GCVSNSVARS - General Catalog of Variable Stars: Suspected Variable Stars (June 2022 Version)
The data contained in the present catalog include positions, magnitudes, variability types, references to the literature, and spectra.
Revised Version of the New Catalogue of Suspected Variable Stars, NSV Release 2, Kazarovets, E. V., Samus, N.N. and Durlevich, O. V. <Astronomy Reports (2022)> =2022ARep...66..555K General catalog of variable stars: Version GCVS 5.1, Samus N.N., Kazarovets E.V., Durlevich O.V., Kireeva N.N., Pastukhova E.N. <Astron. Zh. 94, 87 (2017)> =2017ARep...61...80S =2017AZh....94...87S New Catalogue of Suspected Variable Stars, Kukarkin B.V., Kholopov P.N., Artiukhina N.M., Fedorovich V.P., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kireeva N.N., Kukarkina N.P., Kurochkin N.E., Medvedeva G.I., Perova N.B., Ponomareva G.A., Samus N.N., Shugarov S.Yu. <Moscow: Nauka Publishing House (1982)> New Catalogue of Suspected Variable Stars. Supplement - Version 1.0 Kazarovets E.V., Durlevich O.V., Samus N.N. <Institute of Astronomy of Russian Academy of Sciences and Sternberg Astronomical Institute (1998)> =1998IBVS.4655....1K
The GCVS Suspected Variable Star prefix NSV (for New Suspected Variable) together with a running number (from 1 to 14812 for stars in the original 1982 NSV Catalog, and from 15001 to 26206 for stars in the 1998 Supplement to the NSV). Leading zeroes have been removed from the running number.
The NSV Catalog running number (from 1 to 14812 for stars in the original 1982 NSV Catalog, and from 15001 to 26206 for stars in the Supplement to the NSV). Leading zeroes have been removed from the running number, notice.
This is a flag that is set to 'Y' if there are remarks on the star in the file http://www.sai.msu.su/gcvs/gcvs/nsv2/rem.txt.
The remarks contain information covering situations such as, e.g.:
1. The discoverer of the light variability is not the author of the paper cited in the variability reference, or is one of several authors of the paper cited. In these cases, discoverers' names are given in original transcriptions of the remarks. 2. The most important additional information about a star, although the NSV Supplement compilers did not intend to present complete bibliographies for any cataloged stars. 3. Remarks for visual binaries giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semi-major axis of a relative orbit and period of orbital motion). Then, data for other components are given where applicable. (Combined magnitudes are generally reported in the main database table).Designations of components of double/multiple stars: A,B,C ...; a,b,c ...; 1,2,3 ...; the symbols p = preceding, f = following, N = northern, S = southern, E = eastern, W = western may also appear. If specific component no indicated, then coordinates in the Table refer to the primary component.
The Right Ascension of the star in the specified equinox. This was given to a precision of 0.01 seconds of time in J2000 equatorial coordinates in the originating table.
The Declination of the star in the specified equinox. This was given to a precision of 0.1 arcsecond in J2000 equatorial coordinates in the originating table.
The Galactic Longitude of the star.
The Galactic Latitude of the star.
This is a code flag describing the positional accuracy, as follows:
'A' means right ascensions accurate to one second of time and declinations accurate to one-tenth of an arcminute 'B' means declinations accurate to 1 arcminute
The star's proper motion in Right Ascension, in arcsec/yr.
The star's proper motion in Declination, in arcsec/yr.
The epoch of the tabulated coordinates. No epoch is provided when using coordinates taken from the literature if the epoch was not specified in the publication and could not be established.
This field specifies the reference source of the astrometric data for the star.
The type of variability according to the GCVS (4th Edition) variability classification scheme, with the addition of six new types (ZZO, AM, R, BE, LBV, BLBOO) that were introduced in the Name-Lists 67-72 and in the GCVS vol. V. Descriptions of the 6 new types only are given below, while the entire classification scheme is described in the file http://cdsarc.u-strasbg.fr/ftp/cats/B/gcvs/vartype.txt. The new types are:
ZZO ZZ Cet type variables of the DO spectral type showing HeII and and CIV absorption lines in their spectra. AM AM Her type variables; close binary systems consisting of a dK-dM type dwarf and of a compact object with strong magnetic field, characterized by variable linear and circular polarization of light. The total range of light variations may reach 4-5 mag V. R Close binary systems characterized by the presence of strong reflection (re-radiation) of the light of the hot star illuminating the surface of the cooler companion. Light curves are sinusoidal with the period equal to Porb, maximum brightness coinciding with the passage of the hot star in front of the companion. The eclipse may be absent. The range of light variation is about 0.5-1.0 mag V (KV Vel). BE It becomes more and more clear that, although the majority of Be stars are photometrically variable, not all of them could be properly called GCAS variables. Quite a number of them show small-scale variations not necessarily related to shell events; in some cases the variations are quasi-periodic. By now we are not able to present an elaborated system of classification for Be variables, but we adopt a decision that in the cases when a Be variable cannot be readily described as a GCAS star we give simply BE for the type of variability. BLBOO The so-called "anomalous Cepheids", i.e. stars with periods characteristic of comparatively long-period RRAB variables, but considerably brighter by luminosity (BL Boo = NGC 5466 V19). EP Stars showing eclipses by their planets. Prototype: V0376 Peg. SRS Semiregular pulsating red giants with short period (several days to a month), probably high-overtone pulsators. Prototype: AU Ari. LPB The comparatively long-period pulsating B stars (periods exceeding one day).
This is a flag that is set to the value of '-' if a star's variability seems doubtful or erroneous according to the compilers of the NSV Catalog.
This is a limit flag for the maximum magnitude: '<' indicates that the max_mag value given is a numerical upper limit, i.e., the actual maximum magnitude may be brighter than this value, while '>' means that the max_mag value given is a numerical lower limit, i.e., the actual maximum magnitude may be fainter than this value.
The apparent magnitude at maximum brightness. Magnitudes are reported to hundredths if the observations are photoelectric or CCD, to tenths or whole magnitudes if they are not. If only an amplitude has been measured photoelectrically, then the maximum magnitude is generally given to tenths only and the minimum is reported to hundredths.
This flag is set to ':' if the maximum magnitude is considered uncertain.
This field may contain flag(s) indicating limit and/or amplitude for the min_mag value.
If the field contains '(', that indicates that the quoted min_mag value is an amplitude relative to the value of the max_mag parameter, rather than the actual minimum magnitude, and the limit, if present, applies to this amplitude.
If the value is '>', then the min_mag value given is a bright limit, i.e., the actual minimum magnitude may be fainter than this value, while if the value is '<', then the min_mag value given is a faint limit, i.e., the actual minimum magnitude may be brighter than this value.
The minimum apparent magnitude, or the amplitude of variability. If the value of limit_min_mag contains '(', this indicates that the min_mag value given is an amplitude rather than an observed minimum magnitude. Magnitudes are reported to hundredths if the observations are photoelectric or CCD, to tenths or whole magnitudes if they are not. If only an amplitude has been measured photoelectrically, then the maximum magnitude is generally given to tenths only and the minimum is reported to hundredths. If the value of min_mag_flag is 'st', then the quoted value of min_mag is an amplitude in steps rather than magnitudes, and the original references should be consulted for further information.
This flag is set to ':' if the min_mag value is considered uncertain, and is set to 'st' if the quoted value of min_mag is an amplitude in steps rather than magnitudes, and the original references should be consulted for further information. In 3 cases (NSV 25926, NSV 25927 and NSV 25981) the value is set to 'A' (the HEASARC changed the original '*' since an asterisk is used as a wild card character in its system): the significance of this flag value is not specified in the original CDS documentation.
A code for the photometric system in which the max_mag and min_mag value are reported (if the value of min_mag_system is blank), or for the photometric system in which the max_mag value only is reported (if the value of min_mag_system is non-blank). The main codes are V (visual, photovisual, or Johnson V), B (Johnson B) and p (photographic magnitudes). The designations u, v, b, y refer to the Stroemgren system. The symbols Ic and Rc mean magnitudes in the Cousins I, R system, g designates magnitudes in the system of Thuan and Gunn, T stands for broad-band Tycho magnitudes formed from B and V measurements, while r are red magnitudes not tied to a particular system. A value of 'w' for this parameter means that the quoted magnitude is for a white-light measurement. Several stars from the 68th Name List have values of '1.' for this parameter to designate the 1.04 micron band of the system introduced by G.W. Lockwood.
This is a reference code referring to a study of the star, the key to which can be found in the file http://www.sai.msu.su/gcvs/gcvs/nsv2/ref.txt.
This is a reference code referring to a study that contains a chart or photograph of the star field, the key to which can be found in the file file http://www.sai.msu.su/gcvs/gcvs/nsv2/ref.txt.
The identification of the suspected variable in the paper whose code reference is given in the ref_star parameter. DM numbers are given without a prefix, the standard naming convention of "The Henry Draper Catalogue" being used (BD for declination zones +89 to -22, CD for zones -23 to -51, and CP for zones -52 to -89). Some identifications are given by coordinate designations, a 6-digit number consisting of hours, minutes, and seconds (or tenths of a minute) of time and degrees of declination with sign included. A value of 'Y' signifies that a designation is given in the remarks to the published catalog. This parameter is not populated for the stars in the NSV Supplement (entries with values of the nsv parameter of 15001 or greater).
The spectral type and luminosity class of the suspected variable star, if known. Spectral types from the HD Catalog are generally given in parentheses. Also, the following (non-standard) symbols may be used:
AF for A-F type stars BA for B-A type stars e emission spectrum ea e sub alpha ev variable emission in spectrum FG for F-G type stars KM for K-M type stars T characteristics of T Tauri stars
The alternative name of the suspected variable star either as given in the main Catalog of Galactic Variable Stars (the HEASARC GCVS table, created from the CDS table B/gcvs/gcvs_cat.dat), a Name-List number, if it starts with the 2-digit number 67-77 and is followed by the 4-digit number of the star in the corresponding Name List, or as given in the GCVS Catalog of Extragalactic Variable Stars (the HEASARC GCVSEGVARS table, created from the CDS table B/gcvs/evs_cat.dat). In the last case, the name may be followed by an asterisk: this indicates that there are remarks about this star in GCVS Volume V.
The HEASARC Browse object classification, based on the spectral type parameter (spect_type), if there is information in this field, else based on the variability type parameter (variability_type).