Access to Astronomical Catalogues

Search catalogue
obsoleted
in preparation
catalog without ftp or VizieR link
V/85A               Stellar Mass Catalogue (Belikov 1995)

Stellar Mass Catalogue. Preliminary Version Belikov A.N. <Bull. Inf. CDS 47, 9 (1995)> =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:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 99 360 The catalogue refs.dat 134 246 References
Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
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)
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 4: the final stage of the B-type W UMa configuration 5: used orbit from Lippincott S.L., 1981PASP...93..376L 6: used orbit from Russell & Gatewood, 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 12: sp.elements from Struve & Zetergi, 1959ApJ...130..789S 13: sp.elements from King & Hilditch , 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 17: using sp.elements by Popper D.M., ApJ 166, 366, 1971 (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.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 10 A10 --- AAAref Reference as in "catalog" 12- 30 A19 --- BibCode 19-digit bibcode 32-134 A103 --- Text of reference
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
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

catalogue service

© UDS/CNRS

Contact