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
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