V/120ivo://CDS.VizieR/V/120CDSBondarenko I.I.Perevozkina E.L.2018-01-02T13:42:44Z2005-01-31T22:04:48ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.freclipsing-binary-starsFor the first time the early type contact systems were identified as an individual class in M.A. Svechnikov's Catalogue [1] in 1969, which contains 8 systems of this type. The Catalogue of Coch R.H., Plavec M. and Wood F.B. [2] contains 37 systems of the early spectral type. According to Svechnikov's classification [3] a primary component (more massive and hotter) of a CE-system (contact system of early spectral class) has a spectral class earlier than F0-F2 and an orbital period of more than 0.5 day. Usually the spectral class of a primary is earlier than the spectral class of a secondary. Both components fill their Roche-lobes on 90-100%. The following Catalogue of Svechnikov M.A. and Bessonova L.A. [4] contains 38 CE-systems. In 1986 Bondarenko I.I. [5] published the Catalogue of the CE-stars, which contained 83 systems. Physical characteristics of the CE-stars presented in the list of catalogues abovementioned, were obtained by different authors by using different methods of calculation. We propose the Catalogue of the CE-systems with homogeneous absolute physical characteristics, that allows to define accurately general features of this class of binary stars. The comparing of physical characteristics of the CE-systems with other classes` characteristics of binary stars can show the possible evolutionary stages of the CE-systems. The foundation of absolute elements of the CE-systems are the photometric observations (on the whole, the latest multicolour photoelectric, in a few cases photographic and visual observations). The accuracy of modern photometric observations is high, and generally they are processed with the help of reliable computer methods both classical and synthetical methods). But reliable spectral observations (the ray speed curves) are very scarce, especially for both components). We have preferred the spectral class of a primary (usually it is more bright), supposing, that it's spectral class was defined accurately, and photometric and geometrical elements from light curves. All stars from our Catalogue were classified preliminarily as CE-stars by Svechnikov M.A., Istomin L.F. and Grehova O.A. [6]. We have supposed both components fill their Roche-lobes and by using the diagram (q-r[critical]) of Plavec-Kratochvile [7] mass ratio was obtained. The absolute elements were obtained by the approximated method of Svechnikov, which was modernized for CE-stars. Our Catalogue consist of three parts: photometric, geometrical and absolute elements of CE-systems. All stars were divided approximately into two groups: massive (m1>3 solar masses for primary) and less-massive stars (m1<3 solar masses for primary). A Catalogue has a Supplement.1996IzOde...9...20Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/V/120CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/42 : Close double stars (Svechnikov+, 1984)V/115 : Semidetached and semi-detouched eclipsing binaries (Surkova+, 2004)V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999)V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=V/120https://vizier.iucaa.in/viz-bin/VizieR-2?-source=V/120http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=V/120https://vizier.cds.unistra.fr/viz-bin/votable?-source=V/120https://vizier.iucaa.in/viz-bin/votable?-source=V/120http://vizieridia.saao.ac.za/viz-bin/votable?-source=V/120GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table V/120/table1 (Photometric elements)https://vizier.cds.unistra.fr/viz-bin/conesearch/V/120/table1?https://vizier.iucaa.in/viz-bin/conesearch/V/120/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/V/120/table1?GETtext/xml+votable180.050000true15.42916738.0966670.0055555555555555566/359 1299 1302 1369 1427 1429 2154 2632 2806 2908 3308 3320 4425 6211 6375 6550 7861 11984 12522 13015 13181 13229 13247 13269 13306 13759 13859 14027 14155 14263 14294 14303 14423 14528 14619 14692 15470 15477 15616 15625 15713 15723 16145 16274 16673 17064 18499 18634 20899 21532 21949 21962 23637 23998 24982 26020 26382 27372 27603 27852 28809 29374 29505 29838 30627 30643 32390 32838 33323 35422 36307 36510 37212 37696 37761 37892 37897 37910 38032 39075 39076 39201 39245 39274 39916 39933 40030 40138 41697 41726 41864 42060 42428 43048 43129 43402 44872 47825 48015 48505https://cdsarc.cds.unistra.fr/viz-bin/moc/V/120?format=asciiOpticaldefaultV/120/table1Photometric elementsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.intSeqNumber of (CE)-system (G1)intprimaryNameDesignation in General Catalogue of Variable Stars (4th Edition)charCoef1? limb-darkening coefficientfloatnullableCoef2? limb-darkening coefficientfloatnullablen_Coef1[*] *: Approximated values of darkness to an edge according to the spectral typecharL1? Fractonal light (relative to L1+L2)floatnullableJ1/J2? Surface brightness ratio of componentsfloatnullablePhotPhotometry system of light curve or effective wavelength which was used for photoelectric observation (2)charSimbadSimbad column added by the CDSchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainV/120/table2Geometrical and absolute elementsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.intSeqNumber of (CE)-system (G1)intNameDesignation in General Catalogue of Variable StarscharSp1The spectral class of primary (2)charSp2The spectral class of secondary (2)charM1Mass of primary is determined by the mass-luminosity relation for stars of the main sequencesolMassfloatM2Mass of secondary is calculated using a photometric mass ratio q=M1/M2solMassfloatqPhotometric mass ratio derived from the light curve solution (3)floatR1Radius of primarysolRadfloatR2Radius of secondarysolRadfloataValue of the orbital semimajor axissolRadfloatM1bolAbsolute bolometric magnitude of primarymagfloatWphWeight (10 ball system) (4)intM2bolAbsolute bolometric magnitude of secondaryfloatrad1fFractional radius of the primary from photometric solutionsfloatrad2fFractional radius of the secondary from photometric solutionsfloatiInclination of the orbital axis to the sightdegfloatmu1Degree of filling of Roche-Lobe of primary%intmu2Degree of filling of Roche-Lobe of secondary%intDist? Distance to the systempcintnullableWabsWeight (10 ball system) (5)intPerSideral orbital periodddoublen_Per[*] * - variability of periodcharTypeType of eclipse (6)charMethodMethod of recognition of photometric solution (7)charV/120/notesIndividual notesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.intSeqNumber of (CE)-system (G1)intNoteText of the notechar