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CABSCAT - Chromospherically Active Binary Stars Catalog

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Overview

This 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. This version updates and replaces the 1988 catalog of similar information. (Strassmeier et al., 1988). A key to the number codes used for the references in the present database is given in the Strassmeier et al (1993, A&AS, 100,173) paper. This paper also has short notes for each entry in the catalog that has not been included in the present online version. A "W" precedes numerical values that are approximately equal to whatever follows the flag.

Catalog Bibcode

1993A&AS..100..173S

References

Strassmeier K. G., Hall D. S., Zeilik M., Nelson E., Eker Z., Fekel F. C., 1988 A&AS, 72, 192

Strassmeier K. G., Hall D. S., Fekel F. C., and Scheck M., 1993 A&AS, 100, 173

Parameters

A_Sin_I
A sin(i) hot-cool

Abs_Vmag
M(V) hot-cool

Alt_Name
Identifications originating from other sources: 

     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,
      Gl = Gliese Catalog
      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,
    1E.. = First EINSTEIN catalog of x-ray sources,
     Ynn = Yale Catalog Volume nn number,
     Cnn = Cape Photographic Catalog Volume nn number.

Bayer
Bayer designation.

BII
The galactic latitude of the object.

BV_Color
B-V Color: Mean color in the standard Johnson UBVRI system for the hot/cool component respectively. 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) [ARA&A 4, 193], FitzGerald (1970) [A&A 4, 34], or Schmidt-Kaler (1982) [in: Landolt-Boernstein,Vol. 2b, p.1]. An asterisk, *, means that this entry is measured in the Kron-Cousins UBV(RI)KC system. For transformation to the standard Johnson system, ee, e.g., Bessell (1979) [PASP 91, 589]. Colors in brackets, "[ ]", are assumed from the spectral classification. Slash, "/", always separates values for the hot/cool component, respectively. Braces, "{ }", denote the close binary in a spectroscopic triple system. A color with an asterisk, "*", in front is measured in the Kron-Cousins RI system. All other values are in the Johnson UBVRI system. "const" in the "Delta Vave" column means that photometry has been obtained but no spot wave has been observed.

CaII_Emission
CaII H&K emission. Singly ionized calcium H and K emission. This 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 field. 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, and (E) = emission strength after Hearnshaw's scale. 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.

Class
The Browse classification type. This classification is based on the Spect_Type parameter, using, in the event of multiple values in that field, the first value offered.

Conj_Component
The component behind the conjunction.

Conj_Date
Heliocentric Julian date of conjunction -2400000 with the (presumed) hotter star behind. If the star is not an eclipsing binary, then we have computed Tconj either from the time of periastron passage or, if e = 0, from the time of quadrature in order to simulate primary eclipse.

Dec_1950
Declination in 1950 coordinates

Dec
The Declination of the object.

Delta_V
Maximum amplitude of the "wave" in V passband, due to spots, not ellipticity or reflection. CONST means that photometry has been obtained but no wave has been observed.

Distance
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 an M(V) value itself in brackets, as explained below. Used in calculating W Coords.

DM_Number
Durchmeusterung Identification.

Eccentricity
Eccentricity.

Eclipse
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.

Flamsteed
Flamsteed name.

Halpha
Balmer Halpha line behavior. 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.

HD_Number
HD/HDE identification.

HR_Number
HR number.

IAU_Archive
File in the IAU Commission No. 27 "Archive of Unpublished observations of Variable Stars" (Breger 1985, PASP 97, 85; Breger, Jaschek, Dubois 1990, IBVS 3422).

Inclination
Inclination of the pole of the orbital plane or of the rotation axis, in degrees.

IUE_Archive
Observed with IUE, possible through March 21, 1990.

LII
The galactic longitude of the object.

Mag_Type
Magnitude type.

Masses
Mass in solar units of the hot/cool component respectively. A blank 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.

Name
Designation by which the source is most commonly identified. Alternate names are also included in other fields within the database.

Omega
Longitude of periastron in degrees.

Orbital_Period
Orbital period in days.

Orbital_Variability
Orbital period variability. More quantitative results in terms of (dlnP/dt) are given in the Notes. Y = yes, N = No.

Photo_Period
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 we have computed Pphtm from the wave migration period using the relation 1/Pmigr = 1/Pphtm - 1/Porb; if so, we have 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!

Proper_Motion_Dec
Proper Motion in Dec.

Proper_Motion_RA
Proper motion in RA

RA_1950
Right Ascension in 1950 coordinates

RA
The Right Ascension of the object.

Radii
Radius in solar units of the hot/cool component respectively. A " " indicates that (R sin i) is listed. Same convention as found in masses for cases of identical spectral class or equal mass: 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.

Radio_Flux
Radio flux density.

Ref_A_Sin_I
A sin(i) reference

Ref_Abs_Vmag
M(V) reference

Ref_BV_Color
BV COLOR reference

Ref_Caii_Emission
CaII emission reference

Ref_Conj_Date
Conj date reference

Ref_Delta_V
Delta wave reference

Ref_Distance
Reference for the value of Distance.

Ref_Eccentricity
Reference for Eccentricity.

Ref_Eclipse
Reference for the Eclipse field.

Ref_Halpha
Reference for Balmer Halpha line behavior.

Ref_Inclination
Reference for Inclination.

Ref_Masses
Reference for Masses. Note that all entries in the Masses field followed by the reference (727) cannot be found in that paper, but the original authors used their orbital elements to determine those entries.

Ref_Omega
Reference for Omega.

Ref_Orbital_Period
P(orb) reference

Ref_Photo_Period
Photo Period reference

Ref_Proper_Motion
Proper motion reference

Ref_Radii
Reference for radii.

Ref_Radio_Flux
Radio flux reference

Ref_RI_Color
RI COLOR reference

Ref_SB_Type
Binary nature reference

Ref_Semi_Amplitude
K reference

Ref_Spect_Type
SPECT TYPE reference

Ref_Sys_Velocity
Systemic Velocity reference

Ref_UB_Color
UB COLOR reference

Ref_V_Sin_I
V sin(i) reference

Ref_Variability
Reference for the Orbital period Variability.

Ref_Vmax
Reference for VMax.

Ref_Vr_Color
VR COLOR reference

Ref_Xray_Lum
X-ray Luminosity reference

RI_Color
R-I color: Mean color in the standard Johnson UBVRI system for the color (outside eclipse) is listed. Values in brackets, [ ], are assumed from the spectral type versus color relations of Johnson (1966) [ARA&A 4, 193], FitzGerald (1970) [A&A 4, 34], or Schmidt-Kaler (1982) [in: Landolt-Boernstein,Vol. 2b, p.1]. An asterisk, *, means that this entry is measured in the Kron-Cousins UBV(RI)KC system. For transformation to the standard Johnson system, ee, e.g., Bessell (1979) [PASP 91, 589]. Colors in brackets, "[ ]", are assumed from the spectral classification. Slash, "/", always separates values for the hot/cool component, respectively. Braces, "{ }", denote the close binary in a spectroscopic triple system. A color with an asterisk, "*", in front is measured in the Kron-Cousins RI system. All other values are in the Johnson UBVRI system. "const" in the "Delta Vave" column means that photometry has been obtained but no spot wave has been observed.

SAO_Number
SAO designation.

SB_Type
Binary Nature, as appearing in the following table: 

      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. v sin i Projected rotational velocity for
            the hot/cool component in km/s.

Semi_Amplitude
Semi-amplitude of the hot/cool component in km/s. 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.

Spect_Type
Spectral type and luminosity class of the hot/cool component, always in that order.

Sys_Velocity
System's center-of-mass radial velocity in km/s.

U_Velocity
Space velocities relative to the Sun in km/s. U directs toward the galactic center (= right-hand system).

UB_Color
U-B Color: Mean color in the standard Johnson UBVRI system for the hot/cool component respectively. 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) [ARA&A 4, 193], FitzGerald (1970) [A&A 4, 34], or Schmidt-Kaler (1982) [in: Landolt-Boernstein,Vol. 2b, p.1]. An asterisk, *, means that this entry is measured in the Kron-Cousins UBV(RI)KC system. For transformation to the standard Johnson system, ee, e.g., Bessell (1979) [PASP 91, 589]. Colors in brackets, "[ ]", are assumed from the spectral classification. Slash, "/", always separates values for the hot/cool component, respectively. Braces, "{ }", denote the close binary in a spectroscopic triple system. A color with an asterisk, "*", in front is measured in the Kron-Cousins RI system. All other values are in the Johnson UBVRI system. "const" in the "Delta Vave" column means that photometry has been obtained but no spot wave has been observed.

V_Sin_I
V sin(i) hot-cool

V_Velocity
Space velocities relative to the Sun in km/s. V is in the direction of the galactic rotation.

Var_Name
General Catalog of Variable Stars identification, or New Catalog of Suspected Variable Stars number.

Vmax
Maximum brightness in a V bandpass. "pg" means that only an old photographic magnitude was available.

Vmax_Uncert
Uncertainty flag (":") for VMax.

VR_Color
V-R color: Mean color in the standard Johnson UBVRI system for the hot/cool component respectively. 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) [ARA&A 4, 193], FitzGerald (1970) [A&A 4, 34], or Schmidt-Kaler (1982) [in: Landolt-Boernstein,Vol. 2b, p.1]. An asterisk, *, means that this entry is measured in the Kron-Cousins UBV(RI)KC system. For transformation to the standard Johnson system, ee, e.g., Bessell (1979) [PASP 91, 589]. Colors in brackets, "[ ]", are assumed from the spectral classification. Slash, "/", always separates values for the hot/cool component, respectively. Braces, "{ }", denote the close binary in a spectroscopic triple system. A color with an asterisk, "*", in front is measured in the Kron-Cousins RI system. All other values are in the Johnson UBVRI system. "const" in the "Delta Vave" column means that photometry has been obtained but no spot wave has been observed.

W_Velocity
Space velocities relative to the Sun in km/s. W points in the direction of the galactic north pole. For the computations, the procedure described in Johnson and Soderblom (1987) [AJ 93, 864] were followed. The distances and center of mass velocities were used.

X_Coords
Rectangular space coordinates relative to the sun in parsecs. X is in the direction toward the galactic center.

Xray_Lum
X-ray luminosity, in 1031 ergs s-1. "fx" means that only a flux measure in mW/m2 (erg/cm2/s) is available. Spectral types in brackets, [], are assumed. A slash, /, always separates values for the hot/cool component, respectively. Braces, {}, denote the close binary in a spectroscopic triple system.

Y_Coords
Rectangular space coordinates relative to the sun in parsecs. Y is in the direction of the galactic rotation.

Z_Coords
Rectangular space coordinates relative to the sun in parsecs. Z is the distance from the galactic plane and is positive toward the galactic north pole.

Contact Person

Questions regarding the CABSCAT database table can be addressed to the HEASARC User Hotline.
Page Author: Browse Software Development Team
Last Modified: Wednesday, 29-Jan-2020 16:34:19 EST