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V/76        Chromospherically Active Binaries (Strassmeier+ 1993)

A Catalogue of Chromospherically Active Binary Stars Strassmeier K.G., Hall D.S., Fekel F.C., and Scheck M. <Astron. Astrophys. Suppl. Ser., 100, 173 (1993)> =1993A&AS..100..173S
ADC_Keywords: Stars, double and multiple ; Cross identifications ; Combined data ; Stars, emission ; Stars, variable Abstract: The catalog contains 206 spectroscopic binary systems with at least one late-type component that shows Ca II H and K emission in its spectrum. These systems include the classical RS CVn binaries and BY Dra binaries. The catalog summarizes information on the photometric, spectroscopic, orbital, and physical properties of the systems as well as space motions and positions. Up to 42 "parameters" for each stellar system are listed followed by the appropriate reference to direct interested colleagues to the original papers. A comprehensive selection of further information for each star is given in the individual notes. In addition, the catalog contains a candidate list of 138 stars that have similar characteristics but are not definitely known binaries or have not had Ca II H and K emission observed. This version updates and replaces the 1988 catalog of similar information. (Strassmeier et al., 1988). Introduction: Stars always appear in order of increasing right-ascension for the epoch 2000.0. For the current version of the catalog, the literature was searched through December 31, 1991 although a few later references are included. Additionally, some entries are cited with "private communication", which make this catalog also a first-hand source. A number in parentheses behind an entry always corresponds to a reference given in the bibliography. See the 1988 publication for specific requirements and restrictions in compiling these catalogs. See the source reference for more details about this catalog. The following binary systems, which were listed in the first edition of the catalog, were not included in the present edition due to insufficient evidence for chromospheric activity: eta And 26 Aql 4 UMi nu2 Sgr tau Sgr the following stars are chromospherically active but are components in a "wide" binary and were not included. HD 25893 HD 79211 Forty three new binary systems have been included in the present edition. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file doc.tex 84 623 LaTeX description adc.sty 78 68 Style file required to process doc.tex table1.dat 104 206 Cross references table2.dat 144 206 Photometric properties table3.dat 164 206 Spectroscopic properties table4.dat 154 206 Orbital elements table5.dat 131 206 Stellar properties and general information table6.dat 133 206 Positions and space motions table7.dat 132 436 Candidate list notes.tex 120 1940 Notes in LaTeX refs.dat 206 883 References refs.tex 81 1966 References in LaTeX
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 6- 15 A10 --- name *Variable name 18- 24 A7 --- HD HD/HDE number 26- 29 I4 --- HR ?HR number 32- 42 A11 --- Bayer Bayer name 45- 50 A6 --- Flam Flamsteed name 53- 63 A11 --- DM DM number 66- 68 A3 --- --- [SAO] 70- 75 I6 --- SAO ?SAO number 78-104 A27 --- other *Identifications given by other sources
Note on name: "General Catalog of Variable Stars" identification (cat. II/139) or NSV = "New Catalog of Suspected Variable Stars" number (cat. II/140). Note on other: ADS = Aitken Double Star. (The angle brackets,<>; indicate which of the visual components is the active binary. The parentheses, ( ), indicate the visual component or components that are included in the V-magnitude listed in File 2). GC = General Catalog I/113 Gl = Gliese Catalog V/70 BV = Bamberg Variable, CZ = Cape Zone Star number, FK4 = Fundamental Katalog No. 4, AGK2= Zweiter Katalog der Astronomischen Gesellschaft, AGK3= Dritter Katalog der Astronomischen Gesellschaft, LDS = Luyten Double Star, OS = Otto Struve Variable, P = Prager Variable, S = Sonneberg Variable, vB = van Buren number, SVS = Soviet Variable Star, HV = Harvard Variable, Lal = Lallande Star, Boss= Boss number, BPM = Bruce Proper Motion survey number, PPM = Proper Motion catalog I/146, I/193 1E = First EINSTEIN catalog of X-ray sources, Ynn = Yale Catalog Volume nn number, Cnn = Cape Photographic Catalog Volume nn number.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 5- 18 A14 --- name More commonly used name from table1.dat 19- 25 A7 --- HD HD/HDE number + component 26 A1 --- magtyp Magnitude type 27- 32 F6.3 mag Vmax *? Vmax 33 A1 --- u_Vmax Uncertainty flag (:) on Vmax 34- 38 A5 --- r_Vmax Reference for Vmax 39- 46 A8 mag del *Delta wave 47- 51 A5 --- r_del Delta wave reference 52- 60 A9 d per *Photometric period 61- 69 A9 --- r_per Reference for photometric period 71- 82 A12 mag U-B *< U - B > hot/cool 83- 87 A5 --- r_U-B Reference for < U - B > 88- 98 A11 mag B-V *< B - V > hot/cool 99-103 A5 --- r_B-V Reference for < B - V > 105-119 A15 mag V-R *< V - R > hot/cool 120-124 A5 --- r_V-R Reference for < V - R > 125-139 A15 mag R-I *< R - I > hot/cool 140-144 A5 --- r_R-I Reference for < R - I >
Note on Vmax: Maximum brightness in V bandpass. "pg" means that only an old photographic magnitude was available. Note on del: Maximum amplitude of the "wave" in V passband, due to spots, not ellipticity or reflection. CONST = photometry has been obtained but no wave has been observed. Note on per: Photometric (= rotation) period, in days, derived from the light curve. Rotation periods from (v sin i) measurements are not included. If "(orb)" is given, then the photometric period is nearly the same as the orbital period in File 4. Sometimes Pphtm has been computed from the wave migration period using the relation 1/Pmigr = 1/Pphtm - 1/Porb; if so, this has been mentioned that in the individual notes. Due to the inherently irregular behavior of large starspot groups, the photometric period in all spotted stars is intrinsically variable! Note on U-B B-V V-R R-I: Mean colors in the standard Johnson UBVRI system for the hot/cool component respectively, separated by a slash, "/". If no slash, is given, then the combined color (outside eclipse) is listed. Values in brackets, [ ], are assumed from the spectral type versus color relations of Johnson (1966), FitzGerald (1970), or Schmidt-Kaler (1982). Braces, " ", denote the close binary in a spectroscopic triple system. * = entry is measured in the Kron-Cousins UBV(RI)KC system. All other values are in the Johnson UBVRI system. For transformation to the standard Johnson system, see, e.g., Bessell (1979).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 5- 18 A14 --- name More commonly used name from table1.dat 19- 25 A7 --- HD HD/HDE and component 26- 42 A17 --- spec *Spectral type hot/cool 43- 51 A9 --- r_spec Spectral type reference 53 A1 --- bin *[123Y] Binary nature 55- 59 A5 --- r_bin Binary reference 61- 69 A9 km/s vsini Projected rotational velocity for hot/cool 71- 79 A9 --- r_vsini V sin(i) reference 80- 94 A15 --- Caem *CaII H&K emission 95-103 A9 --- r_Caem CaII emission reference 105-118 A14 --- Halp *Balmer Halpha line behavior 120-128 A9 --- r_Halp Hα reference 129-137 A9 10+24W X *X-ray luminosity (10+31 erg/s) 138-146 A9 --- r_X X-ray reference 147-155 A9 mJy rad Radio flux density 156-164 A9 --- r_rad Radio flux reference
Note on spec: Spectral type and luminosity class of the hot/cool component, respectively, separated by a slash "/". Spectral types and luminosity classes in brackets, "[ ]", are assumed. Braces, " ", denote the close binary in a spectroscopic triple system. Note on bin: Binary nature. SB1 = single-line spectrum SB2 = double-line spectrum SB3 = three components are seen in the spectrum (spectroscopic triple system) Y = yes, spectroscopic binary, but not yet known if the spectrum is single-or double-lined. Note on Caem: Singly ionized calcium H and K emission. This column contains information on the strength of the emission as well as to which component the emission belongs. Absolute emission-line surface fluxes are given, if available, in the "Notes". cool = the cooler component is the emitter hot = the hotter component is the emitter both = both components show H and K emission class A, B, C, D, (E) = emission strength after Hearnshaw's scale, (see Figure 1 in Strassmeier et al. 1988) IK = 5, 4, 3, (2) = strength of the K-emission line in terms of Wilson's eye-estimated intensities on a scale from 0 (no) to 5 ("strong") emission. Note on Halp: abs. = "normal" absorption, em. = emission above the continuum, fld-in abs. = absorption profile "filled-in" with (presumably) chromospheric emission, strong abs. = strong absorption profile, mod. abs. = moderate absorption (this terminology is taken whenever an author used it but is equivalent to "filled-in abs."), wk abs. = weakly filled-in absorption profile (in these cases the degree of "filling-in" is not obviously visible by visual inspection but significant when a standard star spectrum is subtracted). flares = Hff flare has been observed. For further explanation, the original reference should be examined. Note on X: f_x = only a flux measure in mW/m2 (erg/cm2/s) is available.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 5- 18 A14 --- name More commonly used name from table1.dat 19- 25 A7 --- HD HD/HDE and component 26- 34 A9 d per Orbital period 36- 40 A5 --- r_per P(orb) reference 42- 43 A2 --- pervar *Orbital period variability 47- 55 A9 --- r_pervar Period variability reference 58 A1 --- comp *Component behind at conjunction 59- 69 F11.5 d JD *? Heliocentric Julian date - conjunction 70- 74 A5 --- r_JD Conjunction date reference 75- 82 A8 km/s V0 System's center-of-mass radial velocity 83- 88 A6 --- r_V0 V0 reference 89-100 A12 km/s K *Semiamplitude of the hot/cool component 101-109 A9 --- r_K K reference 110 A1 --- --- [(] parentheses in record 155 only 111-114 F4.3 --- e ? Eccentricity 115 A1 --- --- [)] parentheses in record 155 only 116-120 A5 --- r_e Eccentricity reference 122-126 F5.1 deg omega ? Longitude of periastron 128-132 A5 --- r_omega omega reference 133-144 A12 10+6km asini *Separation a sin(i) for hot/cool 146-154 A9 --- r_asini a sin(i) reference
Note on pervar: Orbital period variability. More quantitative results in terms of (dlnP/dt) are given in the individual notes. y = yes n = no Note on comp: p = primary behind s = secondary behind t = tertiary behind Note on JD: Heliocentric Julian date of conjunction -2400000 with the (presumed) hotter star behind. If the star is not an eclipsing binary, then JD has been computed either from the time of periastron passage or, if e = 0, from the time of quadrature in order to simulate primary eclipse. Note on K: If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. Note on asini: (a sin i) = total semimajor axis if no slash, /, is given (a1sin i)/(a2 sin i) = semimajor axis for the orbit of the hot/cool component respectively. "a =" in the (a sin i) column means, that the sum of the orbital semimajor axes is listed. If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. Braces, " ", denote the close binary in a spectroscopic triple system.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 5- 18 A14 --- name More commonly used name from table1.dat 19- 25 A7 --- HD HD/HDE and component 27- 33 A7 pc dist *Distance 34- 38 A5 --- r_dist *Distance reference 40- 53 A14 mag Vmag *M(V) of hot/cool components 55- 59 A5 --- r_Vmag *M(V) reference 60- 74 A15 solMass mass *Masses of hot/cool components 76- 80 A5 --- r_mass *Masses reference 82- 91 A10 solRad rad *Radii of hot/cool components 92-100 A9 --- r_rad *Radii reference 102-105 A4 --- ecl *Eclipse 107-111 A5 --- r_ecl *Eclipse reference 113-118 A6 deg i *Inclination 119-123 A5 --- r_i *Inclination reference 125-127 A3 --- IUE *IUE archive 129-131 A3 --- IAU *IAU Comm. 27 archive
Note on dist: Distance in parsecs. If no reference is given, then the value has been computed from the absolute visual magnitude already given in the catalog. No interstellar absorption was taken into account. A value in brackets, [ ], has been computed from a V value itself in brackets, as explained below. Note on r_dist, r_Vmag, r_mass, r_rad, r_ecl, r_i: Dashes, "-", in a reference column mean that this entry has been computed by the authors. Note on Vmag: Absolute visual brightness. If no reference is given, then the value has been computed from dist. A value in brackets, [ ], is an assumption from the spectral type. Note on mass: Mass in solar units of the hot/cool component respectively. A ">" indicates that (m sin3 i) is listed, and "f(m)" indicates that the mass-function is given. If both stars have the same spectral class, then the more massive star is listed first. If both stars have the same mass, then the larger star is listed first. (Note that all entries in the "MASSES" bytes followed by the reference "(727)" can't be found in that paper, but their orbital elements have been used to determine these entries.) A slash, "/", always separates values for the hot/cool component, respectively. If no slash is given, then the combined value is listed. Note on rad: Radius in solar units of the hot/cool component respectively. A " " indicates that (R sin i) is listed. Same convention as above for cases of identical spectral class or equal mass. A slash, "/", always separates values for the hot/cool component, respectively. If no slash is given, then the combined value is listed. Note on ecl: Type of eclipse. It means: NONE = Not eclipsing, TOT = complete (total/annular) eclipses, PRTL = partial eclipses, YES = an eclipse has been observed, but it is not known if partial or total PSBL = it is possible that eclipses take place but further observations are necessary to confirm it. Note on i: Inclination of the pole of the orbital plane or of the rotation axis, in degrees. Note on IUE: Observed with IUE (through March 31, 1990)? Note on IAU: File in the IAU Commission No. 27 "Archive of Unpublished Observations of Variable Stars" (Breger 1985; Breger, Jaschek, Dubois 1990, IBVS 3422). Values in brackets, "[ ]", are assumed. Braces, " ", denote the close binary in a spectroscopic triple system.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+ Catalog sequence number 5- 18 A14 --- name More commonly used name from table1.dat 19- 25 A7 --- HD HD/HDE and component 27- 28 I2 h RAh Right Ascension J2000.0 (hours) 30- 31 I2 min RAm Right Ascension J2000.0 (minutes) 33- 36 F4.1 s RAs Right Ascension J2000.0 (seconds) 39 A1 --- DE- Declination J2000.0 (sign) 40- 41 I2 deg DEd Declination J2000.0 (degrees) 43- 44 I2 arcmin DEm Declination J2000.0 (minutes) 46- 47 I2 arcsec DEs Declination J2000.0 (seconds) 50- 55 F6.2 deg GLON Galactic longitude 58- 63 F6.2 deg GLAT Galactic latitude 66- 68 I3 pc dist ? Distance from table5.dat 71- 76 F6.1 km/s V0 ? Systemic Velocity from table4.dat 79- 83 I5 mas/yr pmRA ? Proper motion in Right Ascension 85- 89 I5 mas/yr pmDE ? Proper motion in Declination 91- 95 A5 --- r_V0 Systemic velocity reference 98-101 I4 pc X *? X coordinate in galactic plane 103-106 I4 pc Y *? Y coordinate in galactic plane 108-111 I4 pc Z *? Z coordinate above galactic plane 114-119 F6.1 km/s U *? U velocity component 121-126 F6.1 km/s V *? V velocity component 128-133 F6.1 km/s W *? W velocity component
Note on X Y Z: Rectangular space coordinates relative to the sun in parsecs. X is in the direction toward the galactic center, Y is in the direction of the galactic rotation, and Z is the distance from the galactic plane and is positive toward the galactic north pole. Note on U V W: Space velocities relative to the Sun in km/s. U directs toward the galactic center (= right-hand system), V is in the direction of the galactic rotation, and W points in the direction of the galactic north pole. For the computations the procedure described in Johnson and Soderblom (1987) was followed. The distances (`dist') and center-of-mass velocities (`V0') from files table5.dat and table4.dat respectively (reproduced in this file for convenience) were used.
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/206]+= Number, repeated for continuations 6- 26 A21 --- id HD and other Identification 27- 31 F5.2 mag Vmag ? V magnitude, mean brightness in V passband 33- 48 A16 --- chr *Active Chromosphere? 50- 54 A5 --- r_chr Activity reference 57- 66 A10 --- bin *Spectroscopic Binary system? 68- 72 A5 --- r_bin Binary reference 75-132 A58 --- note Individual notes
Note on chr: Active chromosphere? This column lists whether there is observational evidence for the existence of an active chromosphere or not. HK emission = CaII H and K emission lines were observed x-ray source = the star has been detected as an x-ray source H_a em. = Hα line is in emission H_a fld-in = Hα line is in absorption but "filled in" by (presumably) chromospheric emission ? = no observations available Note on bin: Spectroscopic binary system? SB1 = single-lined spectrum SB2 = double-lined spectrum yes = yes, the star is a binary but more observations are needed v_r const? = constancy of measured radial velocities is questioned eclipsing = the system is an eclipsing binary ? = no observations available
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ref Reference Number 5-206 A202 --- text Text of Reference
Remarks: Supersedes V/71/ References: Bessell M.S. 1979, Publ. Astron. Soc. Pac., 91, 589. (1979PASP...91..589B) Breger M. 1985, Publ. Astron. Soc. Pac., 97, 85. (1985PASP...97...85B) Breger M., Jaschek, Dubois 1990, Inf. Bull. Variable Stars, 3422. FitzGerald 1970, Astron. Astrophys., 4, 234. Johnson D.R. 1966, Annu. Rev. Astron. Astrophys., 4, 193. Johnson D.R., and Soderblom D.R. 1987, Astron. J., 93, 864. (1987AJ.....93..864J) Schmidt-Kaler 1982, in: Landolt-Boernstein, Vol. 2b, p.1. Strassmeier K.G., Hall D.S., Fekel F.C., and Scheck M., 1992 Astron. Astrophys. Suppl. Ser., 100, 173. (1993A&AS..100..173S) Strassmeier K.G., Hall D.S., Zeilik M., Nelson E., Eker Z. 1988, Astron. Astrophys. Suppl. Ser., 72, 291. (1988A&AS...72..291S)
(End) Nancy Grace Roman [SSDOO/ADC] (modified J.A. Watko 15-Aug-1996)
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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