V/85A Stellar Mass Catalogue (Belikov 1995)
Stellar Mass Catalogue. Preliminary Version
Belikov A.N.
<Bull. Inf. CDS 47, 9 (1995)>
=1995BICDS..47....9B 1995BICDS..47....9B
ADC_Keywords: Stars, masses
Description:
The catalogue includes binary stars for which dynamical masses of
components has been published in 1969 - 1988. It doesn't contain other
compilation catalogues that was published in this two decades and uses
original data papers only. It collects masses defined by direct,
dynamical methods only (without use of mass-luminosity, mass-radius,
mass-spectrum and similar relations).
The work was supervised by Dr O. Malkov.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 99 360 The catalogue
refs.dat 134 246 References
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Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Principal name of the system
14- 25 A12 --- OtherID Secondary identifier of the system
27- 33 F7.4 solMass M1 Mass of primary component
35- 40 F6.4 solMass e_M1 ? Mean error on M1
42- 48 F7.4 solMass M2 Mass of secondary component
50- 55 F6.4 solMass e_M2 ? Mean error on M2
57- 58 A2 --- Method Method of mass determination (1)
60- 61 A2 --- n_Name Individual note explained in (5)
63- 72 A10 --- AAAref Reference from AAA (2)
74- 78 A5 --- System Type of system (3)
80- 99 A20 --- Sp Spectral types of the two stars (4)
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Note (1): Methods of mass determination:
S = methods for double lined spectroscopic binaries:
The inclination of the system are derived from :
S0 resolved light curve;
S1 visual orbit;
S2 speckle-interferometry;
S3 polarimetry.
V = methods for visual binaries:
Photographic magnitude difference
V0 is known;
V1 is assumed to be zero;
V2 is calculated from visual magnitudes and spectra;
V3 is calculated from visual magnitudes and difference
visual and photographic photocentric semimajor axes;
V4 is known from speckle - interferometry;
V5 is calculated from J,H,K magnitude differences.
R = methods for resolved spectroscopic binaries:
R0 orbital parallax used.
R1 trigonometric parallax used.
Note (2): number of the paper in Astronomy and Astrophysics Abstracts,
made of Volume . Section . Paper number
The references are explained in file "refs.dat"
Note (3): Types of system abbreviations, the colon (:) indicates
an uncertainty:
Al = Algol-type star
c = contact system
ce = evolved contact system
d = detached system
dn = dwarf nova
fl = flare star
nc = near contact system
p.RS = precursor of the RS CVn-type system
R = R CMa-type star
RS = RS CVn-type star
S = W Ser-type star
sd = semidetached system
W = W UMa-type star
WA = W UMa-type star,type A
WB = W UMa-type star,type B
WR = binary system with Wolf-Raet star
WW = W UMa-type star,type W
Note (4): Spectra abbreviations:
e. = early
m. = middle
l. = late
? = unknown spectrum
(Sp) = questionable spectrum
+ = division of primary and secondary component spectra
; = division of composed spectrum of system and component's spectra
- = uncertainty in spectral class
/ = uncertainty in luminosity class
Note (5): Individual Notes:
a: authors calculated all needed parameters, but didn't
calculate final masses.
b: the trigonometric parallax used too.
c: authors used dynamic parallax to calculate sum of mass, but
the system has trigonometric parallax the same. Authors calculated
all needed parameters, but didn't calculate final masses.
d: authors used dynamic parallax to calculate sum of mass but
the system has trigonometric parallax the same.
1: the second of this pair is the intrinsic variable star .
2: to determine mass ratio authors used self-determined
radial velocities.
3: with mass ratio from Wilson & Devinney , 1973ApJ...182..539W 1973ApJ...182..539W
4: the final stage of the B-type W UMa configuration
5: used orbit from Lippincott S.L., 1981PASP...93..376L 1981PASP...93..376L
6: used orbit from Russell & Gatewood, 1984PASP...96..429R 1984PASP...96..429R
7: a system between Roche-lobe filling stage of case C
(post-helium flash) mass transfer
8: 1) the primary is near filling its Roche lobe;
2) intrinsic activity is detected;
3) a member of NGC 752.
9: the secondary is intrinsic variable of delta Scuti type.
10: these system is a member of open cluster NGC 6231 of the Sco OB1
association.
11: sp.elements from Struve & Gratton, 1948ApJ...108..497S 1948ApJ...108..497S
12: sp.elements from Struve & Zetergi, 1959ApJ...130..789S 1959ApJ...130..789S
13: sp.elements from King & Hilditch , 1984MNRAS.209..645K 1984MNRAS.209..645K
14: this system is passing through a transition state from a
semidetached configuration, reached via case A mass transfer
episode to become an evolved and deep-contact A-type W UMa system.
15: UV Cet is B - component of L726-8(A+B).
16: using sp.elements by Harper W.E., Pearce J.A., Petrie R.M.,
Mckellar A., 1935JRASC..29..411H 1935JRASC..29..411H
17: using sp.elements by Popper D.M., ApJ 166, 366, 1971
(1971ApJ...166..361P 1971ApJ...166..361P)
18: primary component is the beta-Cepheid star.
19: Algol-type eclipsing binary with an evolved and less-massive
secondary component (must be filling it's Roche lobe)
20: this system has more than two stars (from anomalous large
total mass) maybe.
21: the secondary has evolved G9 spectrum.
22: the system has third component of A7V spectrum.
23: the system has third component.
24: the system has third component of K5 spectrum.
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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- 10 A10 --- AAAref Reference as in "catalog"
12- 30 A19 --- BibCode 19-digit bibcode
32-134 A103 --- Text of reference
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Author's address:
Belikov Andrew N. ()
Historical Notes:
The decimal points have been added where necessary.
* 06-Nov-2004 (version 'A'): Some corrections provided by the author
(Andrew Belikov) in 2002 were included; the bibcodes were added
in the references, and a few have been corrected.
(End) Francois Ochsenbein [CDS] 19-Jul-1995