Orbit2Begin Triple system composed of M dwarfs, in which all three stars are visible in the spectra. Two sets of velocities were derived from the same spectra using somewhat different procedures and different implementations of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The velocities and elements presented here are from the CfA analysis. The final elements adopted for the system are the average of the elements from the separate Tel Aviv and CfA analyses, and are: Outer orbit P = 625.8 +/- 1.3 days gamma = +15.10 +/- 0.21 km/s K1 = 4.60 +/- 0.22 km/s K2 = 2.95 +/- 0.28 km/s e = 0.053 +/- 0.028 w = 298 +/- 27 deg T = 2,447,208 +/- 45 (HJD) Inner orbit P = 2.965522 +/- 0.000014 days K1 = 17.01 +/- 0.20 km/s K2 = 18.77 +/- 0.23 km/s e = 0.026 +/- 0.007 w = 166 +/- 16 deg T = 2,447,337.30 +/- 0.14 (HJD) Spectroscopic light ratios (mean wavelength = 5187 Angstroms): L(Ba)/L(A) = 0.566 +/- 0.034 L(Bb)/L(A) = 0.358 +/- 0.024 System2683Orbit2End System2684Orbit1Begin Triple system composed of M dwarfs, in which all three stars are visible in the spectra. Two sets of velocities were derived from the same spectra using somewhat different procedures and different implementations of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The velocities and elements presented here are from the Tel Aviv analysis. The final elements adopted for the system are the average of the elements from the separate Tel Aviv and CfA analyses, and are: Outer orbit P = 625.8 +/- 1.3 days gamma = +15.10 +/- 0.21 km/s K1 = 4.60 +/- 0.22 km/s K2 = 2.95 +/- 0.28 km/s e = 0.053 +/- 0.028 w = 298 +/- 27 deg T = 2,447,208 +/- 45 (HJD) Inner orbit P = 2.965522 +/- 0.000014 days K1 = 17.01 +/- 0.20 km/s K2 = 18.77 +/- 0.23 km/s e = 0.026 +/- 0.007 w = 166 +/- 16 deg T = 2,447,337.30 +/- 0.14 (HJD) Spectroscopic light ratios (mean wavelength = 5187 Angstroms): L(Ba)/L(A) = 0.566 +/- 0.034 L(Bb)/L(A) = 0.358 +/- 0.024 System2684Orbit1End System2684Orbit2Begin Triple system composed of M dwarfs, in which all three stars are visible in the spectra. Two sets of velocities were derived from the same spectra using somewhat different procedures and different implementations of the two-dimensional cross-correlation algorithm TODCOR (Zucker & Mazeh 1994). The velocities and elements presented here are from the CfA analysis. The final elements adopted for the system are the average of the elements from the separate Tel Aviv and CfA analyses, and are: Outer orbit P = 625.8 +/- 1.3 days gamma = +15.10 +/- 0.21 km/s K1 = 4.60 +/- 0.22 km/s K2 = 2.95 +/- 0.28 km/s e = 0.053 +/- 0.028 w = 298 +/- 27 deg T = 2,447,208 +/- 45 (HJD) Inner orbit P = 2.965522 +/- 0.000014 days K1 = 17.01 +/- 0.20 km/s K2 = 18.77 +/- 0.23 km/s e = 0.026 +/- 0.007 w = 166 +/- 16 deg T = 2,447,337.30 +/- 0.14 (HJD) Spectroscopic light ratios (mean wavelength = 5187 Angstroms): L(Ba)/L(A) = 0.566 +/- 0.034 L(Bb)/L(A) = 0.358 +/- 0.024 System2684Orbit2End System2685Orbit1Begin The primary of this short-period binary is slowly rotating and has solar abundances. Such abundances make the primary highly unusual because slowly rotating A-type stars almost always have spectrum peculiarities, being classified as either Ap or Am stars. The unseen secondary is likely a K or M dwarf. System2685Orbit1End System2686Orbit1Begin The star is an eclipsing binary with masses of 1.513 and 1.285 solar masses for the F2 dwarf primary and F5 dwarf secondary, respectively. The age of the system is about 1.2 billion years. Value of T is not a time of periastron but is T_0, a time of maximum velocity of the primary. System2686Orbit1End System2687Orbit1Begin The system is a symbiotic binary consisting of a M giant and a probable hot compact companion. The large value of the mass function suggests that this system may be eclipsing. System2687Orbit1End System2688Orbit1Begin The system is a symbiotic binary consisting of an M giant and a probable hot compact companion. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. System2688Orbit1End System2689Orbit1Begin The system is a symbiotic binary consisting of an M giant and a probable hot compact companion. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. System2689Orbit1End System2690Orbit1Begin System2690Orbit1End System2691Orbit1Begin System2691Orbit1End System2692Orbit1Begin System2692Orbit1End System2693Orbit1Begin System2693Orbit1End System2694Orbit1Begin System2694Orbit1End System2695Orbit1Begin System2695Orbit1End System2696Orbit1Begin System2696Orbit1End System17Orbit2Begin System17Orbit2End System120Orbit3Begin System120Orbit3End System2473Orbit2Begin System2473Orbit2End System352Orbit3Begin System352Orbit3End System429Orbit2Begin He II lines only System429Orbit2End System2697Orbit1Begin System2697Orbit1End System2698Orbit1Begin System2698Orbit1End System2699Orbit1Begin System2699Orbit1End System2700Orbit1Begin System2700Orbit1End System2701Orbit1Begin System2701Orbit1End System2702Orbit1Begin System2702Orbit1End System2703Orbit1Begin System2703Orbit1End System2704Orbit1Begin System2704Orbit1End System2705Orbit1Begin System2705Orbit1End System2256Orbit2Begin System2256Orbit2End System2706Orbit1Begin System2706Orbit1End System2707Orbit1Begin System2707Orbit1End System2708Orbit1Begin System2708Orbit1End System243Orbit2Begin System243Orbit2End System2709Orbit1Begin System2709Orbit1End System2279Orbit2Begin System2279Orbit2End System2710Orbit1Begin System2710Orbit1End System693Orbit2Begin System693Orbit2End System2672Orbit2Begin System2672Orbit2End System2711Orbit1Begin System2711Orbit1End System2712Orbit1Begin System2712Orbit1End System2713Orbit1Begin System2713Orbit1End System2714Orbit1Begin System2714Orbit1End System2715Orbit1Begin System2715Orbit1End System1637Orbit2Begin System1637Orbit2End System2716Orbit1Begin System2716Orbit1End System2717Orbit1Begin System2717Orbit1End System2718Orbit1Begin System2718Orbit1End System2719Orbit1Begin System2719Orbit1End System2720Orbit1Begin System2720Orbit1End System2007Orbit2Begin System2007Orbit2End System2721Orbit1Begin System2721Orbit1End System2722Orbit1Begin System2722Orbit1End System1405Orbit2Begin T0 is the time of the secondary minimum. System1405Orbit2End System1451Orbit2Begin System1451Orbit2End System173Orbit2Begin System173Orbit2End System2723Orbit1Begin System2723Orbit1End System2724Orbit1Begin This orbit is very preliminary and no RV could confidently be derived. System2724Orbit1End System770Orbit2Begin System770Orbit2End System631Orbit3Begin System631Orbit3End System1232Orbit2Begin The WR component is treated as the secondary. System1232Orbit2End System2725Orbit1Begin System2725Orbit1End System1907Orbit2Begin System1907Orbit2End System2726Orbit1Begin System2726Orbit1End System1912Orbit2Begin System1912Orbit2End System2026Orbit2Begin System2026Orbit2End System2727Orbit1Begin System2727Orbit1End System2728Orbit1Begin System2728Orbit1End System2729Orbit1Begin System2729Orbit1End System1904Orbit2Begin System1904Orbit2End System573Orbit2Begin System573Orbit2End System2730Orbit1Begin System2730Orbit1End System91Orbit2Begin System91Orbit2End System2731Orbit1Begin System2731Orbit1End System2732Orbit1Begin System2732Orbit1End System1992Orbit2Begin System1992Orbit2End System222Orbit2Begin System222Orbit2End System202Orbit2Begin System202Orbit2End System2733Orbit1Begin System2733Orbit1End System2734Orbit1Begin System2734Orbit1End System2735Orbit1Begin System2735Orbit1End System464Orbit2Begin System464Orbit2End System2736Orbit1Begin System2736Orbit1End System2737Orbit1Begin System2737Orbit1End System2738Orbit1Begin System2738Orbit1End System2739Orbit1Begin System2739Orbit1End System2740Orbit1Begin System2740Orbit1End System2741Orbit1Begin System2741Orbit1End System2742Orbit1Begin System2742Orbit1End System2743Orbit1Begin System2743Orbit1End System2744Orbit1Begin System2744Orbit1End System2745Orbit1Begin System2745Orbit1End System2746Orbit1Begin System2746Orbit1End System1092Orbit4Begin The paper gives several systemic velocities at different epochs. The one adopted for SB9 is based on the data accumulated by Batten and Fletcher (1975). A period derivative, dP/dt, of 5.9966e-7 was also assumed. System1092Orbit4End System2747Orbit1Begin System2747Orbit1End System2748Orbit1Begin System2748Orbit1End System2749Orbit1Begin System2749Orbit1End System2750Orbit1Begin System2750Orbit1End System2751Orbit1Begin System2751Orbit1End System790Orbit2Begin System790Orbit2End System2752Orbit1Begin System2752Orbit1End System2753Orbit1Begin System2753Orbit1End System118Orbit2Begin Adopting some spectroscopic elements, an astrometric orbit with the Hipparcos data resulted in an orbital inclination of 110 degrees. Lines of the secondary were not seen at red wavelengths. The spectral type of the secondary is estimated to be M0V. System118Orbit2End System2754Orbit1Begin System2754Orbit1End System2755Orbit1Begin System2755Orbit1End System2756Orbit1Begin System2756Orbit1End System2757Orbit1Begin System2757Orbit1End System2758Orbit1Begin System2758Orbit1End System2759Orbit1Begin System2759Orbit1End System2760Orbit1Begin System2760Orbit1End System2761Orbit1Begin System2761Orbit1End System2762Orbit1Begin System2762Orbit1End System2763Orbit1Begin System2763Orbit1End System2764Orbit1Begin System2764Orbit1End System2765Orbit1Begin System2765Orbit1End System2766Orbit1Begin System2766Orbit1End System2767Orbit1Begin System2767Orbit1End System2768Orbit1Begin System2768Orbit1End System2769Orbit1Begin System2769Orbit1End System2770Orbit1Begin The David Dunlap Observatory (DDO) radial velocities of component A were used in a joint solution with the Kitt Peak National Observatory (KPNO) velocities of components A and B to determine the orbital period. That period was then fixed and only the KPNO velocities were used to determine the rest of the orbital elements. Both stars are chromospherically active. Based on the Hipparcos parallax and the derived magnitude differences, both components are approximately 1 mag above the zero-age main sequence, a result that is inconsistent with the assumption that the components are coeval. System2770Orbit1End System2771Orbit1Begin All dates and epochs in MJD System2771Orbit1End System2772Orbit1Begin All dates and epochs in MJD System2772Orbit1End System2773Orbit1Begin All dates and epochs in MJD System2773Orbit1End System2774Orbit1Begin All dates and epochs in MJD System2774Orbit1End System2775Orbit1Begin All dates and epochs in MJD System2775Orbit1End System2776Orbit1Begin All dates and epochs in MJD System2776Orbit1End System2777Orbit1Begin All dates and epochs in MJD System2777Orbit1End System2778Orbit1Begin All dates and epochs in MJD System2778Orbit1End System2779Orbit1Begin All dates and epochs in MJD System2779Orbit1End System2780Orbit1Begin All dates and epochs in MJD System2780Orbit1End System2781Orbit1Begin All dates and epochs in MJD System2781Orbit1End System2782Orbit1Begin All dates and epochs in MJD System2782Orbit1End System2783Orbit1Begin All dates and epochs in MJD System2783Orbit1End System2784Orbit1Begin All dates and epochs in MJD System2784Orbit1End System2785Orbit1Begin All dates and epochs in MJD System2785Orbit1End System2786Orbit1Begin All dates and epochs in MJD System2786Orbit1End System2787Orbit1Begin All dates and epochs in MJD System2787Orbit1End System2788Orbit1Begin All dates and epochs in MJD System2788Orbit1End System2789Orbit1Begin All dates and epochs in MJD System2789Orbit1End System2790Orbit1Begin All dates and epochs in MJD System2790Orbit1End System2791Orbit1Begin All dates and epochs in MJD System2791Orbit1End System2792Orbit1Begin All dates and epochs in MJD System2792Orbit1End System2793Orbit1Begin All dates and epochs in MJD System2793Orbit1End System2794Orbit1Begin All dates and epochs in MJD System2794Orbit1End System2795Orbit1Begin All dates and epochs in MJD System2795Orbit1End System2796Orbit1Begin All dates and epochs in MJD System2796Orbit1End System2797Orbit1Begin All dates and epochs in MJD System2797Orbit1End System2798Orbit1Begin All dates and epochs in MJD System2798Orbit1End System2799Orbit1Begin All dates and epochs in MJD System2799Orbit1End System2800Orbit1Begin MSO = Mt. Stromlo Observatory, Gemini S = Gemini South telescope at Cerro Pachon, KPNO = Kitt Peak National Observatory The listed orbit was computed from just the radial velocities. The criteria of Lucy & Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. A second orbit that combined the radial velocities with six line polarization observations from spectropolarimetry reduced orbital period to 1398 days. This combined orbit resulted in an orbital inclination of 94.3 +/- 1.4 deg. The system is a symbiotic star consisting of an M6.5 giant on the asymptotic giant branch and a presumed white dwarf. Eclipses were found in data from the Harvard College Observatory plate archives. The He II emission feature near 1.0123 microns is associated with the hot component, but the orbit that is produced by the emission line radial velocities does not lead to masses that are consistent with other results. System2800Orbit1End System2801Orbit1Begin MSO = Mt. Stromlo Observatory, Gemini S = Gemini South telescope at Cerro Pachon, KPNO = Kitt Peak National Observatory The listed orbit was computed from just the radial velocities. A second orbit that combined the radial velocities with six line polarization observations from spectropolarimetry reduced orbital period to 898 days. This combined orbit resulted in an orbital inclination of 96.7 +/- 7.1 deg. The system is a symbiotic star consisting of an M6 giant on the asymptotic giant branch and a presumed white dwarf. The system is predicted to eclipse. The He II emission feature near 1.0123 microns is associated with the hot component, but the orbit that is produced by the emission line radial velocities does not lead to masses that are consistent with other results. System2801Orbit1End System892Orbit2Begin System892Orbit2End System455Orbit2Begin System455Orbit2End System2802Orbit1Begin This binary is the primary component of a close visual double star, making the system triple. The spectroscopic binary primary is a chromospherically active star with extensive star spot coverage. The system also has partial eclipses, and a simultaneous solution of the spectroscopic and photometric observations results in an inclination of 81.8 deg. A circular orbit has been adopted. Thus, the value of T is NOT a time of periastron passage but is T_0, a time of maximum positive velocity. System2802Orbit1End System2803Orbit1Begin The semiamplitude of 46.6 listed in the original paper is a typographical error. However, the mass ratio and minimum masses in that paper are correct. The primary is a gamma Doradus variable. System2803Orbit1End System251Orbit2Begin Telescope code: MtW = Mt Wilson; Pal = Palomar 200-inch; Cam = Cambridge 36-inch; 2.7 = McDonald 2.7-m; 2.1 = McDonald 2.1-m. System251Orbit2End System468Orbit2Begin System468Orbit2End System1393Orbit2Begin System1393Orbit2End System1447Orbit2Begin System1447Orbit2End System240Orbit2Begin Telescope code: MtW = Mt Wilson; Cam = Cambridge 36-inch; Pal = Palomar 200-inch; Cor = Coravel; V = Victoria; 2.7 = McDonald 2.7-m; 2.1 = McDonald 2.1-m; KP = Kitt Peak coude feed. System240Orbit2End System397Orbit2Begin System397Orbit2End System804Orbit3Begin System804Orbit3End System911Orbit2Begin System911Orbit2End System2804Orbit1Begin The systemic velocity is give for JD 53371.0. A trend of +1.16km/s/(1000d) is ajusted for in the plot. That trend was not applied for the old obser- vations (i.e. prior to 2002). Instead, a correction of -4.7, -4.0 and -0.7 km/s was applied to the 1986, 1988 and 1997/8 data respectively. System2804Orbit1End System2805Orbit1Begin The systemic velocity is give for JD 53371.0. A trend of +2.09km/s/(1000d) is ajusted for in the plot. That trend was not applied for the old obser- vations (i.e. prior to 2001). Instead, a correction of -0.7, -7.4, -45 and -54 km/s was applied to the 2000, 1986/7, 1945/6, and 1933 data respectively. System2805Orbit1End System2806Orbit1Begin System2806Orbit1End System2807Orbit1Begin System2807Orbit1End System2808Orbit1Begin System2808Orbit1End System2809Orbit1Begin System2809Orbit1End System2810Orbit1Begin System2810Orbit1End System2811Orbit1Begin System2811Orbit1End System2812Orbit1Begin System2812Orbit1End System2813Orbit1Begin System2813Orbit1End System2814Orbit1Begin System2814Orbit1End System2669Orbit2Begin System2669Orbit2End System2670Orbit2Begin System2670Orbit2End System2681Orbit2Begin System2681Orbit2End System2815Orbit1Begin System2815Orbit1End System2816Orbit1Begin System2816Orbit1End System2817Orbit1Begin System2817Orbit1End System2818Orbit1Begin System2818Orbit1End System2819Orbit1Begin System2819Orbit1End System2820Orbit1Begin System2820Orbit1End System2821Orbit1Begin System2821Orbit1End System2822Orbit1Begin System2822Orbit1End System2823Orbit1Begin System2823Orbit1End System2824Orbit1Begin System2824Orbit1End System2825Orbit1Begin System2825Orbit1End System2826Orbit1Begin System2826Orbit1End System2827Orbit1Begin System2827Orbit1End System2828Orbit1Begin System2828Orbit1End System309Orbit2Begin System309Orbit2End System2829Orbit1Begin System2829Orbit1End System1081Orbit2Begin System1081Orbit2End System2830Orbit1Begin System2830Orbit1End System2831Orbit1Begin System2831Orbit1End System2832Orbit1Begin System2832Orbit1End System2833Orbit1Begin System2833Orbit1End System2834Orbit1Begin System2834Orbit1End System612Orbit2Begin System612Orbit2End System2835Orbit1Begin System2835Orbit1End System2836Orbit1Begin System2836Orbit1End System2837Orbit1Begin System2837Orbit1End System2838Orbit1Begin System2838Orbit1End System2839Orbit1Begin System2839Orbit1End System2840Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2840Orbit1End System45Orbit3Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System45Orbit3End System2841Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2841Orbit1End System239Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System239Orbit2End System2601Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2601Orbit2End System2842Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2842Orbit1End System271Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System271Orbit2End System2006Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2006Orbit2End System2843Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2843Orbit1End System2844Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2844Orbit1End System470Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System470Orbit2End System2845Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2845Orbit1End System2846Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2846Orbit1End System2847Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2847Orbit1End System607Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System607Orbit2End System627Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System627Orbit2End System690Orbit4Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System690Orbit4End System693Orbit3Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System693Orbit3End System719Orbit3Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System719Orbit3End System735Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Southeastern component of a visual binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System735Orbit2End System2350Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2350Orbit2End System812Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System812Orbit2End System2848Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2848Orbit1End System2849Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2849Orbit1End System840Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System840Orbit2End System2829Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2829Orbit2End System907Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System907Orbit2End System2850Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2850Orbit1End System2851Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2851Orbit1End System1046Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1046Orbit2End System2852Orbit1Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2852Orbit1End System1396Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1396Orbit2End System1402Orbit4Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1402Orbit4End System1450Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1450Orbit2End System377Orbit2Begin Telescope flags (tel): W = Wyeth reflector, T = Tillinghast reflector, M = MMT The system is a double-lined hierarchical triple system. The orbit and velocities reported correspond to the inner binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System377Orbit2End System50Orbit3Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System50Orbit3End System2853Orbit1Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2853Orbit1End System112Orbit2Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System112Orbit2End System169Orbit4Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System169Orbit4End System580Orbit3Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System580Orbit3End System734Orbit2Begin Northwestern component of a visual binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System734Orbit2End System1510Orbit2Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1510Orbit2End System875Orbit2Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System875Orbit2End System1168Orbit3Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1168Orbit3End System1291Orbit3Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1291Orbit3End System2854Orbit1Begin Triple-lined hierarchical triple. Star 1 and 2 form the double-lined binary, and the velocity of the third star seems constant. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2854Orbit1End System2855Orbit1Begin Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System2855Orbit1End System2856Orbit1Begin Velocities for observations with blended components were given zero weight. The criteria of Lucy and Sweeney (1971, AJ, 76, 544) indicate that the circular-orbit solution is to be prefered over the eccentric-orbit solution. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. System2856Orbit1End System2857Orbit1Begin The SB orbit refers to the B-component of the 6.8" visual binary STF 1466 = ADS 7902. MtW - RV from Mount Wilson (Abt, 1970) DAO - RV from DAO (Plaskett et al., 1921) System2857Orbit1End System1528Orbit2Begin Improvement of the orbit published in 2001A&A...374..227T. Data of Struve & Zebergs (1959 AJ 64 219) are used with a correction of -1.8 km/s (marked 'Struve'). The visual secondary B = HD 139460 at 11.8" is physical and has a constant radial velocity of 1.2 +- 0.1 km/s. System1528Orbit2End System2858Orbit1Begin COR - CORAVEL data (de Medeiros & Mayor, 1999). The Aab system is SB, also resolved by speckle as CHR 194. Preliminary visual elements to complement the spectroscopic orbit are: a=37.3 +- 1.6 mas, node=330 +-5 deg., incination 50 +- 10 deg. The resolved photometry of Aa,Ab is based on speckle results. The AB system of 0.7" separation is Kui 80. The omega originally published (329.9+/-4.5) was wrong. System2858Orbit1End System2859Orbit1Begin The SB orbit refers to the B-component of ADS 16676, at 10" from A. The orbit is preliminary. System2859Orbit1End System2860Orbit1Begin A preliminary orbit based on historical RV data from Mt. Wilson (MtW, Abt, 1973) and Pulkova (Albitsky & Shain, 1933). System2860Orbit1End System75Orbit3Begin Published data of two previous studies are incorporated in the common solution with offsets +1.2km/s (Wright & Pugh, 1954, PDAO, 9, 407), 0.0km/s (Mayor & Mazeh, 1987, A&A, 171, 157) and -2.0km/s (present data), a total of 90 points. The data are listed without offsets. A faint visual companion was found with adaptive optics in 2004. System75Orbit3End System2861Orbit1Begin Combined visual-spectroscopic orbit. RVM - Radial-Velocity Meter, the rest is CORAVEL. 0-weight data not included in the orbital fit. System2861Orbit1End System572Orbit2Begin Given the extremely small eccentricity found for the eccentric-orbit solution, a circular-orbit solution was adopted. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Fekel et al. confirm the large minimum masses of the Am star components, determined by Heard and Hurkens (1973, JRASC, 67, 306) but find that the more massive star is the hotter component. The primary is synchronously rotating, while the secondary is possibly synchronously rotating. System572Orbit2End System981Orbit3Begin Given the extremely small eccentricity found for the eccentric-orbit solution, a circular-orbit solution was adopted. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Fekel et al. find that the primary is an Am star, but the A9 secondary has normal abundances. The primary is synchronously rotating, while the secondary is possibly also synchronously rotating. System981Orbit3End System1045Orbit2Begin Given the extremely small eccentricity found for the eccentric-orbit solution, a circular-orbit solution was adopted. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Fekel et al. find that the value of the period given by Abt and Levy (1985, ApJS, 59, 229) is inconsistent with their primary velocities. The mass ratio of Fekel et al. is similar to the value found by Abt and Levy(1985), but the minimum masses of Fekel et al. are more than 20 per cent larger. Both components are synchronously rotating. System1045Orbit2End System2862Orbit1Begin System2862Orbit1End System2863Orbit1Begin System2863Orbit1End System2864Orbit1Begin System2864Orbit1End System1972Orbit3Begin System1972Orbit3End System1973Orbit3Begin System1973Orbit3End System1974Orbit3Begin System1974Orbit3End System1975Orbit3Begin System1975Orbit3End System1976Orbit3Begin System1976Orbit3End System2865Orbit1Begin System2865Orbit1End System2866Orbit1Begin System2866Orbit1End System2496Orbit2Begin System2496Orbit2End System2867Orbit1Begin System2867Orbit1End System2868Orbit1Begin System2868Orbit1End System239Orbit3Begin System239Orbit3End System2601Orbit3Begin System2601Orbit3End System2510Orbit2Begin System2510Orbit2End System2511Orbit2Begin System2511Orbit2End System2512Orbit2Begin System2512Orbit2End System2513Orbit2Begin System2513Orbit2End System2869Orbit1Begin System2869Orbit1End System719Orbit4Begin System719Orbit4End System25Orbit2Begin System25Orbit2End System24Orbit4Begin System24Orbit4End System1806Orbit2Begin System1806Orbit2End System1807Orbit2Begin System1807Orbit2End System1808Orbit2Begin System1808Orbit2End System2870Orbit1Begin System2870Orbit1End System2871Orbit1Begin System2871Orbit1End System2872Orbit1Begin System2872Orbit1End System2584Orbit2Begin System2584Orbit2End System2873Orbit1Begin System2873Orbit1End System2514Orbit2Begin System2514Orbit2End System2515Orbit2Begin System2515Orbit2End System2516Orbit2Begin System2516Orbit2End System2874Orbit1Begin System2874Orbit1End System2497Orbit2Begin System2497Orbit2End System2875Orbit1Begin System2875Orbit1End System2499Orbit2Begin System2499Orbit2End System2499Orbit3Begin System2499Orbit3End System2500Orbit2Begin System2500Orbit2End System2501Orbit2Begin System2501Orbit2End System2502Orbit2Begin System2502Orbit2End System2876Orbit1Begin System2876Orbit1End System2877Orbit1Begin System2877Orbit1End System2504Orbit2Begin System2504Orbit2End System2505Orbit2Begin System2505Orbit2End System2878Orbit1Begin System2878Orbit1End System2879Orbit1Begin System2879Orbit1End System2880Orbit1Begin System2880Orbit1End System2881Orbit1Begin System2881Orbit1End System2882Orbit1Begin System2882Orbit1End System2883Orbit1Begin System2883Orbit1End System2884Orbit1Begin System2884Orbit1End System2885Orbit1Begin System2885Orbit1End System2886Orbit1Begin System2886Orbit1End System2887Orbit1Begin System2887Orbit1End System2888Orbit1Begin System2888Orbit1End System2889Orbit1Begin System2889Orbit1End System2890Orbit1Begin System2890Orbit1End System2891Orbit1Begin System2891Orbit1End System2892Orbit1Begin System2892Orbit1End System2893Orbit1Begin System2893Orbit1End System2894Orbit1Begin System2894Orbit1End System2159Orbit2Begin System2159Orbit2End System2895Orbit1Begin System2895Orbit1End System2896Orbit1Begin System2896Orbit1End System2897Orbit1Begin System2897Orbit1End System2476Orbit3Begin System2476Orbit3End System2898Orbit1Begin System2898Orbit1End System2518Orbit2Begin System2518Orbit2End System2519Orbit2Begin System2519Orbit2End System2899Orbit1Begin System2899Orbit1End System2520Orbit2Begin System2520Orbit2End System2521Orbit2Begin System2521Orbit2End System2522Orbit2Begin System2522Orbit2End System2900Orbit1Begin System2900Orbit1End System2523Orbit2Begin System2523Orbit2End System2901Orbit1Begin System2901Orbit1End System2524Orbit2Begin System2524Orbit2End System2525Orbit2Begin System2525Orbit2End System2526Orbit2Begin System2526Orbit2End System2527Orbit2Begin System2527Orbit2End System2528Orbit2Begin System2528Orbit2End System2529Orbit2Begin System2529Orbit2End System2902Orbit1Begin System2902Orbit1End System2903Orbit1Begin System2903Orbit1End System2904Orbit1Begin System2904Orbit1End System2905Orbit1Begin System2905Orbit1End System2479Orbit2Begin System2479Orbit2End System2477Orbit2Begin System2477Orbit2End System2906Orbit1Begin System2906Orbit1End System2478Orbit2Begin System2478Orbit2End System2907Orbit1Begin System2907Orbit1End System2908Orbit1Begin System2908Orbit1End System2909Orbit1Begin System2909Orbit1End System2910Orbit1Begin System2910Orbit1End System2360Orbit2Begin System2360Orbit2End System1925Orbit3Begin System1925Orbit3End System2911Orbit1Begin System2911Orbit1End System1816Orbit2Begin System1816Orbit2End System1817Orbit2Begin System1817Orbit2End System1819Orbit2Begin System1819Orbit2End System1825Orbit2Begin System1825Orbit2End System1828Orbit2Begin System1828Orbit2End System2912Orbit1Begin System2912Orbit1End System2913Orbit1Begin System2913Orbit1End System2361Orbit2Begin System2361Orbit2End System2362Orbit2Begin System2362Orbit2End System2914Orbit1Begin System2914Orbit1End System2915Orbit1Begin System2915Orbit1End System2916Orbit1Begin System2916Orbit1End System2508Orbit2Begin System2508Orbit2End System2509Orbit2Begin System2509Orbit2End System2917Orbit1Begin System2917Orbit1End System1982Orbit2Begin System1982Orbit2End System1983Orbit2Begin System1983Orbit2End System2918Orbit1Begin System2918Orbit1End System2919Orbit1Begin omega was originally 0 in the publication. System2919Orbit1End System2920Orbit1Begin System2920Orbit1End System2921Orbit1Begin System2921Orbit1End System2490Orbit2Begin System2490Orbit2End System2363Orbit2Begin System2363Orbit2End System2922Orbit1Begin System2922Orbit1End System2923Orbit1Begin System2923Orbit1End System2924Orbit1Begin System2924Orbit1End System2925Orbit1Begin System2925Orbit1End System2926Orbit1Begin System2926Orbit1End System2927Orbit1Begin System2927Orbit1End System2928Orbit1Begin System2928Orbit1End System2929Orbit1Begin System2929Orbit1End System2930Orbit1Begin System2930Orbit1End System2365Orbit2Begin System2365Orbit2End System2366Orbit2Begin System2366Orbit2End System2931Orbit1Begin System2931Orbit1End System2932Orbit1Begin System2932Orbit1End System2933Orbit1Begin System2933Orbit1End System2934Orbit1Begin System2934Orbit1End System2495Orbit2Begin System2495Orbit2End System2480Orbit2Begin System2480Orbit2End System2367Orbit2Begin System2367Orbit2End System2935Orbit1Begin System2935Orbit1End System1856Orbit2Begin System1856Orbit2End System1857Orbit2Begin System1857Orbit2End System2936Orbit1Begin System2936Orbit1End System2937Orbit1Begin System2937Orbit1End System2481Orbit2Begin System2481Orbit2End System2482Orbit2Begin System2482Orbit2End System2483Orbit2Begin System2483Orbit2End System2938Orbit1Begin System2938Orbit1End System2939Orbit1Begin System2939Orbit1End System2486Orbit2Begin System2486Orbit2End System2940Orbit1Begin System2940Orbit1End System2941Orbit1Begin System2941Orbit1End System2942Orbit1Begin System2942Orbit1End System2943Orbit1Begin System2943Orbit1End System2944Orbit1Begin System2944Orbit1End System2945Orbit1Begin System2945Orbit1End System2946Orbit1Begin System2946Orbit1End System1744Orbit2Begin System1744Orbit2End System1744Orbit3Begin System1744Orbit3End System2947Orbit1Begin System2947Orbit1End System2948Orbit1Begin System2948Orbit1End System2949Orbit1Begin System2949Orbit1End System2950Orbit1Begin System2950Orbit1End System2951Orbit1Begin System2951Orbit1End System2952Orbit1Begin System2952Orbit1End System2953Orbit1Begin System2953Orbit1End System2954Orbit1Begin System2954Orbit1End System2955Orbit1Begin System2955Orbit1End System2956Orbit1Begin System2956Orbit1End System2957Orbit1Begin System2957Orbit1End System548Orbit3Begin Unless noted differently, the radial velocities are from McClure and Woodsworth (1992ApJ...352..709M) shifted to the zero point of Coravel by subtracting 0.46km/s System548Orbit3End System2157Orbit2Begin Unless noted differently, the radial velocities are from McClure and Woodsworth (1992ApJ...352..709M) shifted to the zero point of Coravel by subtracting 0.46km/s System2157Orbit2End System1306Orbit3Begin Unless noted differently, the radial velocities are from McClure and Woodsworth (1992ApJ...352..709M) shifted to the zero point of Coravel by subtracting 0.46km/s System1306Orbit3End System2158Orbit2Begin Unless noted differently, the radial velocities are from McClure and Woodsworth (1992ApJ...352..709M) shifted to the zero point of Coravel by subtracting 0.46km/s System2158Orbit2End System1613Orbit2Begin System1613Orbit2End System1615Orbit2Begin System1615Orbit2End System1612Orbit2Begin System1612Orbit2End System1614Orbit2Begin System1614Orbit2End System1616Orbit2Begin System1616Orbit2End System2958Orbit1Begin System2958Orbit1End System2959Orbit1Begin SAO 167450 is the visual secondary of the W UMa-type eclipsing binary AA Cet, making the system quadruple. Both components of SAO 167450 are somewhat metal rich relative to the Sun. The high lithum abundances argue that the system is less than 1 billion years old. System2959Orbit1End System2960Orbit1Begin Observatories: MtStrom = Mount Stromlo, Gemini S = Gemini South, KPNO = Kitt Peak National Observatory, CTIO = Cerro Tololo Inter-American Observatory. The system is a symbiotic binary consisting of a M giant and a probable hot compact companion. The orbital elements were determined from the giant's absorption line velocities. The measured velocities also contain pulsational velocity changes. Velocities of the Paschen delta emission line of hydrogen are almost 180 degrees out of phase with the M giant absorption features and also have nearly the same center of mass velocity as the giant. Thus, they are listed for component B, the presumed hot compact object. The emission velocities have only been used to obtain a mass ratio of the components. System2960Orbit1End System2961Orbit1Begin Observatories: MtStrom = Mount Stromlo, Gemini S = Gemini South, KPNO = Kitt Peak National Observatory, CTIO = Cerro Tololo Inter-American Observatory. The system is a symbiotic binary consisting of a M giant and a probable hot compact companion. The measured velocities also contain pulsational velocity changes. System2961Orbit1End System2962Orbit1Begin Observatories: MtStrom = Mount Stromlo, Gemini S = Gemini South, KPNO = Kitt Peak National Observatory, CTIO = Cerro Tololo Inter-American Observatory. The system is a symbiotic binary consisting of a M giant and a probable hot compact companion. The measured velocities also contain pulsational velocity changes. System2962Orbit1End System2963Orbit1Begin Observatories: CES = Cassegrain Echelle Spectrograph The star is a member of the open cluster Blanco 1 System2963Orbit1End System2964Orbit1Begin Observatories: CES = Cassegrain Echelle Spectrograph. The star is a member of the open cluster Blanco 1. System2964Orbit1End System2965Orbit1Begin Observatories: CES = cassegrain Echelle Spectrograph. The star is a member of the open cluster Blanco 1. System2965Orbit1End System1463Orbit2Begin Observatories: CES = Cassegrain Echelle Spectrograph The star is a member of the open cluster Blanco 1 System1463Orbit2End System2966Orbit1Begin Observatories: CES = cassegrain Echelle Spectrograph The star is a member of the open cluster Blanco 1 System2966Orbit1End System2967Orbit1Begin Observatories: CES = Cassegrain Echelle Spectrograph. The star is a member of the open cluster Blanco 1 System2967Orbit1End System2968Orbit1Begin Observatories: CES = Cassegrain Echelle Spectrograph. The star is a member of the open cluster Blanco 1 System2968Orbit1End System2969Orbit1Begin Observatories: CES = Cassegrain Echelle Spectrograph The star is a member of the open cluster Blanco 1 System2969Orbit1End System1430Orbit2Begin System1430Orbit2End System2970Orbit1Begin System2970Orbit1End System2971Orbit1Begin System2971Orbit1End System2972Orbit1Begin System2972Orbit1End System2973Orbit1Begin System2973Orbit1End System2974Orbit1Begin System2974Orbit1End System914Orbit2Begin System914Orbit2End System2975Orbit1Begin System2975Orbit1End System2976Orbit1Begin System2976Orbit1End System2977Orbit1Begin The T0 originally published was wrong. S. Rucinski revised it prior to uploading the orbits in SB9. He also supplied two alternative solutions: Solution with: P = 0.810720 assumed period, as given in Table 2 V0 = -16.03 +/- 0.45 K1 = 45.36 0.33 K2 = 169.62 1.69 T0 = 2,452,330.2924 +/- 0.0015 2,452,330.1642 as in the table is incorrect eps1 = 1.92 eps2 = 12.71 Solution with: P = 0.810746, the Hipparcos photometric period V0 = -15.85 +/- 0.46 K1 = 45.52 0.32 K2 = 169.58 1.75 T0 = 2,452,330.2870 +/- 0.0015 eps1 = 2.01 eps2 = 12.84 System2977Orbit1End System1215Orbit2Begin All epochs are in MJD System1215Orbit2End System1218Orbit2Begin All epochs in MJD System1218Orbit2End System2978Orbit1Begin System2978Orbit1End System2979Orbit1Begin System2979Orbit1End System2980Orbit1Begin System2980Orbit1End System2981Orbit1Begin System2981Orbit1End System2982Orbit1Begin System2982Orbit1End System2983Orbit1Begin System2983Orbit1End System301Orbit2Begin System301Orbit2End System596Orbit2Begin System596Orbit2End System594Orbit2Begin System594Orbit2End System2984Orbit1Begin System2984Orbit1End System2985Orbit1Begin System2985Orbit1End System828Orbit2Begin In the paper, for this system, the table with RV does not list the epoch, only RV and phase. The epochs were computed for convenience using the period and T0 from Table 3 and the epochs from Table 1. System828Orbit2End System2986Orbit1Begin System2986Orbit1End System2987Orbit1Begin System2987Orbit1End System2988Orbit1Begin System2988Orbit1End System1314Orbit2Begin System1314Orbit2End System728Orbit2Begin System728Orbit2End System2989Orbit1Begin System2989Orbit1End System2990Orbit1Begin System2990Orbit1End System2991Orbit1Begin System2991Orbit1End System2992Orbit1Begin System2992Orbit1End System2993Orbit1Begin System2993Orbit1End System2994Orbit1Begin System2994Orbit1End System2995Orbit1Begin System2995Orbit1End System2996Orbit1Begin In the paper, for this system, the table with RV does not list the epoch, only RV and phase. The epochs were computed for convenience using the period and T0 from Table 2 and the epochs from Table 1. System2996Orbit1End System2997Orbit1Begin System2997Orbit1End System2998Orbit1Begin System2998Orbit1End System2999Orbit1Begin System2999Orbit1End System3000Orbit1Begin System3000Orbit1End System3001Orbit1Begin System3001Orbit1End System3002Orbit1Begin The value used for F is not the one liste in Table 2 (0.3053707d) but the one listed below it. The latter gives a smaller dispersion. System3002Orbit1End System3003Orbit1Begin System3003Orbit1End System3004Orbit1Begin System3004Orbit1End System3005Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). The secondary velocities have a zero-point offset relative to the primary velocities, and can be corrected by adding -3.96 km/s. System3005Orbit1End System3006Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). There was a typo on V0 in the publication which is corrected here. System3006Orbit1End System3007Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3007Orbit1End System3008Orbit1Begin Eclipsing binary. These velocities are from absorption lines, and are the ones adopted for the final spectroscopic solution in the original publication. System3008Orbit1End System912Orbit3Begin Eclipsing binary. System912Orbit3End System3009Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). The secondary velocities have a zero-point offset relative to the primary velocities, and can be corrected by adding -2.31 km/s. System3009Orbit1End System894Orbit3Begin Astrometric-spectroscopic binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System894Orbit3End System3011Orbit1Begin Eclipsing binary. Radial velocities are measured relative to that of GJ 182, for which the value reported by Montes et al. (2001) is +32.4 +/- 1.0 km/s (2001MNRAS.328...45M). System3011Orbit1End System3012Orbit1Begin Eclipsing binary. System3012Orbit1End System1955Orbit4Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System1955Orbit4End System518Orbit2Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System518Orbit2End System944Orbit2Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System944Orbit2End System3013Orbit1Begin System3013Orbit1End System3014Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3014Orbit1End System3015Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3015Orbit1End System3016Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3016Orbit1End System3017Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3017Orbit1End System3018Orbit1Begin Eclipsing binary. Radial velocities are on the native CfA system (+0.139 km/s should be added to these velocities to put them on the absolute velocity system defined by CfA observations of minor planets). System3018Orbit1End System3019Orbit1Begin System3019Orbit1End System3020Orbit1Begin System3020Orbit1End System3021Orbit1Begin System3021Orbit1End System3022Orbit1Begin System3022Orbit1End System3023Orbit1Begin System3023Orbit1End System708Orbit2Begin System708Orbit2End System3024Orbit1Begin System3024Orbit1End System593Orbit2Begin System593Orbit2End System3025Orbit1Begin System3025Orbit1End System921Orbit2Begin System921Orbit2End System3026Orbit1Begin System3026Orbit1End System3027Orbit1Begin System3027Orbit1End System581Orbit2Begin System581Orbit2End System2125Orbit2Begin System2125Orbit2End System594Orbit3Begin System594Orbit3End System127Orbit2Begin We confirm the assessment of Batten et al., who concluded in the previous SB catalog that the orbital period of Northcott is correct. Fair = Fairborn Observatory, KPNO = Kitt Peak National Observatory, McD = McDonald Observatory System127Orbit2End System1068Orbit2Begin Fair = Fairborn Observatory, KPNO = Kitt Peak National Observatory System1068Orbit2End System1466Orbit2Begin Hipparcos photometry shows that this system has partial eclipses. The stars are at the very end of their main sequence lifetimes or have just begun crossing the Hertsprung gap. KPNO = Kitt Peak National Observatory, McD = McDonald Observatory, Fair = Fairborn Observatory System1466Orbit2End System2107Orbit2Begin KPNO = Kitt Peak National Observatory, Fair = Fairborn Observatory System2107Orbit2End System942Orbit2Begin The new orbital elements confirm that the system has a partial primary eclipse, but whether there is a secondary eclipse in this eccentric orbit system remains to be determined. Fair = Fairborn Observatory, KPNO = Kitt Peak National Observatory System942Orbit2End System5Orbit3Begin Both components are Am stars, and both are rotating substantially faster than their pseudosynchronous rotational velocities (Hut 1981, A&A, 99, 126). System5Orbit3End System639Orbit2Begin Both components of 41 Sex are synchronously rotating. For the primary of 41 Sex the spectrum line depth changes noted by Sreedhar Rao et al. (1990, ApJ, 365, 336) were not detected. Given the extremely small eccentricity found for the eccentric-orbit solution, a circular-orbit solution was adopted. Thus, the value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. System639Orbit2End System73Orbit2Begin The binary components are rotating significantly faster than their pseudosynchronous velocities. System73Orbit2End System77Orbit2Begin A new astrometric orbit computed with the Hipparcos astrometry and the above spectroscopic orbital elements produces a very high orbital inclination of 88 deg +/- 5 deg. An extensive series of photometric observations was searched, but no evidence for eclipses was found. System77Orbit2End System1358Orbit2Begin An extensive series of photometric observations was searched, but no evidence for eclipses was found. The primary star is likely just beginning to traverse the Hertzsprung gap. System1358Orbit2End System340Orbit4Begin Observatories: CASS: 2.1m Cassegrain spectrograph at Kitt Peak The star is a member of the Trapezium System and an eclipsing binary. System340Orbit4End System342Orbit3Begin Observatories: CASS: 2.1m Cassegrain spectrogrph at Kitt Peak. The star is a member of the Trapezium System and an eclipsing binary. System342Orbit3End System3028Orbit1Begin Observatories: CASS: 2.1m Cassegrain spectrograph at Kitt Peak. System3028Orbit1End System17Orbit3Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System17Orbit3End System189Orbit2Begin Observatories: CFS = Coude feed Spectrograph at Kitt Peak Coudè feed Telescope System189Orbit2End System3029Orbit1Begin Observatories: CFS = Coude feed Spectrograph at Kitt Peak Coudè Feed Telescope System3029Orbit1End System297Orbit2Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System297Orbit2End System312Orbit2Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System312Orbit2End System3030Orbit1Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System3030Orbit1End System321Orbit2Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System321Orbit2End System3031Orbit1Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System3031Orbit1End System349Orbit2Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System349Orbit2End System354Orbit3Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System354Orbit3End System361Orbit2Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System361Orbit2End System3032Orbit1Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System3032Orbit1End System3033Orbit1Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope System3033Orbit1End System3034Orbit1Begin Observatories: CFS = Coudè Feed Spectrograph at Kitt Peak Coude Feed Telescope SB9: This is the orbit as it appears in the original paper. However, we do obtain a better plot if one replaces the corresponding elements with T=44464.2; omega=73deg and K1=30.4km/s. At least, with those values, the plot looks close to the one in the paper. In any case, the the orbit is very poor. System3034Orbit1End System3035Orbit1Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System3035Orbit1End System865Orbit3Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope SB9: The orbit is just a cut and paste of the orbit from Levato et al. (1987), also in SB9. The data from the paper does not support that orbital solution which is poorly supported by the original observations. System865Orbit3End System3036Orbit1Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System3036Orbit1End System3037Orbit1Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System3037Orbit1End System1170Orbit2Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System1170Orbit2End System3038Orbit1Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System3038Orbit1End System1191Orbit3Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope System1191Orbit3End System3039Orbit1Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope The publication lists 0 for omega ... but it is not consistent with the other parameters (SB9). System3039Orbit1End System1409Orbit3Begin Observatories: CFS = Coude fees Spectrograph at Kitt Peak Coudé Feed Telescope The publication lists 0 for omega ... but it is not consistent with the other parameters (SB9). System1409Orbit3End System1077Orbit2Begin Observatories: Dominion Astrophysical Observatory Reticon The star is a double-lined spectrocopic binary. System1077Orbit2End System1305Orbit2Begin Observatories: DAO: Dominion Astrophysical Observatory´s coude spectrograph on the 1.2 m telescope. The measurements of the profiles were done by fitting Gaussian profiles. The star is an A-type over contact binary W UMa. System1305Orbit2End System1305Orbit3Begin Observatories: DAO: Dominion Astrophysical Observatory´s coude spectrograph on the 1.2 m telescope. The measurements of the profiles were done by fitting Synthetic profiles and the measurements of the primary and secondary components are in excellent agreement. The star is an A-type over contact binary W UMa. System1305Orbit3End System1305Orbit4Begin Observatories: DAO: Dominion Astrophysical Observatory´s coude spectrograph on the 1.2 m telescope. The measurements of the profiles were done by fitting Zero velocity profiles. The star is an A-type over contact binary W UMa. System1305Orbit4End System3040Orbit1Begin Four sophie measurements were taken into account for each component. A correction of 3m/s was added to our original estimation of the RV calculated by fitting two Gaussian curves to the sophie CCF. Seventeen blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.679+/-0.033. System3040Orbit1End System3041Orbit1Begin System3041Orbit1End System3042Orbit1Begin System3042Orbit1End System1514Orbit2Begin Revision of the orbit of Tokovinin (1999,A&AS, 136, 373). The Tokovinin's measurements were taken into account with a correction of +310m/s$, corresponding to the best fit. Three blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.564+/-0.035. System1514Orbit2End System3043Orbit1Begin Sixteen blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.618+/-0.018. System3043Orbit1End System3044Orbit1Begin Preliminary orbit; our observations cover only 79.5pc of the period. System3044Orbit1End System3045Orbit1Begin System3045Orbit1End System3046Orbit1Begin System3046Orbit1End System3047Orbit1Begin The SB1 orbit was computed discarding all the measurements between 0 and -10km/s, which seem to refer to a third component with fixed velocity. The measurements of the secondary component are not symmetric to those of the primary, and it is impossible to derive a SB2 orbit. Finally, a part of a long period orbit is visible in the large residuals of the SB1 orbit. Therefore, the system could be quadruple, although the CCF of a sole sophie spectrum exhibits one dip only. System3047Orbit1End System3048Orbit1Begin System3048Orbit1End System3049Orbit1Begin Orbit calculated discarding the 4 blended measurements. When they are taken into account, the blend coefficient is C_0=0.624+/-0.042, but the orbital elements are not improved. System3049Orbit1End System3050Orbit1Begin The 8 measurements of the secondary seem fixed around -28km/s, and we prefer to discard them. Otherwise, a SB2 orbit is obtained with K_2=8.3km/s. System3050Orbit1End System3051Orbit1Begin System3051Orbit1End System267Orbit2Begin A first orbit was published by Griffin and Gunn (1981, AJ, 86, 588). System267Orbit2End System3052Orbit1Begin A bright SB2 (6.67 mag) with a semi-major axis expected around 58 mas, which should be easily separated. Fifteen blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.762+/-0.061 System3052Orbit1End System3053Orbit1Begin System3053Orbit1End System3054Orbit1Begin System3054Orbit1End System3055Orbit1Begin Five blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.683+/-0.032. System3055Orbit1End System3056Orbit1Begin A visual binary system with separation 0.3 arcsec. The A component is the SB1. The dip of the B component is visible on the coravel CCF, with the fixed velocity V_B=52.08+/-0.33km/s. Twenty-nine blended RV refer to components A and B, with the blend coefficient C_0=0.717+/-0.023. System3056Orbit1End System2549Orbit2Begin Revision of the orbit of Duquennoy and Mayor (1991, A&A, 248, 485). System2549Orbit2End System3057Orbit1Begin System3057Orbit1End System3058Orbit1Begin System3058Orbit1End System3059Orbit1Begin A correction of 0.489 km/s was added to the 7 RV measurements derived from sophie for each component, in order to get the best fit. Twenty-four blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.788+/-0.037. System3059Orbit1End System1499Orbit2Begin Revision of the orbit of Tokovinin (1994, Astronomy Letters, 20, 717), which was based on 17 recent measurements, but also on 9 measurements performed between 1916 and 1932. We applied a correction of +0.381 km/s for the former, and +1.45 km/s for the latter. System1499Orbit2End System3060Orbit1Begin System3060Orbit1End System3061Orbit1Begin A first orbit was published by Jeffries, Bertram and Spurgeon (1995, MNRAS, 276, 397). System3061Orbit1End System3062Orbit1Begin System3062Orbit1End System2183Orbit2Begin Revision of the orbit of Latham et al. (2002, AJ, 124, 1144); we found a correction of -0.120 km/s to apply to their measurements. System2183Orbit2End System3063Orbit1Begin System3063Orbit1End System3064Orbit1Begin A secondary dip was observed by Halbwachs et al. (2011, Proceedings SF2A 2011, pg 303), leading to the mass ratio q approx 0.64. System3064Orbit1End System3065Orbit1Begin A secondary dip was observed by Halbwachs et al. (2011, Proceedings SF2A 2011, pg 303), leading to the mass ratio q approx 0.66. System3065Orbit1End System3066Orbit1Begin A secondary dip was observed by Halbwachs et al. (2011, Proceedings SF2A 2011, pg 303), leading to the mass ratio q approx 0.75. System3066Orbit1End System3067Orbit1Begin Eleven blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.879+/-0.026. System3067Orbit1End System3068Orbit1Begin The star is ADS 8695, a visual binary with P=359y, a=1.18 arcsec and Delta m= 2.2mag (Heintz W.D., 1997, ApJS 111, 335); the secondary component is not visible on our observations, and the SB1 orbit refers to the brightest component of the visual binary. A correction of -0.263 km/s was applied to the 7 original sophie measurements. System3068Orbit1End System3069Orbit1Begin System3069Orbit1End System3070Orbit1Begin Eleven blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.743+/-0.028. System3070Orbit1End System3071Orbit1Begin System3071Orbit1End System3072Orbit1Begin System3072Orbit1End System3073Orbit1Begin Sixteen blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.862+/-0.041. System3073Orbit1End System3074Orbit1Begin A G5-type star without luminosity class. Due to the short period, it cannot be a giant; assuming the primary component is a dwarf, the secondary component has a minimum mass around 50 Jupiter masses, and it is a brown dwarf candidate. System3074Orbit1End System3075Orbit1Begin System3075Orbit1End System3076Orbit1Begin System3076Orbit1End System3077Orbit1Begin System3077Orbit1End System1500Orbit2Begin The star is a triple system, consisting in a long period SB1 with an additional short period orbit. Preliminary elements of the short period orbit were published by Tokovinin and Smekhov (1995, Astronomy Letters, 21, 247); in order to avoid the drift due to the long period, we rejected 21 of our coravel measurements made before JD 2449000, but we took into account 16 measurements performed with Russian telescopes; the correction to add to the latter is +1.15 km/s. System1500Orbit2End System2198Orbit2Begin Revision of the orbit of Latham et al. (2002, AJ, 124, 1144), with a correction of -0.328 km/s to their measurements. The spectral type of the star is G7 V, leading to a minimum mass around 30 Jupiter masses for the secondary component. System2198Orbit2End System3078Orbit1Begin A bright SB2 (6.70 mag) with a semi-major axis expected around 17 mas, which should be easily separated. Five blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.683+/-0.024. System3078Orbit1End System3079Orbit1Begin A bright SB2 (6.70 mag) with a semi-major axis expected around 17 mas, which should be easily separated. Two blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.736+/-0.061. System3079Orbit1End System3080Orbit1Begin Triple system already studied by Tokovinin (1998, Astronomy Letters, 24, 288). A triple system solution was computed, combining a long period SB2 with a SB1 as primary component. The period of the SB2 was fixed to the value obtained by Docobo and Costa (1986, IAU Double Star Inf. Circ. 99) for a visual orbit, as reported by Hartkopf and Mason (Sixth Catalog of Orbits of Visual Binary Stars, http://ad.usno.navy.mil/wds/orb6.html). The selection of the blended measurements was done as follows: when only one RV was obtained, it was assumed to be a blend as soon as the difference |V_1 - V_2| was found to be less than 30 km/s. Nineteen blended measurements were taken into account in the calculation of the spectroscopic elements, resulting in the blend coefficient C_0=0.928+/-0.022. The solution presented hereafter is based on our measurements only, since it is better than the one obtained when the measurements of Tokovinin are added. The blended values together with theoretical uncertainty are listed below 47363.559 -23.27 1.14 Coravel 47532.242 -4.62 0.58 Coravel 47882.229 14.06 1.04 Coravel 48142.425 -6.26 0.74 Coravel 48144.484 5.13 0.85 Coravel 48510.443 -9.06 0.57 Coravel 48546.371 25.49 0.97 Coravel 49687.283 -14.47 0.82 Coravel 49925.516 18.04 0.76 Coravel 49930.575 28.37 2.06 Coravel 49931.535 5.80 0.67 Coravel 49952.556 -0.36 0.76 Coravel 49954.522 -0.84 0.74 Coravel 49957.508 18.76 0.79 Coravel 50315.569 1.69 0.64 Coravel 50341.500 20.44 0.88 Coravel 50342.409 25.00 0.97 Coravel 50343.433 -23.80 1.16 Coravel 50665.579 2.11 0.63 Coravel System3080Orbit1End System1508Orbit2Begin System1508Orbit2End System3081Orbit1Begin System3081Orbit1End System3082Orbit1Begin System3082Orbit1End System3083Orbit1Begin System3083Orbit1End System3084Orbit1Begin System3084Orbit1End System3085Orbit1Begin System3085Orbit1End System3086Orbit1Begin System3086Orbit1End System3087Orbit1Begin System3087Orbit1End System3088Orbit1Begin System3088Orbit1End System3089Orbit1Begin System3089Orbit1End System1922Orbit3Begin System1922Orbit3End System666Orbit2Begin System666Orbit2End System3090Orbit1Begin System3090Orbit1End System3091Orbit1Begin System3091Orbit1End System3092Orbit1Begin System3092Orbit1End System3093Orbit1Begin System3093Orbit1End System3094Orbit1Begin System3094Orbit1End System1404Orbit2Begin System1404Orbit2End System3095Orbit1Begin System3095Orbit1End System3095Orbit2Begin System3095Orbit2End System2856Orbit2Begin The value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Fair = Fairborn Observatory, Lick =Lick Observatory, KPNO = Kitt Peak National Observatory A spectroscopic abundance analysis indicates that the stars are somewhat metal rich compared to the Sun. Despite the relative similarity of the components, the two stars have lithium abundances that differ by at least a factor of 18. The system has a warm disk of particles that are thought to be the remnants of a recent collision of rocky bodies. System2856Orbit2End System1728Orbit1Begin The system is a detached eclipsing binary with nearly identical components. The binary also has light variability due to starspots on one or both components that produce a rotation period of 8.49 days. System1728Orbit1End System2143Orbit1Begin System is an eclipsing binary with relatively shallow (0.3 mag) partial eclipses. The more precise photometric period was adopted as the orbital period. The value of T is NOT a time of periastron passage but rather is T_0, a time of maximum positive velocity. Fair = Fairborn Observatory, KPNO = Kitt Peak National Observatory System2143Orbit1End System2168Orbit1Begin System is an eclipsing binary with fairly deep (0.5 mag) partial eclipses. The more precise photometric period was adopted as the orbital period. Despite the short 3.45 day period, the orbit is still significantly eccentric as predicted by tidal theory for an early-type binary with an estimated age of 380 Myr. System2168Orbit1End System1107Orbit4Begin Code for RV references: 1= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 2= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1987, ApJS, 65, 307 3= Wilson, T.D., Carter, M.W., Barnes, T.G., Van Citters, G.W., and Moffett, T.J . 1989, ApJS, 69, 951 4= Kiss et al 2000 MN 314 5= Evans et al 1990AJ.....99.1598 6= Gorynya et al VizieR On-line Data Catalog: III/229 System1107Orbit4End System709Orbit5Begin Code for RV references: 1= Petterson_ea_05MN362_1167_RV.dat 2= Petterson: (2004) MN250 pre-1996 data 3= Petterson: (2004) MN250 recent data 4= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 5= Grayzeck, E.J. 1978 AJ, 83, 1397 BUT NOT USED IN ORBITAL ANALYSIS 6= Lloyd Evans 1968, MNRAS 141, 109 7= Campbell Moore 1928 8= B\"ohm-Vitense, E., Clark, M., Cottrell, P.L., Wallerstein, G. 1990, AJ, 99, 353 9= Stibbs 1955 10= Bersier 02ApJS140 465 System709Orbit5End System3096Orbit1Begin Code for RV references 1= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 2= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 3= Stibbs 1955 4= Lloyd Evans 1968 MNRAS 141, 109 5= Grayzeck, E.J. 1978 AJ, 83, 1397 6= Mermilliod, J.-C., Mayor, M., Burki, G. 1987 A\&AS 70, 389 7= Feast 1967 MNRAS, 136, 141 8= Cambell and Moore 1928 Lick Obs Bull 16 9= Breger M, 1970, AJ 75, 239 System3096Orbit1End System1185Orbit5Begin Code for RV references 1= Gorynya catalog 2= Barnes_ea_05ApJS156_227_RV.dat 3= Kiss et al 2000 MN 314, 420 4= no 4 as part og 9 5= Wilson, T.D., Carter, M.W., Barnes, T.G., Van Citters, G.W., Moffett, T.J. 1989, ApJS, 69, 95 6= Evans_76ApJS32_399_RV. 7= Breitfellner, M.G.,& Gillet, D. 1993, A\&A, 277, 541 8= Evans, N.R., Welch, D.L., Slovak, M.H., Barnes, T.G.,Moffett, T.J. 1993, AJ, 106, 1599 DAO data 9= idem McDonald data 10= Herbig, G.H., \& Moore, J.H. 1952, ApJ 116, 348 System1185Orbit5End System3097Orbit1Begin Code for RV references 1= Gorynya catalog 2= Storm et al. 2004A&A...415..531 3= Kiss et al 2000 MN 314, 420 4= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 5= Wilson, T.D., Carter, M.W., Barnes, T.G., Van Citters, G.W., Moffett, T.J. 1989, ApJS, 69, 951 6= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1987, ApJS, 65, 307 7= Adams, W.S., \& Shapley, H. 1918 ApJ, 47, 46 8= Abt, H.A. 1959 AJ, 130, 1021 9= Niva, G.D., \& Schmidt, E.G. 1979, ApJ, 234, 245 10= Gieren, W. 1976, A\&A 47, 211 11= H\"aupl, W 1988, AN, 309, 327 12= Beavers, W.I. \& Eitter, J.J. 1986, ApJS, 62, 147 System3097Orbit1End System1172Orbit4Begin Code for RV references 1= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1987, ApJS, 65, 307 2= Wilson, T.D., Carter, M.W., Barnes, T.G., Van Citters, G.W. 3= gornya catalog 4= Evans, N.R. 1988, APJS 66, 343 5= Maddrill, J.D. 1906, PASP 18. 252 6= Abt, H.A. 1973, ApJS 26, 365 7= unpublished David Dunlap data, as quoted by Evans 8= unpublished Data by Barry Madore using Cambridge RV spectrometer (by Evans?) 9= Imbert, M. 1985, A\&AS 58, 529 System1172Orbit4End System2000Orbit3Begin Code for RV references 1= gorynya catalog 2= Storm et al. 2004A&A...415..531 3= Kiss et al 2000 MN 314, 420 4= Petterson: (2004) MN250 5= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 6= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1987, ApJS, 65, 307 7= Evans, N.R., Carpenter, K., Robinson, R., et al. 1999, ApJ, 524, 379 8= Frost, E.B. 1906, ApJ, 23, 264 9= Sanford, R.F. 1927, ApJ, 66, 170 10= Sanford, R.F., 1956, ApJ, 123, 201 11= Wallerstein, G. 1972, PASP, 84, 656 12= Evans, N.R. 1976, ApJS, 32, 399 13= Coulson, I.M. 1983, MNRAS, 203, 925 14= Griffin (quoted in Coulson) 15= Evans, N.R., & Lyons, R. 1994, AJ, 107, 2164 16= Gieren, W.P. 1989, A&A, 216, 135 =16 17= Harper, W.E. 1934, Publ. DAO, 6, 151 System2000Orbit3End System1722Orbit2Begin Code for RV references 1= Gorynya catalog 2= Barnes_ea_05ApJS156_227_RV.dat 3= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1988, ApJS, 66, 43 4= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 5= Sanford, R.F. 1951, ApJ, 114, 331 6= Evans_76ApJS32_399_RV.pdf 7= Feast 1967 MNRAS, 136, 141 System1722Orbit2End System1929Orbit3Begin Code for RV references 1= Gorynya catalog 2= Petterson_ea_05MN362_1167_RV.dat 3= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 4= Gieren, W. 1981, ApJS, 46, 287 5= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1988, ApJS, 66, 43 6= Evans, N.R., \& Sugars, B.J.A. 1997, AJ, 113, 792 7= Joy 1951 ApJ 86 363 8= Groenewegen 2012 (in prep.) 9= Evans et al. 2011, dataset 7 by Eaton System1929Orbit3End System3098Orbit1Begin V0 adopted from 1987PASP...99.1206M Code for RV references 1= Gorynya catalog 2= Gieren, W. 1981, ApJS, 46, 287 3= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1988, ApJS, 66, 43 4= Lloyd Evans 1968 MNRAS 141, 109 5= Stibbs 1955 6= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 7= Storm_ea_2011AA534_A94_Table3.dat 8= Cambell and Moore 1928 Lick Obs Bull 16 9= Breger M, 1970, AJ 75, 239 System3098Orbit1End System1930Orbit2Begin Code for RV references: 1= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 2= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1988, ApJS, 66, 43 3= gornya catalog 4= Barnes ea 05ApJS156 227.dat 5= JOY 1937 6= Storm ea 2011AA534 A94 System1930Orbit2End System2001Orbit3Begin V0 adopted from 1987PASP...99.1206M Code for RV references 1= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 2= NOT USED: Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1987, ApJS, 65, 307 3= Bersier, D., Burki, G., Mayor, M., and Duquennoy, A. 1994, A&AS, 108, 25 4= Wilson, T.D., Carter, M.W., Barnes, T.G., et al. 1989, ApJS, 69, 951 5= Petterson, O. K. L., Cottrell, P. L. & Albrow, M. D. 2005 MN362 1167 6= Albrow Cottrell 1996 MN 280, 917 7= Babel ea 1989 AA 216, 125 8= Jacobsen, T.S., Wallerstein, G., Abt, H.A., 1984, PASP 96, 630 9= Jacobsen, T. S. 1974, ApJ 191, 691 10= Petterson, O. K. L., Cottrell, P. L. & Albrow, M. D. 2004 MN350 , 95 11= Lloyd Evans 1968, MNRAS 141, 109 12= NOT USED Wallerstein et al 1992 MNRAS 259, 474 13= Stibbs 1955 System2001Orbit3End System3099Orbit1Begin V0 adopted from 1987PASP...99.1206M System3099Orbit1End System3010Orbit1Begin Code for RV references 1= Bersier 02ApJS140 465 2= Coulson, I.M., Caldwell, J.A.R., and Gieren, W.P. 1985, ApJS, 57, 595 3= Lloyd Evans, T. 1980, SAAO Circulars, 1, 257 4= Stibbs 1955 5= Feast 67MN136 141 6= Grayzeck 1978 System3010Orbit1End System1721Orbit3Begin Code for RV references 1= Gorynya catalog 2= Barnes_ea_05ApJS156_227 3= Barnes, T.G., Moffett, T.J., and Slovak, M.H. 1988, ApJS, 66, 43 4= Evans, N.R. and Welch, D.L. 1993, PASP, 105, 836 5= Gieren W., 1989, PASP, 101, 160 6= Joy, H.A. 1937, ApJ, 86, 363 7= Imbert, M. 1996, A\&AS, 116, 497 8= Sugars, B.J.A., Evans, N.R. \& 1996, AJ, 112, 1670 System1721Orbit3End