00057+4549AB The Sixth Catalog of Orbits of Visual Binary Stars lists two
00057+4549AB orbits for the AB pair of that system (separated by about 6"):
00057+4549AB one with a period of 1550yr (Popovic and Pavlovic,
00057+4549AB 1996BOBeo.153...57P) and another with a period of 509yr
00057+4549AB (Kiyaeva et al., 2001AstL...27..391K), indicating that the
00057+4549AB solution is not yet well constrained. Radial velocities
00057+4549AB obtained by CORAVEL and by Tokovinin & Smekhov
00057+4549AB (2002A&A...382..118T), as listed in Table A.4 and displayed in
00057+4549AB Fig. A.1, correspond to a radial velocity difference VB-VA
00057+4549AB slightly decreasing from -2.7km/s in 1980 to -3.8km/s in 1996.
00057+4549AB The value -3.0km/s has been used by Kiyaeva et al.
00057+4549AB (2001AstL...27..391K) to determine unambiguously the ascending
00057+4549AB node. This result is confirmed thanks to the precise
00057+4549AB radial-velocity measurements of Marcy (2013, priv. comm.) that
00057+4549AB show a linear variation for VB-VA amounting to -6.4m/s/yr from
00057+4549AB 2000 to 2010, while a value of -11.5m/s/yr is calculated from
00057+4549AB the visual orbit. Thus we have computed the position of the
00057+4549AB orbital pole but it is not expected to be precise. Kiyaeva et
00057+4549AB al. (2001AstL...27..391K) also suggested that ADS 48 ABF is a
00057+4549AB hierarchical triple system whose orbits (AB) and (AB-F) are not
00057+4549AB coplanar. This hypothesis was contradicted by Cvetkovic et al.
00057+4549AB (2012AJ....144...80C), who concluded that the F component has a
00057+4549AB common proper motion with
00057+4549AB the AB pair, but that it is not bound by gravity.
00184+4401AB Indeterminate visual orbit.
00321+6715Aa,Ab and AB. The preliminary visual orbits of this triple
00321+6715Aa,Ab hierarchical system were computed by Docobo et al.
00321+6715Aa,Ab (2008A&A...478..187D). No radial velocity measurements are
00321+6715Aa,Ab available to resolve the ambiguity of the ascending node.
00321+6715AB and Aa,Ab. The preliminary visual orbits of this triple
00321+6715AB hierarchical system were computed by Docobo et al.
00321+6715AB (2008A&A...478..187D). No radial velocity measurements are
00321+6715AB available to resolve the ambiguity of the ascending node.
01083+5455Aa,Ab Drummond et al. (1995ApJ...450..380D) obtained the first
01083+5455Aa,Ab relative astrometric orbit for that system from their direct
01083+5455Aa,Ab detection of the faint B component. Combining that orbit with
01083+5455Aa,Ab earlier photocentric positions (Lippincott 1981ApJ...248.1053L;
01083+5455Aa,Ab Russell & Gatewood, 1984PASP...96..429R), masses could be
01083+5455Aa,Ab derived: MA=0.74+/-0.06M_{sun}_ and MB=0.17+/-0.01M_{sun}_.
01083+5455Aa,Ab Duquennoy & Mayor (1991A&A...248..485D) derived a preliminary
01083+5455Aa,Ab spectroscopic orbit, and Abt & Willmarth (2006ApJS..162..207A)
01083+5455Aa,Ab obtained thereafter more radial velocities; however, Abt &
01083+5455Aa,Ab Willmarth (2006ApJS..162..207A) did not attempt to compute a
01083+5455Aa,Ab combined orbit, and merged the orbital elements of Duquennoy &
01083+5455Aa,Ab Mayor (1991A&A...248..485D) and Drummond et al.
01083+5455Aa,Ab (1995ApJ...450..380D). Because this is not fully satisfactory
01083+5455Aa,Ab and is prone to confusion (as further discussed below),
01083+5455Aa,Ab especially regarding the ambiguity on {omega}, we decided to
01083+5455Aa,Ab compute a new combined orbit (Fig. A.2), using data of
01083+5455Aa,Ab Duquennoy & Mayor (1991A&A...248..485D) as well as more recent
01083+5455Aa,Ab unpublished CORAVEL data (Table A.5), plus velocities reported
01083+5455Aa,Ab by Abt & Willmarth (2006ApJS..162..207A). The astrometric
01083+5455Aa,Ab positions of B relative to A taken from the WDS database at
01083+5455Aa,Ab USNO were used as well. As shown in Table A.2, the value of
01083+5455Aa,Ab {omega} for the astrometric orbit of B around A is
01083+5455Aa,Ab 329.4{deg}+/-3.8{deg} (thus a change of 180{deg} from the
01083+5455Aa,Ab relative orbit of Drummond et al., 1995ApJ...450..380D; their
01083+5455Aa,Ab Table 9), and we stress that the value (332.7{deg}+/-3.1{deg})
01083+5455Aa,Ab listed by Abt & Willmarth (2006ApJS..162..207A) for the
01083+5455Aa,Ab spectroscopic orbit (of A around the centre of mass of the
01083+5455Aa,Ab system) is incorrect, as it should differ by 180{deg} from the
01083+5455Aa,Ab astrometric value, confirming the suspected confusion. It is in
01083+5455Aa,Ab fact just the value reported by Drummond et al.
01083+5455Aa,Ab (1995ApJ...450..380D), which should not have been copied
01083+5455Aa,Ab without change! Instead, the value (147.9{deg}+/-4.9{deg}) of
01083+5455Aa,Ab Duquennoy & Mayor (1991A&A...248..485D) for the spectroscopic
01083+5455Aa,Ab orbit is correct.
01398-5612AB Indeterminate visual orbit. In the absence of recent
01398-5612AB radial-velocity measurements it is not possible to lift the
01398-5612AB ambiguity on the position of the ascending node.
01418+4237AB Spectroscopic orbits were published by Duquennoy & Mayor
01418+4237AB (1991A&A...248..485D) and Abt & Willmarth
01418+4237AB (2006ApJS..162..207A). The present orbit (Table A.2) improves
01418+4237AB upon those, as it includes several unpublished CORAVEL
01418+4237AB velocities given in Table A.6. Lippincott et al.
01418+4237AB (1983PASP...95..271L) and Soderhjelm (1999A&A...341..121S)
01418+4237AB published astrometric orbits. Here, we obtained a combined
01418+4237AB astrometric/spectroscopic solution by considering the
01418+4237AB astrometric measurements from the Fourth Catalogue of
01418+4237AB Interferometric Measurements of Binary Stars. This solution
01418+4237AB agree well with the existing solutions quoted above.
01425+2016AB This system was announced as an astrometric binary with a period
01425+2016AB of 0.567yr by the Double and Multiple Star Annex (DMSA) of the
01425+2016AB Hipparcos Catalogue (ESA, 1997, Cat. I/239), Cat. I/239).
01425+2016AB However, reprocessing the Hipparcos data along the method
01425+2016AB outlined by Pourbaix (2000A&AS..145..215P) for a combined
01425+2016AB solution including the CORAVEL velocities does not allow us to
01425+2016AB confirm the Hipparcos DMSA/O solution. This system was
01425+2016AB therefore dropped from our final list.
02278+0426AB The most recent and thorough analysis of that system was
02278+0426AB presented by Andrade (2007RMxAA..43..237A), including a revised
02278+0426AB visual orbit. CORAVEL data (Table A.7) make it possible now to
02278+0426AB compute a combined SB2/astrometric orbit, which thus gives
02278+0426AB access for the first time to the masses of the system
02278+0426AB components. The combined orbital elements and other physical
02278+0426AB parameters of the system (such as orbital parallax and
02278+0426AB component masses) are listed in Table A.3, which identifies the
02278+0426AB components as 1 and 2 rather than A and B. It must be stressed
02278+0426AB that there is no easy way to identify for sure the
02278+0426AB spectroscopic component 1 with either visual component A or B,
02278+0426AB since both components fall in the spectrograph slit and are of
02278+0426AB almost equal brightness: Hipparcos gives mHp,A=9.45 and
02278+0426AB mHp,B=9.63. An indirect way to identify components A and B is
02278+0426AB by noting that in Table A.3, the velocity semi-amplitude K2 is
02278+0426AB higher than K1, hence M2 is smaller than M1. Since both
02278+0426AB components lie on the main sequence, component 2 should thus be
02278+0426AB less luminous than component 1, hence component 2 should be
02278+0426AB identified with B. It is possible to check quantitatively this
02278+0426AB assumption by using the mass-luminosity relationship provided
02278+0426AB by Kroupa et al. (1993MNRAS.262..545K), namely MV,1=5.4 for
02278+0426AB M1=0.95M_{sun}_ and MV,2=6.2 for M2=0.85M_{sun}_, or
02278+0426AB MV,2-MV,1=0.8, somewhat larger than the observed
02278+0426AB mHp,B-mHp,A=0.18, but certainly consistent with the error bars
02278+0426AB on M1,2. Although Andrade (2007RMxAA..43..237A) classified
02278+0426AB HD 15285 A as K7V based on several spectral features, among
02278+0426AB which the presence of weak TiO bands, its inferred mass of
02278+0426AB 0.95M_{sun}_ is more typical of a G5V type, while the mass of
02278+0426AB component B would flag it as K0V (Cox, 2000, Allen's
02278+0426AB Astrophysical Quantities (New York: Springer)).
02278+0426AB These masses were derived from the orbital parallax of
02278+0426AB 52+/-2mas, to be compared with the Hipparcos value of
02278+0426AB 60.2+/-1.7mas (ESA, 1997, Cat. I/239) or 58.3+/-1.1mas
02278+0426AB (van Leeuwen, 2007, Cat. I/311), which yield total masses of
02278+0426AB 1.16 and 1.28M_{sun}_, respectively, to be compared with
02278+0426AB 1.8M_{sun}_ for the orbital parallax. From the fractional mass
02278+0426AB M2/(M1+M2)=0.47 (Table A.3), one obtains, (M1,M2)=(0.62,0.54)
02278+0426AB and (0.68, 0.60)M_{sun}_. These values agree much better with a
02278+0426AB K7V spectral type for component A.
02361+0653A The 22 CORAVEL measurements available for component A (spanning
02361+0653A 6837d) yield a standard deviation of 0.29km/s, identical to the
02361+0653A average error on a single measurement. The constancy of the
02361+0653A radial velocity was confirmed by Chubak et al. (2012,
02361+0653A arXiv:1207.6212), who obtained 62 measurements spanning 1299d,
02361+0653A with a standard deviation of 0.142km/s. Hence, radial
02361+0653A velocities cannot be used to lift the ambiguity on the
02361+0653A orbital orientation.
02442+4914AB Indeterminate visual orbit and roughly constant radial velocity
02442+4914AB between 1900 and 1990.
03575-0110AB Indeterminate visual orbit and almost constant radial velocity
03575-0110AB between 1984 and 1993.
04153-0739BC In the triple system STF 518 A-BC, B is the white dwarf omi Eri
04153-0739BC B and C the flare star DY Eri.
04312+5858Aa,Ab Triple system, with the A component being an astrometric binary
04312+5858Aa,Ab in the visual binary STI 2051 AB.
05074+1839AB Visual orbit highly conjectural and radial velocity from
05074+1839AB Duquennoy & Mayor (1991A&A...248..485D) is constant.
06003-3102AC A quadruple system (Tokovinin et al., 2005A&A...441...69L):
06003-3102AC HU 1399 AB (P=67.7yr, a=0.912"), HJ 3823 AC (P=390.6yr,
06003-3102AC a=3.95" by Baize (1980, Inf. Circ. IAU Comm., 26, 80), not
06003-3102AC confirmed by Tokovinin et al., 2005A&A...441...69L),
06003-3102AC TOK 9 C,CE (P=23.7yr, a=0.12"). A, B and C, CE are coplanar
06003-3102AC (Tokovinin et al., 2005A&A...441...69L).
06262+1845AB Triple system, with A known as SB2 with P=6.99d
06262+1845AB (Griffin & Emerson, 1975Obs....95...23G).
06293-0248AB Solution for the SB2 orbit includes masses and orbital parallax
06293-0248AB (Segransan et al., 2000A&A...364..665S). Although not clearly
06293-0248AB stated, the orbital elements listed by Segransan et al.
06293-0248AB (2000A&A...364..665S) correspond to the spectroscopic orbit
06293-0248AB (hence {omega} and {Omega} listed in our Table 3 differ by
06293-0248AB 180{deg} from theirs).
06579-4417AB Indeterminate visual orbit.
07100+3832 The spectro-visual orbit of this system was only recently
07100+3832 computed by Barry et al. (2012ApJ...760...55B).
07175-4659AB The visual orbit is still very uncertain. The total mass of the
07175-4659AB system is abnormally low given the spectral type.
07346+3153AB A difficult system since both A and B are spectroscopic binaries
07346+3153AB (Vinter Hansen et al., 1940LicOB..19...89V), with P=9.21d and
07346+3153AB P=2.93 d, respectively. Batten (1967, IAU Symp., 30, 199) has
07346+3153AB lifted the ambiguity on the ascending node for that system, and
07346+3153AB we used the orbital elements of the 6th Catalogue of Visual
07346+3153AB Binary Orbits to compute the position of the pole, agreeing
07346+3153AB with that of Batten (1967, IAU Symp., 30, 199), allowing for
07346+3153AB the fact that our poles follow the right-hand rule, opposite to
07346+3153AB that of Batten.
07393+0514AB The pole ambiguity was lifted from the radial-velocity drift
07393+0514AB present in the Duquennoy et al. (1991A&AS...88..281D) data.
08592+4803A,BC Indeterminate visual orbit. It might be a quadruple system,
08592+4803A,BC since Aa seems to be a SB1 system with a period P~11yr
08592+4803A,BC (Abt, 1965ApJS...11..429A) although the spectroscopic orbit is
08592+4803A,BC not of an excellent quality.
09006+4147AB The period of 21.05yr for that visual binary is well established
09006+4147AB (Muterspaugh et al., 2010AJ....140.1623M). Based on an older
09006+4147AB (albeit similar) value of the visual period from Heintz (1967,
09006+4147AB VeMun, 7, 31), Abt & Levy (1976ApJS...30..273A) proposed a
09006+4147AB spectroscopic orbit based on Heintz' visual elements plus
09006+4147AB approximate values for the systemic velocity and the
09006+4147AB semi-amplitude, which could account for Abt & Levy's own
09006+4147AB velocity measurements and older ones from Underhill
09006+4147AB (1963PDAO...12..159U). Although it is rather uncertain, this
09006+4147AB orbit is still the one quoted by the SB9 catalogue (Pourbaix et
09006+4147AB al., 2004A&A...424..727P). The spectroscopic orbit is
09006+4147AB difficult to derive because (i) the components are not
09006+4147AB separated widely enough on the sky to record their spectra
09006+4147AB separately; (ii) the velocity semi-amplitude is small; and
09006+4147AB (iii) component A appears to rotate relatively fast. Therefore,
09006+4147AB the available unpublished CORAVEL measurements appear useless,
09006+4147AB since the two components appear hopelessly blended in the
09006+4147AB cross-correlation function. More recent HERMES/Mercator spectra
09006+4147AB (Raskin et al., 2011A&A...526A..69R) have a resolution high
09006+4147AB enough to allow a comfortable double-Gaussian fit of the
09006+4147AB cross-correlation function (CCF; Fig. A.5). Although such a
09006+4147AB fit has not necessarily a unique solution, we found it
09006+4147AB re-assuring that the CCFs for all seven available dates
09006+4147AB (Table A.1) are well fitted with Gaussians having the same
09006+4147AB properties: height ~0.08 and {sigma}=14km/s for the F4V
09006+4147AB component A (V=4.2), and height ~0.04 and {sigma}=4km/s for the
09006+4147AB K0V component B (V=6.5). It thus appears that component A is a
09006+4147AB relatively fast rotator. The assignment of either of the two
09006+4147AB CCF peaks to component A thus relies on the assumption that
09006+4147AB component A, being of spectral type F4V, should correspond to
09006+4147AB the deepest peak when computed with a F0V template.
09006+4147AB The validity of our double-Gaussian fits, and of the resulting
09006+4147AB orbital elements listed in Table A.3, may be assessed a
09006+4147AB posteriori by the comparison of the orbital parallax
09006+4147AB (53.8+/-1.0mas) with the Hipparcos parallax (60.9+/-1.3mas;
09006+4147AB ESA, 1997, Cat. I/239). The discrepancy probably comes from
09006+4147AB the fact that the limited phase coverage for the radial
09006+4147AB velocities does not yet impose strong enough constraints on the
09006+4147AB velocity semi-amplitudes (Fig. A.4). The astrometrically
09006+4147AB derived masses (MA=1.37M_{sun}_, MB=1.04M_{sun}_, in relatively
09006+4147AB good agreement with the spectral types; Martin & Mignard,
09006+4147AB 1998A&A...330..585M; Soderhjelm, 1999A&A...341..121S) are
09006+4147AB different from the types derived from our combined orbit
09006+4147AB (MA=1.73M_{sun}_, MB=1.69M_{sun}_), which also hints at
09006+4147AB inaccurate velocity semi-amplitudes.
09144+5241AB For this long-period binary, the determination of the orbital
09144+5241AB pole is based on the agreement between the variation of the
09144+5241AB radial velocities VA and VB measured between 1910 and 1997 and
09144+5241AB the value predicted using the elements of the visual orbit.
09144+5241AB This result is confirmed by the value of the measurement of
09144+5241AB (VB-VA) performed with the HERMES spectrograph in 2012
09144+5241AB (see Table A.1).
09313-1329AB Mass-ratio derived from the astrometry (Soderhjelm,
09313-1329AB 1999A&A...341..121S). Two HERMES radial-velocity measurements
09313-1329AB obtained one year apart neither showed any significant drift
09313-1329AB (Vr=7.93km/s on JD=2455657.5 and Vr=7.89km/s on JD=2456038.4),
09313-1329AB nor any line doubling, as would be expected for a system
09313-1329AB consisting of two components only 0.6 arcsec apart.
09357+3549AB Indeterminate visual orbit.
10454+3831AB Triple system, Aa being the speckle binary CHR 191. A value of
10454+3831AB (VB-VA) obtained with the HERMES spectrograph in 2012 is
10454+3831AB listed in Table A.1.
11182+3132AB Quadruple system, A and B are both SB1 with P=670.24d and
11182+3132AB P=3.98d respectively (Griffin, 1998Obs...118..273G).
11247-6139AB Abnormally high total mass, inconsistent with the spectral types
13100+1732AB Spectral types and masses of components from ten Brummelaar et
13100+1732AB al. (2000AJ....119.2403T).
13198+4747AB Triple system (Aa=CHR 193; Beuzit et al., 2004A&A...425..997B).
13198+4747AB CORAVEL sees this star as SB3, but no satisfactory attribution
13198+4747AB of the various peaks to the corresponding components could be
13198+4747AB made, making it very difficult to isolate the trend of Vr(A).
13473+1727AB Indeterminate orbit. The component {tau} BooAb is a star with
13473+1727AB planet.
13491+2659AB The pole ambiguity was lifted from unpublished CORAVEL
13491+2659AB velocities yielding the sign of Vr(B)-Vr(A) (=-3.3km/s) during
13491+2659AB the observation span 1983-1988 (Table A.1).
13547+1824 Jancart et al. (2005A&A...442..365J) obtained a combined
13547+1824 spectroscopic/astrometric orbit based on Hipparcos data and the
13547+1824 spectroscopic orbit of Bertiau (1957ApJ...125..696B). The value
13547+1824 of {omega} from Jancart et al. (2005A&A...442..365J) has been
13547+1824 adopted in Table 3.
14514+1906AB The visual orbital period is 151 yr (Soderhjelm,
14514+1906AB 1999A&A...341..121S), so that no strong trend must be expected
14514+1906AB from the radial velocities over three decades. CORAVEL
14514+1906AB observations (Duquennoy et al., 1991A&A...248..485D)
14514+1906AB exhibit a weak upward trend between 1977 (1km/s) and 1991
14514+1906AB (1.4km/s), which is however not significant based on the
14514+1906AB average measurement uncertainty of 0.34km/s. Later measurements
14514+1906AB by Abt & Willmarth (2006ApJS..162..207A) seem to confirm that
14514+1906AB trend, but the trend is made fragile by a possible zero-point
14514+1906AB offset between the two data sets. Nevertheless, the pole quoted
14514+1906AB in Table 3 is based on the assumption that the radial-velocity
14514+1906AB trend is real, which then implies that the node given in the
14514+1906AB 6th USNO Catalogue is the correct one.
14575-2125AB Indeterminate visual orbit.
15038+4739AB Triple star: Bb=eclipsing SB2 with P=0.27d
15038+4739AB (Lu et al., 2001AJ....122..402L).
15527+4227 The Hipparcos Double and Multiple Star Annex (DMSA; ESA, 1997,
15527+4227 Cat. I/239) claims HIP 77760 to be an astrometric binary with
15527+4227 an orbital period of 0.14yr and an inclination of 131.68{deg}.
15527+4227 These values seem, however, incompatible with the absence of
15527+4227 (CORAVEL) radial-velocity variations (33 measurements with a
15527+4227 standard deviation of 0.413km/s, to be compared with the
15527+4227 average instrumental error of 0.380km/s).
16413+3136AB There are many visual orbits available for that system, the most
16413+3136AB recent ones by Baize (1976A&AS...26..177B) and Soderhjelm
16413+3136AB (1999A&A...341..121S). Scarfe et al. (1983JRASC..77..126S)
16413+3136AB already computed an orbit combining visual data and a
16413+3136AB collection of Coude radial velocities. Unpublished CORAVEL
16413+3136AB velocities given in Table A.8 nicely complement Scarfe's
16413+3136AB velocities, yielding a somewhat more accurate orbit as listed
16413+3136AB in Table A.2. A third component has been detected by IR speckle
16413+3136AB interferometry (McCarthy, 1983, IAUCo, 76, 107).
16555-0820AB A triple system composed of M dwarfs, in which all three stars
16555-0820AB are visible in the spectra. Spectroscopic orbits are available
16555-0820AB for the inner (Ba-b) and outer pairs (A-Bab), both as SB2
16555-0820AB (Segransan et al., 2000A&A...364..665S). The two orbits are
16555-0820AB probably coplanar (Mazeh et al., 2001MNRAS.325..343M). The
16555-0820AB whole system is probably septuple.
17121+4540AB A visual orbit for that system was obtained by Hartkopf et al.
17121+4540AB (1996AJ....111..370H). The available CORAVEL velocities shown
17121+4540AB in Table A.9 make it possible to derive a combined orbit for
17121+4540AB the first time. Visual observations are from the CHARA
17121+4540AB database. The new combined orbit is presented in Fig. A.7.
17153-2636AB Irwin et al. (1996PASP..108..580I) derived precise B-A radial
17153-2636AB velocities (except for an acceleration component that they were
17153-2636AB unable to explain). Velocity measurements of Vr(A) and Vr(B)
17153-2636AB were obtained in 2012 by the HERMES spectrograph (Table A.1).
17191-4638AB Indeterminate visual orbit.
17304-0104AB A combined astrometric/spectroscopic solution has been computed
17304-0104AB by Pourbaix (2000A&AS..145..215P) and has been used to compute
17304-0104AB the position of the orbital pole.
17349+1234 Spectral types from Gatewood (2005AJ....130..809G). Kamper et
17349+1234 al. (1989AJ.....98..686K) performed a combined
17349+1234 spectroscopic/astrometric analysis of this system, and their
17349+1234 orbit has been recently updated by Hinkley et al.
17349+1234 (2011ApJ...726..104H), from whom we adopted the orbital
17349+1234 elements without requiring any change to comply with our
17349+1234 conventions.
17364+6820Aa,Ab Velocity measurements of Vr(A) and Vr(B) obtained in 2012 by the
17364+6820Aa,Ab HERMES spectrograph are listed in Table A.1.
17465+2743BC HD 161797 ({mu} Her) is a quadruple system (Raghavan et al.,
17465+2743BC 2010ApJS..190....1R). The components of the wide pair
17465+2743BC STF 2220 AB (35") have common proper motion. The component A is
17465+2743BC an astrometric binary (period of 65 years, Heintz,
17465+2743BC 1994AJ....108.2338H). The components B and C form the visual
17465+2743BC binary AC 7 for which the orbital pole ambiguity has been
17465+2743BC lifted from unpublished CORAVEL velocities, yielding a drift of
17465+2743BC Vr(B) over 1975-1995.
18070+3034AB Based on available CORAVEL velocities (unpublished measurements
18070+3034AB are given in Table A.10), a combined astrometric/spectroscopic
18070+3034AB solution (Table A.2 and Fig. A.8) improves the spectroscopic
18070+3034AB orbital elements provided by Abt & Willmarth
18070+3034AB (2006ApJS..162..207A) for that system. AC 15 AB is a triple
18070+3034AB system, with the separation Aa-Ab amounting to 0.228" and that
18070+3034AB of AB to 0.851" in 2005, according to Scardia et al.
18070+3034AB (2008AN....329...54S).
18428+5938AB Velocity measurements (4 for Vr(A) and one for Vr(B)) obtained
18428+5938AB by the HERMES spectrograph in 2012 are listed in Table A.1.
18570+3254AB A combined astrometric/spectroscopic solution confirms the
18570+3254AB spectroscopic orbital elements provided by Abt & Willmarth
18570+3254AB (2006ApJS..162..207A) for that system. BU 648 AB is a binary
18570+3254AB with an exoplanet (Muterspaugh et al., 2010AJ....140.1657M)
18570+3254AB in coplanar orbits.
19121+0254AB Masses are from Benedict et al. (2001AJ....121.1607B).
19255+0307Aa,Ab Kamper et al. (1989AJ.....98..686K) performed a combined
19255+0307Aa,Ab spectroscopic/astrometric analysis of the Aa-Ab pair. We
19255+0307Aa,Ab adopted the orbital elements from their Table V, except that
19255+0307Aa,Ab 180{deg} was added to their value of {omega}, to conform with
19255+0307Aa,Ab our convention that {omega} corresponds to the visual orbit of
19255+0307Aa,Ab Ab around Aa, rather than to the spectroscopic orbit of Aa
19255+0307Aa,Ab around the centre of mass. One HERMES measurement was obtained
19255+0307Aa,Ab (Table A.1) that reveals for the first time the companion in
19255+0307Aa,Ab the cross-correlation function as a narrow peak on top of the
19255+0307Aa,Ab broad peak (Vrsini=84km/s) due to the FV primary (Fig. A.9).
19255+0307Aa,Ab The companion does not rotate fast. From the orbit described
19255+0307Aa,Ab in Kamper et al. (1989AJ.....98..686K), we estimate that the
19255+0307Aa,Ab HERMES data point (Vr(Aa)=-26.68km/s) has been taken at orbital
19255+0307Aa,Ab phase 0.54+/-0.14, when the velocity is km/s higher than the
19255+0307Aa,Ab centre of mass (CoM) velocity. The CoM velocity is thus
19255+0307Aa,Ab estimated to be km/s. Combined with Vr(Ab)=-37.70km/s, this
19255+0307Aa,Ab yields a surprisingly high mass ratio MAa/MAb of 5.6, or a mass
19255+0307Aa,Ab of 0.29M_{sun}_ for the companion if the primary is a F0V star
19255+0307Aa,Ab of mass 1.6M_{sun}_. The corresponding spectral type would
19255+0307Aa,Ab then be M4V for the Ab component, 8.6mag fainter than the
19255+0307Aa,Ab primary component. The close pair WDS 19255+0307Aa,Ab, seems to
19255+0307Aa,Ab form a triple system with the wide pair (WDS 19255+0307AB=
19255+0307Aa,Ab BUP 190, separation 96 to 133"), but the physical nature of
19255+0307Aa,Ab this system is yet to be confirmed.
21000+4004AB Fekel et al. (1978AJ.....83.1445F) found that the visual
21000+4004AB component A of KUI 103 is itself a spectroscopic binary with a
21000+4004AB period of 3.27 d, but no information is available about
21000+4004AB coplanarity (Tokovinin, 2008MNRAS.389..925T). Pourbaix
21000+4004AB (2000A&AS..145..215P) has made a combined analysis of the
21000+4004AB visual and spectroscopic data. However, the authors note that
21000+4004AB this orbital solution is somewhat uncertain, given the large
21000+4004AB error bars and inconsistencies in the derived values for
21000+4004AB stellar masses and orbital parallax. Thus, we decided to base
21000+4004AB our determination of the orbital pole of this system on the
21000+4004AB analysis of the published radial velocity measurements
21000+4004AB (Pourbaix, 2000A&AS..145..215P) and the orbital elements of the
21000+4004AB new visual orbit proposed by Docobo & Ling (2010, IAU
21000+4004AB Commission on Double Stars, 171, 1).
21069+3845AB The mass ratio is taken from Gorshanov et al.
21069+3845AB (2006Ap.....49..386G). The node assignment is based on the
21069+3845AB difference Vr(B)-Vr(A)~+1km/s>0, as provided by Table 1 of
21069+3845AB Gorshanov et al. (2006Ap.....49..386G) and confirmed by
21069+3845AB unpublished CORAVEL measurements.
22234+3228AB The total mass seems too high for the spectral type.
22280+5742AB Masses are from Delfosse et al. (2000A&A...364..217D). Among the
22280+5742AB many radial velocities available in the literature for the
22280+5742AB components of this system, we give the highest weight to the
22280+5742AB measurement [Vr(A)=-32.7km/s and Vr(B)=-33.2km/s] by Gizis et
22280+5742AB al. (2002AJ....123.3356G) because (i) that measurement is
22280+5742AB precisely dated (JD 2450005.6) and on the same night for A
22280+5742AB and B; and (ii) the 0.5km/s velocity difference is consistent
22280+5742AB with the prediction from the visual orbit. The measurement
22280+5742AB (Vr(A)=-34.0km/s and Vr(B)=-35.0km/s) by Delfosse et al.
22280+5742AB (1998A&A...331..581D) is equally useful (its epoch is not as
22280+5742AB precisely known as that report by Gizis, but it was obtained
22280+5742AB between September 1995 and March 1997, a short time span with
22280+5742AB respect to the 44.7yr orbital period); the 1km/s velocity
22280+5742AB difference agrees better with the prediction from the visual
22280+5742AB orbit than Gizis' 0.5km/s. The determination of the sign of
22280+5742AB Vr(B)-Vr(A)=-1km/s is important and it is opposite to the
22280+5742AB prediction from the visual orbital elements from the 6th COVBS.
22280+5742AB It is thus necessary to add 180{deg} to the values of {Omega}
22280+5742AB and {omega} listed in the 6th COVBS. It is noteworthy that the
22280+5742AB velocity values listed in the Wilson - Evans - Batten
22280+5742AB catalogue (Duflot et al., 1995A&AS..114..269D, Vr(A)=-24.0km/s
22280+5742AB and Vr(B)=-28.0km/s) or in Reid et al. (1995AJ....110.1838R)
22280+5742AB (Vr(A)=-16.0km/s and Vr(B)=-29.0km/s), although the differences
22280+5742AB are much larger than anticipated, always have Vr(B)-Vr(A)<0.
23317+1956AB Indeterminate visual orbit.
23524+7533AB Indeterminate visual orbit. A triple system with A being SB2
23524+7533AB with a period of 7.75d (Christie, 1934ApJ....80..181C).