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V/76 Chromospherically Active Binaries (Strassmeier+ 1993)
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A Catalogue of Chromospherically Active Binary Stars
Strassmeier K.G., Hall D.S., Fekel F.C., Scheck M.
<Astron. Astrophys. Suppl. Ser., 100, 173 (1993)>
=1993A&AS..100..173S
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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:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [1/206]+ Catalog sequence number
6- 15 A10 --- name *Variable name
18- 24 A7 --- HD HD/HDE number
26- 29 A4 --- HR HR number
32- 42 A11 --- Bayer Bayer name
45- 50 A6 --- Flam Flamsteed name
53- 63 A11 --- DM DM number
66- 68 A3 --- SAOzone SAO zone
70- 75 A6 --- SAOnum SAO number
78-104 A27 --- other *Identifications given by other sources
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Note on name:
"General Catalog of Variable Stars" identification or
NSV = "New Catalog of Suspected Variable Stars" number.
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,
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.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [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 V *? Vmax
33 A1 --- u_V Uncertainty flag (:) on V
34- 38 A5 --- r_V 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 >
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Note on V:
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).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [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 H{alpha} line behavior
120-128 A9 --- r_Halp H{alpha} 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
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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.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [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 --- paren1 *[ (] parentheses
111-114 F4.3 --- e ? Eccentricity
115 A1 --- paren2 *[ )] parentheses
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
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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 paren*:
Parentheses appear here only in record 155. The meaning is unknown.
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.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [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 V *M(V) of hot/cool components
55- 59 A5 --- r_V *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
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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_*:
Dashes, "-", in a reference column mean that this entry has been computed
by the authors.
Note on V:
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 sin^3^ 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.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [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 2000.0 (hours)
30- 31 I2 min RAm Right Ascension 2000.0 (minutes)
33- 36 F4.1 s RAs Right Ascension 2000.0 (seconds)
39 A1 --- DE- Declination 2000.0 (sign)
40- 41 I2 deg DEd Declination 2000.0 (degrees)
43- 44 I2 arcmin DEm Declination 2000.0 (minutes)
46- 47 I2 arcsec DEs Declination 2000.0 (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
103-106 I4 pc Y *? Y
108-111 I4 pc Z *? Z
114-119 F6.1 km/s U *? U
121-126 F6.1 km/s V *? V
128-133 F6.1 km/s W *? W
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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.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- num [1/206]+? Number; blank indicates continuation
6- 26 A21 --- id HD and other Identification
27- 31 F5.2 mag V ? 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
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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. = H{alpha} line is in emission
H_a fld-in = H{alpha} 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
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- ref Reference Number
5-206 A202 --- text Text of Reference
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Remarks:
Supersedes V/71/
References:
Bessell M.S. 1979, Publ. Astron. Soc. Pac., 91, 589.
Breger M. 1985, Publ. Astron. Soc. Pac., 97, 85.
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.
Schmidt-Kaler 1982, in: Landolt-Boernstein, Vol. 2b, p.1.
Strassmeier K.G., Hall D.S., Zeilik M., Nelson E., Eker Z., Fekel F.C.,
1988, Astron. Astrophys. Suppl. Ser., 72, 192.
Strassmeier K.G., Hall D.S., Fekel F.C., and Scheck M., 1992 Astron.
Astrophys. Suppl. Ser., 100, 173.
Strassmeier K.G., Hall D.S., Zeilik M., Nelson E., Eker Z. 1988, Astron.
Astrophys. Suppl. Ser., 72, 291.
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(End) Nancy Grace Roman [SSDOO/ADC] (modified J.A. Watko 15-AUG-1996)