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Extrait du General Catalog of Variable Stars (Kholopov+ 1998) Organisation du catalogue : Les Θtoiles sont rΘparties dans 50 zones de 30x30 degrΘs selon le mΩme principe que les grandes rΘgions du Guide Star Catalog . ( Voir Jenkner et al. The Astronomical Journal vol 99, num 6 June 1990 p.2087) dΘclinaison nombre numΘro de la du centre de zones premiΦre zone ------------- ------------ -------------- 15 12 1 45 9 13 75 4 22 -15 12 26 -45 9 38 -75 4 47 Chaque zone est matΘrialisΘe par un fichier . Description des enregistrements des fichiers : Toutes les donnΘes proviennent des fichiers gcvs.dat, evs_cat.dat, nsv.dat. GCVrec = record ar, de, num :longint ; period : single; max, min : smallint; lmax, lmin, mcode : char; gcvs, vartype : array[1..10] of char; end; - ar : ascention droite 2000 en degrΘs * 100'000 - de : declinaison 2000 * 100'000 - num : numΘro de constelation et d'Θtoile - period: periode de variation en jours - max : magnitude maximum * 100 - min : magnitude minimum * 100 - lmax : limite de magnitude maximum - lmin : limite de magnitude minimum - mcode : systΦme photomΘtrique - gcvs : identification de l'Θtoile variable - vartype: type de variable + annΘe de nova Type Intervalle Format ------------ -------------------------- ------------------- Shortint -128 .. 127 SignΘ, 8 bits SmallInt -32768 .. 32767 SignΘ, 16 bits Longint -2147483648 .. 2147483647 SignΘ, 32 bits Byte 0 .. 255 Non signΘ, 8 bits Word 0 .. 65535 Non signΘ, 16 bits Chiffres Taille en Type PortΘe significatifs octets -------- ----------------------------- ------------- ------ Real 2.9 * 10-39 .. 1.7 * 1038 11-12 6 Single 1.5 * 10-45 .. 3.4 * 1038 7-8 4 Double 5.0 * 10-324 .. 1.7 * 10308 15-16 8 Extended 3.4 * 10-4932 .. 1.1 * 104932 19-20 10 ======================================================================== GCVS Variability Types ======================================================================== An improved system of variability classification is used in the fourth edition of the GCVS, based on recent developments in classification principles and taking into account the suggestions of a number of specialists. Variability types are grouped according to the major astrophysical reasons for variability, viz., 1. eruptive (FU, GCAS, I, IA, IB, IN, INA, INB, INT, IN(YY), IS, ISA, ISB, RCB, RS, SDOR, UV, UVN, WR), 2. pulsating (ACYG, BCEP, BCEPS, CEP, CEP(B), CW, CWA, CWB, DCEP, DCEPS, DSCT, DSCTC, L, LB, LC, M, PVTEL, RR, RR(B), RRAB, RRC, RV, RVA, RVB, SR, SRA, SRB, SRC, SRD, SXPHE, ZZ, ZZA, ZZB), 3. rotating (ACV, ACVO, BY, ELL, FKCOM, PSR, SXARI), 4. cataclysmic (explosive and novalike) variables (N, NA, NB, NC, NL, NR, SN, SNI, SNII, UG, UGSS, UGSU, UGZ, ZAND), 5. eclipsing binary systems (E, EA, EB, EW, GS, PN, RS, WD, WR, AR, D, DM, DS, DW, K, KE, KW, SD), 6. intense variable X-ray sources (X, XB, XF, XI, XJ, XND, XNG, XP, XPR, XPRM), 7. other symbols (BLLAC, CST, GAL, L:, QSO, S:, *, +). All of these classes include objects of a dissimilar nature that belong to different types of light variability. On the other hand, an object may be variable because of almost all of the possible reasons or because of any combination of them. If a variable belongs to several types of variability, the types are joined in the data field by a "+" sign, e.g., E+UG, UV+BY. Despite considerable success in understanding stellar variability pro- cesses, the classification adopted in the Catalogue is far from perfect. This is especially the case for explosive, symbiotic and novalike variables; X-ray sources; and peculiar objects. The new variability types (ZZO, AM, R, BE, LBV, BLBOO) have been added in the Name-Lists 67- 72 and in the GCVS vol.V. ZZO ZZ Cet type variables of the DO spectral type showing HeII and and CIV absorbtion 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 0.5-1.0mag 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. LBV For comparatively long-period pulsating B stars (periods exceeding one day), we introduce a provisional type LBV. 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). 1. Eruptive Variable Stars Eruptive variables are stars varying in brightness because of violent processes and flares occurring in their chromospheres and coronae. The light changes are usually accompanied by shell events or mass outflow in the form of stellar winds of variable intensity and/or by interaction with the surrounding interstellar medium. This class includes the following types: FU Orion variables of the FU Orionis type. Characterized by gradual increases in brightness by about 6 mag in several months, followed by either almost complete constancy at maximum that is sustained for long periods of time or slow decline by 1-2 mag. Spectral types at maximum are in the range Ae(alpha) - Gpe(alpha). After an outburst, a gradual development of an emission spectrum is observed and the spectral type becomes later. These variables probably mark one of the evolutionary stages of T Tauri-type Orion variables (INT), as evidenced by an outburst of one member, V1057 Cyg, but its decline (2.5 mag in 11 years) commenced immediately after maximum brightness was attained. All presently known FU Ori variables are coupled with reflecting cometary nebulae. GCAS Eruptive irregular variables of the Gamma Cas type. These are rapidly rotating B III-IVe stars with mass outflow from their equatorial zones. The formation of equatorial rings or disks is often accompanied by temporary fading. Light amplitudes may reach 1.5 mag in V. I Poorly studied irregular variables with unknown features of light variations and spectral types. This is a very inhomogeneous group of objects. IA Poorly studied irregular variables of early (O-A) spectral type. IB Poorly studied irregular variables of intermediate (F-G) to late (K-M) spectral type. IN Orion variables. Irregular, eruptive variables connected with bright or dark diffuse nebulae or observed in the regions of these nebulae. Some of them may show cyclic light variations caused by axial rotation. In the Spectrum-Luminosity diagram, they are found in the area of the main sequence and subgiants. They are probably young objects that, during the course of further evolution, will become light-constant stars on the zero-age main sequence (ZAMS). The range of brightness variations may reach several magnitudes. In the case of rapid light variations having been observed (up to 1 mag in 1-10 days), the letter "S" is added to the symbol for the type (INS). This type may be divided into the following subtypes: INA Orion variables of early spectral types (B-A or Ae). They are often characterized by occasional abrupt Algol-like fadings (T Ori); INB Orion variables of intermediate and late spectral types, F-M or Fe-Me (BH Cep, AH Ori). F-type stars may show Algol-like fadings similar to those of many INA stars; K-M stars may produce flares along with irregular light variations; INT Orion variables of the T Tauri type. Stars are assigned to this type on the basis of the following (purely spectroscopic) criteria: spectral types are in the range Fe-Me. The spectra of most typical stars resemble the spectrum of the solar chromosphere. The feature specific to the type is the presence of the flourescent emission lines Fe II 4046, 4132 A (anomalously intense in the spectra of these stars), emission lines [Si II] and [O I], as well as the absorption line Li I 6707 A. These variables are usually observed only in diffuse nebulae. If it is not apparent that the star is associated with a nebula, the letter "N" in the symbol for the type may be omitted, e.g., IT (RW AUR); IN(YY) Some Orion variables (YY Ori) show the presence of absorption components on the redward sides of emission lines, indicating the infall of matter toward the stars' surfaces. In such cases, the symbol for the type may be accompanied by the symbol "YY". IS Rapid irregular variables having no apparent connection with diffuse nebulae and showing light changes of about 0.5 - 1.0 mag within several hours or days. There is no strict boundary between rapid irregular and Orion variables. If a rapid irregular star is observed in the region of a diffuse nebula, it is considered an Orion variable and designated by the symbol INS. To attribute a variable to the IS type, it is necessary to take much care to be certain that its light changes are really not periodic. Quite a number of the stars assigned to this type in the third edition of the GCVS turned out to be eclipsing binary systems, RR Lyrae variables, and even extragalactic BL Lac objects. ISA Rapid irregular variables of the early spectral types, B-A or Ae; ISB Rapid irregular variables of the intermediate and late spectral types, F-M and Fe-Me. RCB Variables of the R Coronae Borealis type. These are hydrogen-poor, carbon- and helium-rich, high-luminosity stars belonging to the spectral types Bpe-R, which are simultaneously eruptive and pulsating variables. They show slow nonperiodic fadings by 1-9 mag in V lasting from a month or more to several hundred days. These changes are superposed on cyclic pulsations with amplitudes up to several tenths of a magnitude and periods in the range 30-100 days. RS Eruptive variables of the RS Canum Venaticorum type. This type is ascribed to close binary systems with spectra showing Ca II H and K in emission, their components having enhanced chromospheric activity that causes quasi-periodic light variability. The period of variation is close to the orbital one, and the variability amplitude is usually as great as 0.2 mag in V (UX Ari). They are X-ray sources and rotating variables. RS CVn itself is also an eclipsing system (see below). SDOR Variables of the S Doradus type. These are eruptive, high-luminosity Bpec-Fpec stars showing irregular (sometimes cyclic) light changes with amplitudes in the range 1-7 mag in V. They belong to the brightest blue stars of their parent galaxies. As a rule, these stars are connected with diffuse nebulae and surrounded by expanding envelopes (P Cyg, Eta Car). UV Eruptive variables of the UV Ceti type, these are K Ve-M Ve stars sometimes displaying flare activity with amplitudes from several tenths of a magnitude up to 6 mag in V. The amplitude is considerably greater in the ultraviolet spectral region. Maximum light is attained in several seconds or dozens of seconds after the beginning of a flare; the star returns to its normal brightness in several minutes or dozens of minutes. UVN Flaring Orion variables of spectral types Ke-Me. These are phenomenologically almost identical to UV Cet variables observed in the solar neighborhood. In addition to being related to nebulae, they are normally characterized by being of earlier spectral type and greater luminosity, with slower development of flares (V389 Ori). They are possibly a specific subgroup of INB variables with irregular variations superimposed by flares. WR Eruptive Wolf-Rayet variables. Stars with broad emission features of He I and He II as well as C II-C IV, O II-O IV, and N III-N V. They display irregular light changes with amplitudes up to 0.1 mag in V, which are probably caused by physical processes, in particular, by nonstable mass outflow from their atmospheres. 2. Pulsating Variable Stars Pulsating variables are stars showing periodic expansion and contraction of their surface layers. The pulsations may be radial or nonradial. A radially pulsating star remains spherical in shape, while in the case of nonradial pulsations the star's shape periodically deviates from a sphere, and even neighboring zones of its surface may have opposite pulsation phases. Depending on the period value, on the mass and evolutionary status of the star, and on the scale of pulsational phenomena, the following types of pulsating variables may be distinguished: ACYG Variables of the Alpha Cygni type, which are nonradially pulsating supergiants of Bep-AepIa spectral types. The light changes with amplitudes of the order of 0.1 mag often seem irregular, being caused by the superposition of many oscillations with close periods. Cycles from several days to several weeks are observed. BCEP Variables of the Beta Cephei type (Beta Cep, Beta CMa), which are pulsating O8-B6 I-V stars with periods of light and radial-velocity variations in the range of 0.1 - 0.6 days and light amplitudes from 0.01 to 0.3 mag in V. The light curves are similar in shape to average radial-velocity curves but lag in phase by a quarter of the period, so that maximum brightness corresponds to maximum contraction, i.e., to minimum stellar radius. The majority of these stars probably show radial pulsations, but some (V649 Per) display nonradial pulsations; multiperiodicity is characteristic of many of these stars. BCEPS A short-period group of Beta Cep variables. The spectral types are B2-B3 IV-V; periods and light amplitudes are in the ranges 0.02 - 0.04 days and 0.015 - 0.025 days, respectively, i.e., an order of magnitude smaller than the normally observed ones. CEP Cepheids. Radially pulsating, high luminosity (classes Ib-II) vari- ables with periods in the range of 1-135 days and amplitudes from several hundredths to 2 mag in V (in the B band, the amplitudes are greater). Spectral type at maximum light is F; at minimum, the types are G-K. The longer the period of light variation, the later is the spectral type. The maximum of the surface-layer expansion velocity almost coinciding with maximum light. CEP(B) Cepheids (TU Cas, V 367 Sct) displaying the presence of two or more simultaneously operating pulsation modes (usually the fundamental tone with the period P0 and the first overtone P1). The periods P0 are in the range from 2 to 7 days, with the ratio P1/P0 approx. 0.71. CW Variables of the W Virginis type. These are pulsating variables of the galactic spherical component (old disk) population with periods of approximately 0.8 to 35 days and amplitudes from 0.3 to 1.2 mag in V. They obey a period-luminosity relation different from that for Delta Cep variables (see DCEP). For an equal period value, the W Vir variables are fainter than the Delta Cep stars by 0.7 - 2 mag. The light curves of W Vir variables for some period intervals differ from those of Delta Cep variables for corresponding periods either by amplitudes or by the presence of humps on their descending branches, sometimes turning into broad flat maxima. W Vir variables are present in globular clusters and at high galactic latitudes. They may be separated into the following subtypes: CWA W Vir variables with periods longer than 8 days (W Vir); CWB W Vir variables with periods shorter than 8 days (BL Her). DCEP These are the classical cepheids, or Delta Cep-type variables. Com- paratively young objects that have left the main sequence and evolved into the instability strip of the Hertzsprung-Russell (H-R) diagram, they obey the well-known Cepheid period-luminosity relation and belong to the young disk population. DCEP stars are present in open clusters. They display a certain relation between the shapes of their light curves and their periods. DCEPS These are Delta Cep variables having light amplitudes <0.5 mag in V (<0.7 mag in B) and almost symmetrical light curves (M-m approx. 0.4 - 0.5 periods); as a rule, their periods do not exceed 7 days. They are probably first-overtone pulsators and/or are in the first transition across the instability strip after leaving the main sequence (SU Cas). Traditionally, both Delta Cep and W Vir stars are quite often called Cepheids because it is often impossible to discriminate between them on the basis of the light curves for periods in the range 3 - 10 days. However, these are distinct groups of entirely different objects in different evolutionary stages. One of the significant spectral differences between W Vir stars and Cepheids is the presence, during a certain phase interval, of hydrogen-line emission in the former and of Ca II H and K emission in the latter. DSCT Variables of the Delta Scuti type. These are pulsating variables of spectral types A0-F5 III-V displaying light amplitudes from 0.003 to 0.9 mag in V (usually several hundredths of a magnitude) and periods from 0.01 to 0.2 days. The shapes of the light curves, periods, and amplitudes usually vary greatly. Radial as well as nonradial pulsations are observed. The variability of some members of this type appears sporadically and sometimes completely ceases, this being a consequence of strong amplitude modulation with the lower value of the amplitude not exceeding 0.001 mag in some cases. The maximum of the surface layer expansion does not lag behind the maximum light for more than 0.1 periods. DSCT stars are representatives of the galactic disk (flat component) and are phenomenologically close to the SX Phe variables. DSCTC Low amplitude group of Delta Sct variables (light amplitude <0.1 mag in V). The majority of this type's representatives are stars of luminosity class V; objects of this subtype generally are representative of the Delta Sct variables in open clusters. L Slow irregular variables. The light variations of these stars show no evidence of periodicity, or any periodicity present is very poorly defined and appears only occasionally. Like for the type I, stars are often attributed to this type because of being insufficiently studied. Many type L variables are really semiregulars or belong to other types. LB Slow irregular variables of late spectral types (K, M, C, S); as a rule, they are giants (CO Cyg). This type is also ascribed, in the GCVS, to slow red irregular variables in the case of unknown spectral types and luminosities. LC Irregular variable supergiants of late spectral types having amplitudes of about 1 mag in V (TZ Cas). M Mira (Omicron) Ceti-type variables. These are long-period variable giants with characteristic late-type emission spectra (Me, Ce, Se) and light amplitudes from 2.5 to 11 mag in V. Their periodicity is well pronounced, and the periods lie in the range between 80 and 1000 days. Infrared amplitudes are usually less than in the visible and may be <2.5 mag. For example, in the K band they usually do not exceed 0.9 mag. If the amplitudes exceed 1 - 1.5 mag , but it is not certain that the true light amplitude exceeds 2.5 mag, the symbol "M" is followed by a colon, or the star is attributed to the semiregular class with a colon following the symbol for that type (SR). PVTEL Variables of the PV Telescopii type. These are helium supergiant Bp stars with weak hydrogen lines and enhanced lines of He and C. They pulsate with periods of approximately 0.1 to 1 days, or vary in brightness with an amplitude of 0.1 mag in V during a time interval of about a year. RR Variables of the RR Lyrae type, which are radially-pulsating giant A-F stars having amplitudes from 0.2 to 2 mag in V. Cases of variable light-curve shapes as well as variable periods are known. If these changes are periodic, they are called the "Blazhko effect." Traditionally, RR Lyrae stars are sometimes called short-period Cepheids or cluster-type variables. The majority of these stars belong to the spherical component of the Galaxy; they are present, sometimes in large numbers, in some globular clusters, where they are known as pulsating horizontal-branch stars. Like Cepheids, maximum expansion velocities of surface layers for these stars practically coincide with maximum light. RR(B) RR Lyrae variables showing two simultaneously operating pulsation modes, the fundamental tone with the period P0 and the first overtone, P1 (AQ Leo). The ratio P1/P0 is approximately 0.745; RRAB RR Lyrae variables with asymmetric light curves (steep ascending branches), periods from 0.3 to 1.2 days, and amplitudes from 0.5 to 2 mag in V; RRC RR Lyrae variables with nearly symmetric, sometimes sinusoidal, light curves, periods from 0.2 to 0.5 days, and amplitudes not greater than 0.8 mag in V (SX UMa). RV Variables of the RV Tauri type. These are radially pulsating supergiants having spectral types F-G at maximum light and K-M at minimum. The light curves are characterized by the presence of double waves with alternating primary and secondary minima that can vary in depth so that primary minima may become secondary and vice versa. The complete light amplitude may reach 3-4 mag in V. Periods between two adjacent primary minima (usually called formal periods) lie in the range 30-150 days (these are the periods appearing in the Catalogue). Two subtypes, RVA and RVB, are recognized: RVA RV Tauri variables that do not vary in mean magnitude (AC Her); RVB RV Tauri variables that periodically (with periods from 600 to 1500 days and amplitudes up to 2 mag in V) vary in mean magnitude (DF Cyg, RV Tau). SR Semiregular variables, which are giants or supergiants of intermediate and late spectral types showing noticeable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to >2000 days, while the shapes of the light curves are rather different and variable, and the amplitudes may be from several hundredths to several magnitudes (usually 1-2 mag in V). SRA Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small (<2.5 mag in V) light amplitudes (Z Aqr). Amplitudes and light-curve shapes generally vary and periods are in the range of 35-1200 days. Many of these stars differ from Miras only by showing smaller light amplitudes; SRB Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes, and even with light constancy intervals (RR CrB, AF Cyg). Every star of this type may usually be assigned a certain mean period (cycle), which is the value given in the Catalogue. In a number of cases, the simultaneous presence of two or more periods of light variation is observed; SRC Semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days; SRD Semiregular variable giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days (SX Her, SV UMa). SXPHE Phenomenologically, these resemble DSCT (Delta Sct) variables and are pulsating subdwarfs of the spherical component, or old disk galactic population, with spectral types in the range A2-F5. They may show several simultaneous periods of oscillation, generally in the range 0.04-0.08 days, with variable-amplitude light changes that may reach 0.7 mag in V. These stars are present in globular clusters. ZZ ZZ Ceti variables. These are nonradially pulsating white dwarfs that change their brightnesses with periods from 30 s to 25 min and amplitudes from 0.001 to 0.2 mag in V. They usually show several close period values. Flares of 1 mag are sometimes observed; however, these may be explained by the presence of close UV Ceti companions. These variables are divided into the following subtypes: ZZA ZZ Cet-type variables of DA spectral type (ZZ Cet) having only hydrogen absorption lines in their spectra; ZZB ZZ Cet-type variables of DB spectral type having only helium absorption lines in their spectra. 3. Rotating Variable Stars Variable stars with nonuniform surface brightness and/or ellipsoidal shapes, whose variability is caused by axial rotation with respect to the observer. The nonuniformity of surface brightness distributions may be caused by the presence of spots or by some thermal or chemical inhomogeneity of the atmosphere caused by a magnetic field whose axis is not coincident with the rotation axis. These stars are subdivided into the following types: ACV Alpha2 Canum Venaticorum variables. These are main-sequence stars with spectral types B8p-A7p and displaying strong magnetic fields. Spectra show abnormally strong lines of Si, Sr, Cr, and rare earths whose intensities vary with rotation. They exhibit magnetic field and brightness changes (periods of 0.5-160 days or more). The amplitudes of the brightness changes are usually withine 0.01-0.1 mag in V. ACVO Rapidly oscillating Alpha2 CVn variables. These are nonradially pulsating, rotating magnetic variables of Ap spectral type (DO Eri). Pulsation periods are in the range of 6-12 mmag (0.004-0.01 days), while amplitudes of light variation caused by the pulsation are about 0.01 mag in V. The pulsational variations are superposed on those caused by rotation. BY BY Draconis-type variables, which are emission-line dwarfs of dKe-dMe spectral type showing quasiperiodic light changes with periods from a fraction of a day to 120 days and amplitudes from several hundredths to 0.5 mag in V. The light variability is caused by axial rotation of a star with a variable degree of nonuniformity of the surface brightness (spots) and chromospheric activity. Some of these stars also show flares similar to those of UV Cet stars, and in those cases they also belong to the latter type and are simultaneously considered eruptive variables. ELL Rotating ellipsoidal variables (b Per, Alpha Vir). These are close binary systems with ellipsoidal components, which change combined brightnesses with periods equal to those of orbital motion because of changes in emitting areas toward an observer, but showing no eclipses. Light amplitudes do not exceed 0.1 mag in V. FKCOM FK Comae Berenices-type variables. These are rapidly rotating giants with nonuniform surface brightnesses, which have G-K spectral types with broad H and K Ca II emission and sometimes Halpha. They may also be spectroscopic binary systems. Periods of light variation (up to several days) are equal to rotational periods, and amplitudes are several tenths of a magnitude. It is not excluded that these objects are the product of further evolution of EW (W UMa) close binary systems (see below). PSR Optically variable pulsars (CM Tau), which are rapidly rotating neutron stars with strong magnetic fields, radiating in the radio, optical, and X-ray regions. Pulsars emit narrow beams of radiation, and periods of their light changes coincide with rotational periods (from 0.004 to 4 s), while amplitudes of the light pulses reach 0.8 mag. SXARI SX Arietis-type variables. These are main-sequence B0p-B9p stars with variable-intensity He I and Si III lines and magnetic fields. They are sometimes called helium variables. Periods of light and magnetic field changes (about 1 day) coincide with rotational periods, while amplitudes are approximately 0.1 mag in V. These stars are high-temperature analogs of the ACV variables. 4. Cataclysmic (Explosive and Novalike) Variables These are variable stars showing outbursts caused by thermonuclear burst processes in their surface layers (novae) or deep in their interiors (supernovae). We use the term "novalike" for variables that show novalike outbursts caused by rapid energy release in the surrounding space (UG-type stars - see below) and also for objects not displaying outbursts but resembling explosive variables at minimum light by their spectral (or other) characteristics. The majority of explosive and novalike variables are close binary systems, their components having strong mutual influence on the evolution of each star. It is often observed that the hot dwarf component of the system is surrounded by an accretion disk formed by matter lost by the other, cooler, and more extended component. This category is subdivided into the following types: N Novae. Close binary systems with orbital periods from 0.05 to 230 days. One of the components of these systems is a hot dwarf star that suddenly, during a time interval from one to several dozen or several hundred days, increases its brightness by 7-19 mag in V, then returns gradually to its former brightness over several months, years, or decades. Small changes at minimum light may be present. Cool components may be giants, subgiants, or dwarfs of K-M type. The spectra of novae near maximum light resemble A-F absorption spectra of luminous stars at first. Then broad emission lines (bands) of hydrogen, helium, and other elements with absorption components indicating the presence of a rapidly expanding envelope appear in the spectrum. As the light decreases, the composite spectrum begins to show forbidden lines characteristic of the spectra of gas nebulae excited by hot stars. At minimum light, the spectra of novae are generally continuous or resemble the spectra of Wolf-Rayet stars. Only spectra of the most massive systems show traces of cool components. Some novae reveal pulsations of hot components with periods of approximately 100 s and amplitudes of about 0.05 mag in V after an outburst. Some novae eventually turn out to be eclipsing systems. According to the features of their light variations, novae are subdivided into fast (NA), slow (NB), very slow (NC), and recurrent (NR) categories. NA Fast novae displaying rapid light increases and then, having achieved maximum light, fading by 3 mag in 100 or fewer days (GK Per); NB Slow novae that fade after maximum light by 3 mag in >= 150 days (RR Pic). Here the presence of the well-known "dip" in the light curves of novae similar to T Aur and DQ Her is not taken into account: The rate of fading is estimated on the basis of a smooth curve, its parts before and after the "dip" being a direct continuation of one another; NC Novae with a very slow development and remaining at maximum light for more than a decade, then fading very slowly. Before an outburst these objects may show long-period light changes with amplitudes of 1-2 mag in V (RR Tel); cool components of these systems are probably giants or supergiants, sometimes semiregular variables, and even Mira variables. Outburst amplitudes may reach 10 mag. High excitation emission spectra resemble those of planetary nebulae, Wolf-Rayet stars, and symbiotic variables. The possibility that these objects are planetary nebulae in the process of formation is not excluded; NL Novalike variables, which are insufficiently studied objects resembling novae by the characteristics of their light changes or by spectral features. This type includes, in addition to variables showing novalike outbursts, objects with no bursts ever observed; the spectra of novalike variables resemble those of old novae, and small light changes resemble those typical for old novae at minimum light. However, quite often a detailed investigation makes it possible to reclassify some representatives of this highly inhomogeneous group of objects into other types; NR Recurrent novae, which differ from typical novae by the fact that two or more outbursts (instead of a single one) separated by 10-80 years have been observed (T CrB). SN Supernovae (B Cas, CM Tau). Stars that increase, as a result of an outburst, their brightnesses by 20 mag and more, then fade slowly. The spectrum during an outburst is characterized by the presence of very broad emission bands, their widths being several times greater than those of the bright bands observed in the spectra of novae. The expansion velocities of SN envelopes are in the thousands of km/s. The structure of a star after outburst alters completely. An expanding emission nebula results and a (not always observable) pulsar remains at the position of the original star. According to the light curve shape and the spectral features, supernovae are subdivided into types I and II. SNI Type I supernovae. Absorption lines of Ca II, Si, etc., but no hydrogen lines are present in the spectra. The expanding envelope almost lacks hydrogen. During 20-30 days following maximum light, the brightness decreases by approximately 0.1 mag per day, then the rate of fading slows and reaches a constant value of 0.014/day; SNII Type II supernovae. Lines of hydrogen and other elements are apparent in their spectra. The expanding envelope consists mainly of H and He. Light curves show greater diversity than those of type I supernovae. Usually after 40-100 days since maximum light, the rate of fading is 0.1 mag per day. UG U Geminorum-type variables, quite often called dwarf novae. They are close binary systems consisting of a dwarf or subgiant K-M star that fills the volume of its inner Roche lobe and a white dwarf surrounded by an accretion disk. Orbital periods are in the range 0.05-0.5 days. Usually only small, in some cases rapid, light fluctuations are observed, but from time to time the brightness of a system increases rapidly by several magnitudes and, after an interval of from several days to a month or more, returns to the original state. Intervals between two consecutive outbursts for a given star may vary greatly, but every star is characterized by a certain mean value of these intervals, i.e., a mean cycle that corresponds to the mean light amplitude. The longer the cycle, the greater the amplitude. These systems are frequently sources of X-ray emission. The spectrum of a system at minimum is continuous, with broad H and He emission lines. At maximum these lines almost disappear or become shallow absorption lines. Some of these systems are eclipsing, possibly indicating that the primary minimum is caused by the eclipse of a hot spot that originates in the accretion disk from the infall of a gaseous stream from the K-M star. According to the characteristics of the light changes, U Gem variables may be subdivided into three types: SS Cyg, SU UMa, and Z Cam. UGSS SS Cygni-type variables (SS Cyg, U Gem). They increase in brightness by 2-6 mag in V in 1-2 days and in several subsequent days return to their original brightnesses. The values of the cycle are in the range 10 days to several thousand; UGSU SU Ursae Majoris-type variables. These are characterized by the presence of two types of outbursts called "normal" and "supermaxima". Normal, short outbursts are similar to those of UGSS stars, while supermaxima are brighter by 2 mag, are more than five times longer (wider), and occur several times less frequently. During supermaxima the light curves show superposed periodic oscillations (superhumps), their periods being close to the orbital ones and amplitudes being about 0.2-0.3 mag in V. Orbital periods are shorter than 0.1 days; companions are of dM spectral type; UGZ Z Camelopardalis-type stars. These also show cyclic outbursts, differing from UGSS variables by the fact that sometimes after an outburst they do not return to the original brightness, but during several cycles retain a magnitude between maximum and minimum. The values of cycles are from 10 to 40 days, while light amplitudes are from 2 to 5 mag in V. ZAND Symbiotic variables of the Z Andromedae type. They are close binaries consisting of a hot star, a star of late type, and an extended envelope excited by the hot star's radiation. The combined brightness displays irregular variations with amplitudes up to 4 mag in V. A very inhomogeneous group of objects. 5. Close Binary Eclipsing Systems We adopt a triple system of classifying eclipsing binary systems: according to the shape of the combined light curve, as well as to physical and evolutionary characteristics of their components. The classification based on light curves is simple, traditional, and suits the observers; the second and third classification methods take into account positions of the binary-system components in the (MV ,B-V) diagram and the degree of inner Roche lobe filling. Estimates are made by applying the simple criteria proposed by Svechnikov and Istomin (1979). The symbols for the types of eclipsing binary systems that we use are given below. a) Classification based on the shape of the light curve E Eclipsing binary systems. These are binary systems with orbital planes so close to the observer's line of sight (the inclination i of the orbital plane to the plane orthogonal to the line of sight is close to 90 deg) that the components periodically eclipse each other. Consequently, the observer finds changes of the apparent combined brightness of the system with the period coincident with that of the components' orbital motion. EA Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes. EB Beta Lyrae-type eclipsing systems. These are eclipsing systems having ellipsoidal components and light curves for which it is impossible to specify the exact times of onset and end of eclipses because of a continuous change of a system's apparent combined brightness between eclipses; secondary minimum is observed in all cases, its depth usually being considerably smaller than that of the primary minimum; periods are mainly longer than 1 day. The components generally belong to early spectral types (B-A). Light amplitudes are usually <2 mag in V. EW W Ursae Majoris-type eclipsing variables. These are eclipsers with periods shorter than 1 days, consisting of ellipsoidal components almost in contact and having light curves for which it is impossible to specify the exact times of onset and end of eclipses. The depths of the primary and secondary minima are almost equal or differ insignificantly. Light amplitudes are usually <0.8 mag in V. The components generally belong to spectral types F-G and later. b) Classification according to the components' physical characteristics GS Systems with one or both giant and supergiant components; one of the components may be a main sequence star. PN Systems having, among their components, nuclei of planetary nebulae (UU Sge). RS RS Canum Venaticorum-type systems. A significant property of these systems is the presence in their spectra of strong Ca II H and K emission lines of variable intensity, indicating increased chromospheric activity of the solar type. These systems are also characterized by the presence of radio and X-ray emission. Some have light curves that exhibit quasi sine waves outside eclipses, with amplitudes and positions changing slowly with time. The presence of this wave (often called a distortion wave) is explained by differential rotation of the star, its surface being covered with groups of spots; the period of the rotation of a spot group is usually close to the period of orbital motion (period of eclipses) but still differs from it, which is the reason for the slow change (migration) of the phases of the distortion wave minimum and maximum in the mean light curve. The variability of the wave's amplitude (which may be up to 0.2 mag in V) is explained by the existence of a long-period stellar activity cycle similar to the 11-year solar activity cycle, during which the number and total area of spots on the star's surface vary. WD Systems with white-dwarf components. WR Systems having Wolf-Rayet stars among their components (V 444 Cyg). c) Classification based on the degree of filling of inner Roche lobes AR Detached systems of the AR Lacertae type. Both components are subgiants not filling their inner equipotential surfaces. D Detached systems, with components not filling their inner Roche lobes. DM Detached main-sequence systems. Both components are main-sequence stars and do not fill their inner Roche lobes. DS Detached systems with a subgiant. The subgiant also does not fill its inner critical surface. DW Systems similar to W UMa systems in physical properties (KW, see below), but not in contact. K Contact systems, both components filling their inner critical surfaces. KE Contact systems of early (O-A) spectral type, both components being close in size to their inner critical surfaces. KW Contact systems of the W UMa type, with ellipsoidal components of F0-K spectral type. Primary components are main-sequence stars and secondaries lie below and to the left of the main sequence in the (MV,B-V) diagram. SD Semidetached systems in which the surface of the less massive com- ponent is close to its inner Roche lobe. The combination of the above three classification systems for eclipsers results in the assignment of multiple classifications for object types. These are separated by a solidus ("/") in the data field. Examples are: E/DM, EA/DS/RS, EB/WR, EW/KW, etc. 6. Optically Variable Close Binary Sources of Strong, Variable X-ray Radiation (X-ray Sources) X Close binary systems that are sources of strong, variable X-ray emis- sion and which do not belong to or are not yet attributed to any of the above types of variable stars. One of the components of the system is a hot compact object (white dwarf, neutron star, or possibly a black hole). X-ray emission originates from the infall of matter onto the compact object or onto an accretion disk surrounding the compact object. In turn, the X-ray emission is incident upon the atmosphere of the cooler companion of the compact object and is reradiated in the form of optical high-temperature radiation (reflection effect), thus making that area of the cooler companion's surface an earlier spectral type. These effects lead to quite a peculiar complex character of optical variability in such systems. These objects may be subdivided into the following types: XB X-ray bursters. Close binary systems showing X-ray and optical bursts, their duration being from several seconds to ten minutes, with amplitudes of about 0.1 mag in V (V 801 Ara, V 926 Sco); XF Fluctuating X-ray systems showing rapid variations of X-ray (Cygnus X-1 = V1357 Cyg) and optical (V821 Ara) radiation on time scales of dozens of milliseconds; XI X-ray irregulars. Close binary systems consisting of a hot compact object surrounded by an accretion disk and a dA - dM-type dwarf. These display irregular light changes on time scales of minutes and hours, and amplitudes of about 1 mag in V. Superposition of a periodic variation because of orbital motion is possible (V818 Sco); XJ X-ray binaries characterized by the presence of relativistic jets evident at X-ray and radio wavelengths, as well as in the optical spectrum in the form of emission components showing periodic displacements with relativistic velocities (V1343 Aql); XND X-ray, novalike (transient) systems containing, along with a hot compact object, a dwarf or subgiant of G-M spectral type. These systems occasionally rapidly increase in brightness by 4-9 mag in V, in the visible simultaneously with the X-ray range, with no envelope ejected. The duration of the outburst may be up to several months (V616 Mon); XNG X-ray, novalike (transient) systems with an early-type supergiant or giant primary component and a hot compact object as a companion. Following the main component's outburst, the material ejected by it falls onto the compact object and causes, with a significant delay, the appearance of X rays. The amplitudes are about 1-2 mag in V (V725 Tau); XP X-ray pulsar systems. The primary component is usually an ellipsoidal early-type supergiant. The reflection effect is very small and light variability is mainly caused by the ellipsoidal primary component's rotation. Periods of light changes are between 1 and 10 days; the period of the pulsar in the system is from 1 s to 100 min. Light amplitudes usually do not exceed several tenths of a magnitude (Vela X-1 = GP Vel); XPR X-ray pulsar systems featuring the presence of the reflection effect. They consist of a dB-dF-type primary and an X-ray pulsar, which may also be an optical pulsar. The mean light of the system is brightest when the primary component is irradiated by X rays; it is faintest during a low state of the X-ray source. The total light amplitude may reach 2-3 mag in V (HZ Her); XPRM X-ray systems consisting of a late-type dwarf (dK-dM) and a pulsar with a strong magnetic field. Matter accretion on the compact object's magnetic poles is accompanied by the appearance of variable linear and circular polarization; hence, these systems are sometimes known as "polars". The amplitudes of the light changes are usually about 1 mag in V but, provided that the primary component is irradiated by X rays, the mean brightness of a system may increase by 3 mag in V. The total light amplitude may reach 4-5 mag in V (AM Her, AN UMa). If the beam of X-ray emission originating at the magnetic poles of the rotating hot compact object does not pass through the observer's position and the system is not observed as a pulsar, the letter "P" in the above symbols for X-ray- system types is not used. If an X-ray system is also an eclipsing or an ellipsoidal variable, the X-ray symbol is preceded by "E" or "ELL" joined with the X-ray symbol by a "+" sign (e.g., E+X, ELL+X). 7. Other Symbols In addition to the variable-star types described above, certain other symbols that need to be explained will be found in the Type data field: BLLAC Extragalactic BL Lacertae-type objects. These are compact quasistellar objects showing almost continuous spectra with weak emission and absorption lines and relatively rapid irregular light changes with amplitudes up to 3 mag in V or more. Sources of strong X-ray radiation and radio waves, their emission displays strong and variable linear polarization in the visible and infrared spectral regions. Some objects of this type, considered erroneously to be variable stars and designated in the GCVS system, will probably sometimes be included in the main table of the Catalogue in the future, too. CST Nonvariable stars, formerly suspected to be variable and hastily designated. Further observations have not confirmed their variability. GAL Optically variable quasistellar extragalactic objects (active galactic nuclei [AGNs]) considered to be variable stars by mistake. L: Unstudied variable stars with slow light changes. QSO Optically variable quasistellar extragalactic sources (quasars) that earlier were erroneously considered to be variable stars. S: Unstudied variable stars with rapid light changes. * Unique variable stars outside the range of the classifications de- scribed above. These probably represent either short stages of transition from one variability type to another or the earliest and latest evolutionary stages of these types, or they are insufficiently studied members of future new types of variables. + If a variable star belongs to several types of light variability simultaneously, the types are joined in the Type field by a "+" sign (e.g., E+UG, UV+BY). ======================================================================== (End) N.N. Samus [Moscow Inst. Astron.], O.V. Durlevich [Sternberg Astron. Inst., Moscow] 6-May-1998 Description originale du catalogue : II/214A Combined General Catalogue of Variable Stars (Kholopov+ 1998) ================================================================================ The Combined General Catalogue of Variable Stars, 4.1 Edition. General Catalogue of Variable Stars 4th Edition, Volumes I-III, Kholopov P.N., Samus N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kireeva N.N., Kukarkina N.P., Kurochkin N.E., Medvedeva G.I., Pastukhova E.N., Perova N.B., Rastorguev A.S., Shugarov S.Yu. <Moscow: Nauka Publishing House (1985-1988)> General Catalogue of Variable Stars Volume IV, 4th ed. The cross-identification tables. Kholopov P.N., Samus N.N., Durlevich O.V., Kazarovets E.V., Kireeva N.N., Tsvetkova T.M. <Institute of Astronomy of Russian Academy of Sciences and Sternberg State Astronomical Institute of the Moscow State University, Nauka, Moscow, (1990)> General Catalogue of Variable Stars, 4rd ed., vol.V. Extragalactic Variable Stars Artiukhina N.M., Durlevich O.V., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kholopov P.N., Kireeva N.N., Kurochkin N.E., Lipunova N.A., Medvedeva G.I., Pastukhova E.N., Samus N.N., Tsvetkova T.M. <"Kosmosinform", Moscow, (1995)> 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)> ================================================================================ ADC_Keywords: Stars, variable; Combined data; Supernovae Description: The GCVS is the only reference source on all known variable stars. This version contains all of the electronically-readable version as distributed by the Sternberg Astronomical Institute and Institute of Astronomy (Russian Acad.Sci.), Moscow. It includes the catalog of variable stars, updated and completed with the seven Name-Lists of Variables Stars Nos.67-73 (see IBVS No.2681,1985; No.3058,1987; No.3323,1989; No.3530,1990; No.3840,1993; No.4140,1995; No.4471,1997), a catalog of suspected variables, a cross-index of variable star names, a catalog of extragalactic variables, and a catalog of supernovae. Introduction: The present improved electronic version of the GCVS4 Volumes I-V, combined with Name-Lists of Variable Stars Nos.67-73, are also available from Sternberg Institute via anonymous ftp to ftp.sai.msu.su, /pub/groups/cluster/gcvs... and via http://www.sai.msu.su/groups/cluster/gcvs/ . The information at this site is regularly updated (corrections of detected mistakes, improvements of identifications and coordinates, etc.). gcvs.dat is the combined computer-readable version of the GCVS4 Vols. I-III (Kholopov et al. 1985-1988) and Name-Lists of Variable Stars Nos.67-73 (1985IBVS.2681....1K, 1987IBVS.3058....1K, 1989IBVS.3323....1K, 1990IBVS.3530....1K, 1993IBVS.3840....1K, 1995IBVS.4140....1K and 1997IBVS.4471....1K) published in the system introduced during the preparation of the 4th GCVS edition. The total number of designated variable stars has now reached 31918; of them, 3506 stars enter the Name-Lists Nos.67-73. Errors detected in the printed Volumes I-III and in the Name-Lists were corrected; the file includes also improved equatorial positions for some variable stars. crossid.dat contains all variables, including extragalactic variables, stars from the Name-Lists, and stars suspected of variability since the compilation of the NSV catalog, ordered by right ascension (B1950). The authors tried to provide as complete lists as possible for the stars identified with the catalogues HD, BD, CoD, CPD, BS, ADS and for the stars with preliminary HV (Harvard Variable) designations. As for the other catalogues, their task here was more difficult since they had to rely upon references to source catalogue names made by variable star researchers; the tables in the present volume reproduce the materials used in their work, and incompleteness seems to be unavoidable. Starting with Name-List No.71, the identifications became more reliable and complete thanks to special effort of the compilers. The final, fifth volume contains data for variables in external galaxies (including the Magellanic Clouds) and for extragalactic supernovae (see evs*.dat and sn*.dat). All variables in the present data set are arranged in the order of their names inside constellations. For Name-list stars, the information follows the format of the Name-Lists, that is, it includes only coordinates, the variability type, the range of brightness variations, and references. The file nsv.dat is a compilation of 14811 stars suspected of variability and not finally designated as variables prior to 1980. It is the successor to the "Catalogues of Stars Suspected of Variability" published in 1951 and 1965 (Kukarkin et al.). Data contained in the present catalog include positions, magnitudes, variability types, alternate designations, and references to the literature. The computer version of NSV contains principally the same data as in the printed catalog, but only the data table without the textual material (bibliography, remarks) is included. Necessary corrections were introduced, as of June, 1997, and coordinates were improved, compared to the printed version, for about half of the stars in the catalog. The Sternberg Institute has started preparation of an electronic release GCVS 4.2 which will contain improved light elements, classifications etc. along with sufficiently accurate positional information. The first approach to this project has resulted in improved equatorial positions (B1950, J2000) for variable stars in the constellations of Andromeda, Antlia and Apus including the stars from the GCVS proper plus the stars from the subsequent Name-lists, with a new standard of positional accuracy, to 1 second of arc (IAU Inform. Bull. Var. Stars, in preparation). These positions have been incorporated in the present data set. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file gcvs.dat 170 31991 Combined GCVS (vols I-III and name lists) crossid.dat 36 98642 *The Cross-Identifications of Variable Stars evs_cat.dat 154 10979 Extragalactic Variable Stars. Catalogue evs_rem.dat 82 1926 Extragalactic Variable Stars. Remarks evs_ref.dat 80 667 Extragalactic Variable Stars. References sn_cat.dat 128 984 Extragalactic supernovae. Catalogue sn_rem.dat 80 277 Extragalactic supernovae. Remarks sn_ref.dat 80 719 Extragalactic supernovae. References nl_ref.dat 80 2567 References for name lists nsv.dat 89 14811 *Suspected variables vartype.txt 80 918 Description of variability types -------------------------------------------------------------------------------- Note on crossid.dat: this file is Version 1.2; it replaced version 1.1 on 22 May 1999; further corrections applied on 16-Jun-1999. Note on nsv.dat: a newer version of this file is available in Cat. <II/219> -------------------------------------------------------------------------------- See also: II/195 : Namelists of variable stars II/219 : New Suspected Variable Stars Supplement (Kazarovets+ 1999) ftp://ftp.sai.msu.su/pub/groups/cluster/gcvs : Sternberg files http://www.sai.msu.su/groups/cluster/gcvs/gcvs/ : GCVS Database Byte-by-byte Description of file: gcvs.dat ------------------------------------------------------------------------------ Bytes Format Units Label Explanations ------------------------------------------------------------------------------ 1- 3 I3 --- Constell [1/88]Constellation numeric code 4- 7 I4 --- Number Star number within the constellation 8 A1 --- Component *Component identification 9- 18 A10 --- GCVS *Variable star designation 19 A1 --- NoteFlag *[*] Notes in published catalog 20- 21 I2 h RAh *? Hours RA, equinox 1950.0 22- 23 I2 min RAm *? Minutes RA, equinox 1950.0 24- 27 F4.1 s RAs *? Seconds RA, equinox 1950.0 28 A1 --- DE- *Sign Dec, equinox 1950.0 29- 30 I2 deg DEd *? Degrees Dec, equinox 1950.0 31- 32 I2 arcmin DEm *? Minutes Dec, equinox 1950.0 33- 34 I2 arcsec DEs *? Seconds Dec, equinox 1950.0 35 A1 --- u_DEs *[:*'] position accuracy flags 36- 45 A10 --- VarType *Type of variability 46 A1 --- l_magMax [<>(] ">" if magMax is a faint limit "<" if magMax is a bright limit "(" if magMax is an amplitude 47- 52 F6.3 mag magMax ? Magnitude at maximum brightness 53 A1 --- u_magMax Uncertainty flag (:) on magMax 54 A1 --- f_magMax [)] ")" if magMax is an amplitude 55 A1 --- l_magMin [<(] "<" if magMin is a bright limit "(" if magMin is an amplitude 57- 62 F6.3 mag magMin ? Minimum magnitude or amplitude 63 A1 --- u_magMin Uncertainty flag (:) on magMin 64 A1 --- n_magMin *Alternative photometric system for magMin 65 A1 --- f_magMin [)] ")" if magMin is an amplitude 66- 67 A2 --- magCode *The photometric system for magnitudes 68- 81 F14.6 d Epoch *? Epoch for maximum light, Julian days 82 A1 --- q_Epoch *[:+-] Quality flag on Epoch 83- 86 I4 --- YearNova *?Year of outburst for nova 87 A1 --- l_Period *[<>(] Code for upper or lower limits 88-103 F16.10 d Period ? Period of the variable star 104 A1 --- u_Period Uncertainty flag (:) on Period 105-107 A3 --- n_Period *[*/N) ] Uncertainty notes on Period 108-110 A3 % M-m/D *Rising time (M-m) or duration of eclipse (D) 111 A1 --- u_M-m/D Uncertainty flag (:) on M-m/D 112 A1 --- n_M-m/D *[*] Note for eclipsing variable 113-129 A17 --- SpType Spectral type 130-134 A5 --- Ref1 *Reference to a study of the star 136-140 A5 --- Ref2 *Reference to a chart or photograph 142-155 A14 --- Exists *Cases of non-existence of the variable etc. 156-157 I2 h RA2000h ? Hours RA, equinox 2000.0 158-159 I2 min RA2000m ? Minutes RA, equinox 2000.0 160-163 F4.1 s RA2000s ? Seconds RA, equinox 2000.0 164 A1 --- DE2000- Sign Dec, equinox 2000.0 165-166 I2 deg DE2000d ? Degrees Dec, equinox 2000.0 167-168 I2 arcmin DE2000m ? Minutes Dec, equinox 2000.0 169-170 I2 arcsec DE2000s ? Seconds Dec, equinox 2000.0 ------------------------------------------------------------------------------- Note on Component: designations of components of double/multiple stars: A,B; 1,2,3 ... (tau 1). Usually only one component of the binary is variable, but there exist two cases (CE Cas A,B; EQ Peg A,B) when both components are variable and enter the catalogue as separate lines. Note on GCVS: traditional transliterations of greek letters are used. Lower- and upper-case latin letters must be distinguished (e.g. u Her and U Her). Note on NoteFlag: see the document by Kholopov et al. (1985-1988). Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs: the position is not listed when the variable is equivalent to another catalogued variable ("=" in column Exists, byte 142). Note on u_DEs: the real coordinates accuracy uses the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. (') means right ascensions accurate to one minute of time and declinations accurate to one arcminute. Note on VarType: type of variability. The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67- 72 and in the GCVS vol.V (see file "vartype.txt"). Note on n_magMin: Code for alternative photometric system. Field is non-blank if magMin is a magnitude or amplitude given in a system other than that indicated by magCode. An asterisk in the corresponding position means the amplitude measured in white light. Note on magCode: the photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). See also the documents by Kholopov et al. (1985-1988) or Warren (1989). Several stars from the 68th Name-List have in these positions "1." designating the 1.04 micrometer band of the system introduced by G.W.Lockwood. The designations u,v,b,y refer to the Stroemgren system. The symbols "I" and "R" mean magnitudes in Cousins' I system. "g" designates magnitudes in the system of Thuan and Gunn; "T" stands for broad-band Tycho magnitudes formed from B and V measurements; "r" are red magnitudes not tied to a particular system. Note on Epoch, YearNova: Epochs are given for minimum light for all eclipsing and ellipsoidal variables, as well as for RV Tau and RS CVn types, and for maximum for all other types. This rule may occasionally be broken, but this is explained only in the remarks to the catalog, which are not available in machine-readable form at this time. The epochs are Julian dates. For novae (types N) and supernovae (types SN), the Epoch is completed by a year of outburst in the YearNova column. Note on q_Epoch: the following codes are used (see also note on Epoch) : ":" epoch is uncertain. "+" epoch may be later than that reported; "-" epoch may be earlier than that reported. Note on l_Period: the following codes are used: ">" or "<" if period is a lower or upper limit, respectively. "(": the period is the mean cycle time of a U Gem or recurrent nova (in this case, there is ")" in n_Period column) Note on n_Period: the following codes are used: "*N" if the period may be a multiple of the quoted value; "/N" if the period may be a fraction of the quoted value; ")" - see the note on l_Period. Note on M-m/D: this column holds the rising time (M-m) of intrinsic variables, or the duration of the eclipse (D) for eclipsing binaries. These values help to define the shape of the light curve. The value is given in percentage of the period of the star. Note on n_M-m/D: the "*" indicates that the duration of the light constancy phase at minimum light (d) for an eclipsing variable is equal to zero. Note on Ref1, Ref2: "00001" - if the main characteristics of the star were determined by the authors themselves. "00002" - "09148" - Vol. I GCVS (see Kholopov et al., 1985-1988). "09149" - "09558" - Vol. II GCVS "09559" - "10200" - Vol. III GCVS "V 001" - "V 554" - Vol. V GCVS (see file evs_ref.dat) "67001" - "73381" - Name-Lists Nos.67-73 (see file nl_ref.dat) If no chart is available for the variable, but the star is contained in one of the Durchmusterung catalogs or the Hubble Space Telescope Guide Star Catalog, the corresponding abbreviation (BD, CPD, CoD, GSC) is given. Note on Exists: the following codes are used in column Exists: "N" in byte 142 if the star does not exist. "=" in byte 142 appears in three cases. First, it is used if the variable is equivalent to another catalogued variable. In such case, after the "=" symbol, the alternative name of the variable follows, and all necessary information on the star is to be found under that alternative name. Second, it is used for all variables of the Name-Lists Nos.67-73, it is followed by the two-digit number of the Name-list and the four-digit number of the star in the Name-list, and the information for the star follows the format of the Name-lists (see above). Third, the "=" symbol may be followed by the star's name in the GCVS Vol. V (see the file evs_cat.dat). This means that the star enters also Vol. V, and the information of Vol. V makes it possible to improve the data of Vols. I-III. In this case, the symbol "*" in byte 153 means the presence of remarks in Vol. V; the symbol(s) "n" or "n:" in bytes 154-155 means that the star is nonmember (possible nonmember) of the galaxy in question. ------------------------------------------------------------------------------ Byte-by-byte Description of file: crossid.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 A4 --- Cat *Abbreviated name of catalog or list 6- 16 A11 --- Seq Star number or name in the respective catalog 18- 21 A4 --- m_Seq *Component designation 23- 34 A12 --- Vname *Designation in GCVS or NSV 35 A1 --- m_var *Component designation 36 A1 --- IDflag [:] Uncertainty flag on cross-identification. -------------------------------------------------------------------------------- Note on Cat: -------------------------------------------------------------------- ADS = R.G.Aitken, 'New General Catalouge of Double Stars', Carnegie Inst. of Washington Publ. no.417, vols.I, II, 1932 AN = Preliminary designations of variable stars introduced by the 'Astronomische Nachrichten' AS = P.W. Merrill, C.G.Burwell, 'Additional Stars whose Spectra have a Bright H Alpha Line', Astrophys. J. 112, 72, 1950 (=1950ApJ...112...72M); see also Astrophys. J. 113, 624, 1951 (=1951ApJ...113..624M) BAY = Bayer, list of those bright stars having designations by Greek letters in their constellations BD = Bonner Durchmusterung, F.W.A. Argelander, Bonner Sternverzeichniss, 1 bis 4 sektion, Astronomische Beobachtungen auf der Sternwarte de Kgl. Rhein/ Friedrich-Wilhelms-Unviersiaet zu Bonn (Catalogs <I/119> and <I/122>) BS (HR) = D. Hoffleit, 'The Bright Star Catalogue', 4th Revised Ed., Yale University Observatory, New Haven, Conn. USA, 1982 (see catalog <V/50>) CoD = Cordoba Durchmusterung, J. M. Thome, Resultados del Observatorio Nacional Argentino 16 - 18; 21, 1892-1932 (catalog <I/114>) CPD = Cape Photographic Durchmusterung, D. GIll and J. C. Kapteyn, Ann. Cape Obs. 3-5, 1895 - 1900 (catalog <I/108>) CRL (AFGL) = Air Force Geophysics Laboratory. Four-Color Infrared Sky Survey (and supplement): S.D. Price and R.G. Walker - AFGL-TR-76-028 (Hanscom AFB, MA, Air Force Geophysics Lab., Air Force Systems Command, USAF, 1976; S.D. Price and T.L. Murdock - Air Force Geophysics Laboratory, AFGL-TR-83-0161 (see catalog <II/94>) EG = O.J. Eggen, J.L. Greenstein, 'Spectra, Colors, Luminosities, and Motions of the White Dwarfs', Astrophys. J. 141, 83 (1965ApJ...141...83E); additional stars in Astrophys. J. 142, 925 (1965ApJ...142..925E) and 150, 927 (1967ApJ...150..927E); more stars added by J.L. Greenstein, see references in McCook and Sion, Astrophys. J. Suppl. 65, 603 (1987ApJS...65..603M) FLM = Flamsteed, List of those bright stars having designations by number in their constellations G = H.L. Giclas, R. Burnham Jr., and N.G. Thomas, (Large Proper Motion Stars) - Publications of Lowell Obs., Flagstaff, Arizona, 1971 (Catalogs <I/79> and <I/112>) GD = H.L. Giclas White Dwarfs (Lowell Obs.) Gl = W. Gliese, 'Catalogue of Nearby Stars', Veroeff. Astron. Rechen-Inst. Heidelberg nr.22, 1969; W. Gliese, H. Jahreiss, 'Nearby star data published 1969-1978', Astron. Astrophys. Suppl. 38, 423 (1979A&AS...38..423G); see catalog <V/70> HD = Henry Draper Catalogue - A.J. Cannon and E.C. Pickering, Havard Obs. Ann. 91 - 99, 1918-1924; A. J. Cannon, Harvard Obs. Ann. 100, 1925 - 1936; see catalog <III/135> He = A number of lists of planetary nebulae and emission-line stars by K. Henize HII = E. Hertzsprung, 'Catalogue de 3259 Etoiles dans les Pleiades', Ann. Sterrewacht Leiden, 19, pt. 1A, 1947 HRC = G.H. Herbig, N.K. Rao, 'Second Catalog of Emission-line Stars of the Orion Population', Astrophys. J. 174, 401 (1972ApJ...174..401H); G.H. Herbig, K.R. Bell, 'Third Catalog of Emission-Line Stars of the Orion Population', Lick Obs. Bull. no. 1111, 1988 (catalog <V/73>) HV = Harvard variables IRC = G. Neugebauer, R.B. Leighton, 'Two-Micron Sky Survey, A Preliminary Catalog', NASA SP-3047, 1969; catalog <II/2> LH = Lick H Alpha: A number of lists of emission-line stars by G.H. Herbig MH = Mount Wilson H-Alpha Stars, see references for MWC and AS MWC = P.W. Merrill, C.G. Burwell, 'Catalogue and Bibliography of Stars of Classes B and A Whose Spectra have Bright Hydrogen Lines', Astrophys. J. 78, 87 (1933ApJ....78...87M) (Mount Wilson Catalogue); Supplements: Astrophys. J. 98, 153 (1943ApJ....98..153M); 110, 387 (1949ApJ...110..387M) OH = OH sources designated by their galactic coordinates Par = A List of Stars in the Region of the Orion Nebula (P.P. Parenago, Sternberg Inst. Publ. vol. 25, 1954; catalog <II/171>) PG = Palomar-Green survey S = Preliminary designations of variables discovered at Sonneberg Observatory SAO = 'Smithsonian Astrophysical Observatory Star Catalog', parts I-IV, Smithsonian Inst. Washington, 1966 (catalog <I/131>) SVS = Soviet Variable Stars (preliminary designations of Soviet-discovered variables) VV = Vatican variable stars WD = G.P. Mc Cook, E.M. Sion, 'Catalog of Spectroscopically Identified White Dwarfs', Astrophys. J. Suppl. 65, 603 (1987ApJS...65..603M); see catalog <III/129>. WR = K.A. van der Hucht et al. 'The Sixth Catalogue of Galactic Wolf-Rayet Stars, Their Past and Present', Space Sci. Rev. 28, 227, 1981 (Catalog <III/85>) -------------------------------------------------------------------- Note on m_Seq, m_Variable: 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 may also appear. In the cases of ADS 03201 and ADS 03202 the symbols k1 and k2 mean kappa 1 and kappa 2, respectively. Note on Vname: name of the object in the GCVS, its Volume V, or the NSV. Lower- and upper-case latin letters must be distinguished (e.g. u Her and U Her). -------------------------------------------------------------------------------- Byte-by-byte Description of file: evs_cat.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- GalNo *[89/123] Galaxy code 4- 7 I4 --- VarNo *Variable star number within the galaxy 9- 20 A12 --- Name *Variable star designation 21 A1 --- RemFlag [*] indicates a remark in file evs_rem.dat 22- 23 I2 h RAh *Right ascension, equinox 1950.0 24- 25 I2 min RAm (minutes) 26- 30 F5.2 s RAs (seconds) 31 A1 --- DE- sign of declination, 1950.0 32- 33 I2 deg DEd *Declination, equinox 1950.0 34- 35 I2 arcmin DEm (arc minutes) 36- 39 F4.1 arcsec DEs (arc seconds) 40 A1 --- u_DEs *[":*!] accuracy flags 41- 48 A8 --- VarType *Type of variability 49- 53 F5.2 mag magMax ?Magnitude at maximum brightness 54 A1 --- u_magMax Uncertainty flag (:) on magMax 55 A1 --- l_magMin *[<(] magMin is an upper limit or amplitude 56- 60 F5.2 mag magMin *?Magnitude at minimum brightness, or amplitude 61 A1 --- u_magMin Uncertainty flag (:) on magMin 62 A1 --- n_magMin *[)] ")" if magMin is an amplitude 63 A1 --- magCode *Code for photometric system 64- 77 F14.6 d Epoch *?Epoch 78 A1 --- u_Epoch Uncertainty flag on Epoch 79 A1 --- l_P *[(] '(' for U Gem 80- 92 F13.8 d P *?Period 93 A1 --- u_P Uncertainty flag (:) on P 94 A1 --- n_P *[)] ')' for U Gem 95- 96 I2 % M-m/D *?M-m or D 97 A1 --- u_M-m/D Uncertainty flag (:) on M-m/D 98 A1 --- n_M-m/D *[*] Note for eclipsing variable 99-104 A6 --- SpType *Spectrum 106-108 A3 --- evsRef1 Reference for study of the star, see file evs_ref.dat 109-111 A3 --- evsRef2 Reference for chart or photograph, see file evs_ref.dat 113-126 A14 --- Desig1 designation in paper Ref1 127-138 A12 --- Desig2 designation in paper Ref2 139-146 A8 --- VarName Designation in gcvs.dat or nsv.dat 148-149 A2 --- nonMem *[n: ] Non-member note 150-153 I4 yr YearNova *? Year of outburst 154 A1 --- u_YearNova [:] Uncertainty flag on YearNova -------------------------------------------------------------------------------- Note on GalNo: Code identifying the galaxy. This numbering system begins with 089, the first 88 codes being reserved for constellations (cf. catalog <II/139>). Note that NGC 1466 is a globular cluster (not a galaxy) between the LMC and the SMC; we presented it separately, because it is not clear to which galaxy to attribute its variable stars. Note on VarNo: variable star No within the galaxy. Number of the variable star in the galaxy. If in the literature for the considered galaxy there exist several different variable star numbering systems, we have introduced new numbers in the order of increasing right ascension for the equinox 1950.0. But if the variable star numbering system for the galaxy is practically of general use, we have retained it - if necessary, with additional numbers ordered by increasing right ascension. Note on Name: Variable star Designation. The name of the variable in the adopted system of variable star designations: name of the galaxy + "V" + variable star No. within the galaxy (see column VarNo) Note on RAh, DEd: If the star's coordinates are only roughly known, they are nevertheless formally presented to one second of time in right ascension (with the decimal point following) and to one arcsecond in declination (with the decimal point following). See column u_DEs which indicates the real accuracy. Note on u_DEs: the real coordinates accuracy uses the symbols: (") means right ascensions accurate to one second of time and declinations accurate to one arcsecond; (:) means declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. (!) for V0474 in the Sculptor system, the listed coordinates refer to the galaxy's center since the coordinates of the star itself are unknown. Note on VarType: type of variability. The classification systems corresponds to the GCVS vols. I-III (catalog <II/139>), with the addition of the new "BLBOO" type, called after the prototype star BL Boo = NGC 5466 V19 referring to the so-called "anomalous Cepheids", i.e. stars with periods characteristic of comparatively long-period RRAB variables, but considerably brighter by luminosity. There are also suspected variables designated by the symbol "var:". Note on l_magMin, magMin, n_magMin: minMag contains the minimum brightness, or the variability amplitude instead (in brackets, i.e. l_magMin='(' and n_magMin=')'). (<) means that minMag is an upper limit (light) Note on magCode: designation of the photometric band. P means photographic magnitudes, V means visual or photovisual magnitudes as well as V system magnitudes. In the latter case, they are usually distinguishable from visual magnitudes by the number of digits after the decimal point (as a rule, V system magnitudes are based upon photoelectric or CCD photometry). Letters U, B, R, I, J, H, K, L, M, N, O, Q mean, as a rule, magnitudes expressed in corresponding systems of broad-band photometry. Note on Epoch, YearNova: The epoch expressed as Julian Date. For eclipsing and ellipsoidal variables, RV Tau and RS CVn stars, the catalogue gives epochs of minimum light, and for the rest of variables, epoch of maximum light. For novae (types N) and supernovae (types SN), the Epoch is completed by a year of outburst (YearNova column). Note on l_P, P, l_P, n_P: For U Gem stars and recurrent novae, the P column gives (in brackets) the mean cycle value, if known. Note on M-m/D, n_M-m/D: Duration of light increase from minimum to maximum (M-m) for intrinsic variable stars or the eclipse duration (D) for Algol type variables are expressed in hundredths of the photometric period for the star in question. An asterisk (*) in n_M-m/D means, for an eclipsing variable, that the duration of the constant brightness phase in minimum (d) for this star is equal to zero. Note on SpType: If there exist several spectral type determinations for a star, we preferred more recent ones, taking into account reliability of each determination. We converted symbols "d" (dwarfs) and "g" (giants) into luminosity classes V and III. If a nova showed spectral features typical of novae during or after the outburst, a symbol (NOVA) is given in this column. If the spectrum shows features characteristic of U Gem variables, this column contains the symbol (UG). Continuous spectrum is designated "cont", the symbol "e" means emission spectrum, lower case letters "ea", "eb" in this column stand for "e alpha", "e beta". For RR Lyrae stars, spectral types from hydrogen lines are given. A plus sign (+) between two spectral type values means that spectra of two components of a spectroscopic binary are observed. Two spectral type values separated with a minus sign (-) mean the range of spectral type variations in the process of brightness changes. Note on nonMem: Symbols "n" or "n:" for nonmembers (possible nonmembers) of the galaxy in question. For the stars that enter the GCVS vols. I-III (file gcvs.dat) or the NSV catalogue (file "nsv.dat") and are not members of the corresponding galaxy, the present volume gives only the running number, coordinates, the symbol "n", and the GCVS or NSV name. -------------------------------------------------------------------------------- Byte-by-byte Description of file: evs_rem.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 12 A12 --- Name *Variable star designation 14- 82 A69 --- Text Text of remark -------------------------------------------------------------------------------- Note on Name: When more than one line is required, this field is repeated. -------------------------------------------------------------------------------- Byte-by-byte Description of file: evs_ref.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 A3 --- evsRef Reference number, repeated if more than 1 line 4 A1 --- --- [.] Period ending number 6- 80 A75 --- Text Text of reference -------------------------------------------------------------------------------- Byte-by-byte Description of file: sn_cat.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- SN Supernova designation 7 A1 --- n_SN [-?] Doubtful (?), or rejected (-) SN 8 A1 --- RemFlag [*] The '*' indicates a remark in sn_rem.dat 10- 19 A10 --- Gal *Parent galaxy designation 21- 22 I2 h RAh ?RA 1950 (hours) of Parent galaxy 23- 24 I2 min RAm ?Right Ascension 1950 (minutes) 25- 28 F4.1 s RAs ?Right Ascension 1950 (seconds) 29 A1 --- DE- Declination 1950 (sign) 30- 31 I2 deg DEd ?Declination Deg. 1950 of Parent galaxy 32- 33 I2 arcmin DEm ?Declination 1950 (minutes) 34- 35 I2 arcsec DEs ?Declination 1950 (seconds) 36 A1 --- u_DEs *[":'] Accuracy flags 37- 42 A6 --- MType Type of the parent galaxy 43- 47 F5.2 mag BT ?Integrated magnitude of parent galaxy 48 A1 --- u_BT [: ]Uncertainty flag (:) on BT 49 A1 --- n_BT [BJV] Band indicator, blank for photographic 51- 58 A8 --- maxDate *Date of the SN's maximum or of discovery 60- 64 F5.2 mag magMax ?Magnitude at maximum (light) of SN 65 A1 --- u_magMax [: ]Uncertainty flag (:) on magMax 66 A1 --- n_magMax [BJVRIKr] Band indicator, blank for photographic 67 A1 --- f_magMax *[*] '*' if maximum not observed 69- 73 F5.1 arcsec dRA *?Distance of SN from galaxy nucleus 74- 75 A2 --- oRA [NSEW:? ] Orientation of dRA 77- 81 F5.1 arcsec dDE *?Distance of SN from galaxy nucleus 82- 83 A2 --- oDE [NSEW:? ] Orientation of dDE 84- 85 I2 h RASN.h ?Right Ascension 1950 (hours) of SN 86- 87 I2 min RASN.m ?Right Ascension 1950 (minutes) 88- 91 F4.1 s RASN.s ?Right Ascension 1950 (seconds) 92 A1 --- DESN.- Declination 1950 (sign) 93- 94 I2 deg DESN.d ?Declination 1950 (degrees) of SN 95- 96 I2 arcmin DESN.m ?Declination 1950 (minutes) 97- 98 I2 arcsec DESN.s ?Declination 1950 (seconds) 99 A1 --- u_DESN.s *[":'] accuracy flags on SN position 100-105 A6 --- SNType *SN classification 107-122 A16 --- Discov *Name of the SN discoverer 123-125 A3 --- snRef1 *Reference for study of the star 126-128 A3 --- snRef2 *Reference for chart or photograph -------------------------------------------------------------------------------- Note on Gal: "N" means NGC catalogue numbers, "I" refers to the IC catalogue, "U" to the UGC catalogue, "M" to the MCG catalogue, "E" to ESO survey lists. "An" means an anonymous galaxy "Intergal" is for cases when the supernova cannot be reliably attributed to a particular galaxy and is considered intergalactic. Note on u_DEs, u_DESN.s: The real coordinates accuracy is denoted by (") means right ascensions accurate to one second of time and declinations accurate to one arcsecond; (:) means declinations accurate to one tenth of an arcminute; (') means declinations accurate to one arcminute. Note on maxDate, f_magMax: The date of the SN's maximum or of discovery, or of an isolated observation at high brightness. If maxDate or f_magMax contains an asterisk (*), it means that the date and/or the magnitude refer not to the maximum (not covered with observations), but to the EPOCH OF DISCOVERY or to an isolated observation at high brightness. As a rule, information about maxima was not included if it was based on considerable extrapolation. Note on dRA: In line 393, 1970K, the offset is 0.3E Note on dDE: In line 732, 1988T, the offset is 0.4N Note on SNType: Limited to types I (I-A, I-B) and II (II-l, II-pl), with possible indications of peculiarities (pec). Note on Discov: In case of several discoverers, the name of the first author of the discovery is given followed by "+" symbol. As a rule, information on independent rediscoveries is not presented in the remarks, for the sake of brevity. The abbreviation "BASST" in this column means that the supernova was discovered by the Berkeley Automated Supernova Search Team. Note on snRef1 and snRef2: See file sn_ref.dat -------------------------------------------------------------------------------- Byte-by-byte Description of file: sn_rem.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- SN Supernova designation, repeated if more than 1 line 7 A1 --- n_SN [-?] Doubtful (?), or rejected (-) SN 9- 80 A72 --- Text Text of remarks -------------------------------------------------------------------------------- Byte-by-byte Description of file: sn_ref.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 A3 --- snRef Reference number, repeated if more than 1 line 4 A1 --- --- [. ] Period following Reference number 6- 80 A75 --- Text Text of reference -------------------------------------------------------------------------------- Byte-by-byte Description of file: nl_ref.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 A2 --- NLnum Name-List number 3- 5 A3 --- Ref *Reference number 7- 80 A74 --- Text Text of reference -------------------------------------------------------------------------------- Note on Ref: In the present version the authors attempted to give Latin transliterations of Russian-language names of astronomical periodicals and books. They did not try to unify the Latin spelling of names with Cyrillic (or other) original forms, but simply tried to reproduce the Latin transcriptions in the publications referred to. Of course this may lead to some confusion, hopefully minor. If a paper enters lists of references of several Name-Lists, it appears several times in the present version. ------------------------------------------------------------------------------ Byte-by-byte Description of file: nsv.dat ------------------------------------------------------------------------------ Bytes Format Units Label Explanations ------------------------------------------------------------------------------ 1- 5 I5 --- NSV NSV number 6 A1 --- NSVLetter *NSV letter suffix 7 A1 --- u_NSV [-]Dubitancy flag if a star's variability seems doubtful or erroneous to the catalog compilers 8 A1 --- NoteFlag1 *[*] Notes in published catalog 9- 10 I2 h RAh *?Hours RA, equinox 1950.0 11- 12 I2 min RAm *?Minutes RA, equinox 1950.0 13- 16 F4.1 s RAs *?Seconds RA, equinox 1950.0 17 A1 --- DE- *Sign Dec, equinox 1950.0 18- 19 I2 deg DEd *?Degrees Dec, equinox 1950.0 20- 21 I2 arcmin DEm *?Minutes Dec, equinox 1950.0 22- 23 I2 arcsec DEs *?Seconds Dec, equinox 1950.0 24 A1 --- u_DEs *[:*] accuracy flags 25- 29 A5 --- VarType *Type of variability 31- 35 F5.2 mag magMax *?Magnitude at maximum brightness 36 A1 --- u_magMax [:]Uncertainty flag on magMax 38- 39 A2 --- l_magMin [><(] "<" if magMin is a bright limit "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit. 40- 45 F6.3 mag magMin *?Minimum magnitude or amplitude 46- 47 A2 --- u_magMin [st:] a light amplitude is reported for the minimum and it is given in steps Uncertainty flag (:) on magMin 48 A1 --- f_magMin [)] ")" if magMin is an amplitude 49 A1 --- magCode *The photometric system for magnitudes 51- 57 A7 --- Ref1 *Reference to a study of the star see the document by Kukarkin et al.(1982) 59- 67 A9 --- Desig *Designation in paper Ref1 69- 70 A2 --- SpType *Spectral type 72- 77 A6 --- Ref2 *Chart reference see the document by Kukarkin et al.(1982) 79- 88 A10 --- VarName *Designation in GCVS 89 A1 --- NoteFlag2 [*] Notes in catalog GCVS Vol.V ------------------------------------------------------------------------------- Note on NSVLetter: The letter "A" is present for one star, NSV 10360A, which is a completely different object from NSV 10360. Note on NoteFlag1: See the document by Kukarkin et al.(1982). There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are, unfortunately, not machine readable, but they do contain much supplemental information. There, one will find information covering situations like, 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 italics in original transcriptions of the remarks. 2. The most important additional information about a star, although the NSV compilers did not intend to present complete bibliographies for any catalogued stars. 3. Remarks for visual binaries (in parentheses following the number of a star in the corresponding catalog) giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semimajor axis of a relative orbit and period of orbital motion). Data for other components are then given where applicable. (Combined magnitudes are generally reported in the machine-readable table.) Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs: The position is not listed when the variable is equivalent to a GCVS star (column VarName). Note on u_DEs: The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. Note on VarType: type of variability. The system of variable star classification corresponds to the GCVS4 (see file "vartype.txt"). Note on magMax, magMin: Magnitudes are reported to hundredths if the observations are photoelectric, 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. Note on magCode: The photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). Note on Ref1: Usually a 6-digit number coding, as a rule, the reference to the announcement of the discovery of variability. The first two digits give the year (in the 20th century) when the announcement was published (blank for the 19th century). The next four digits give the number in the list of references contained in the published catalog, which is generally the first publication announcing the possible variability. The numbers are followed by a letter code in most cases (byte 57) with the following meanings: K: the cited paper contains a chart or photograph of the field with the suspected variable marked. D: the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (DM) (BD,CD,CPD). Note on Desig: The identification of the suspected variable in the paper referenced above. DM numbers are given without a prefix, the standard naming convention of "The Henry Draper Catalogue" being used (BD for zones +89 to -22; CD for -23 to -51; CP for -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. An asterisk (*) signifies that a designation is given in the remarks to the published catalog. Stars are sometimes designated with numbers from the catalogs of Zinner (ZI, 1929) and Prager (PR, 1934, 1937) because the original discovery publications were not available to the NSV compilers. The catalogs of Zinner and Prager give detailed references to early observations of such stars. Note on SpType: Temperature classes and subclasses only are given. Most luminosity classes are III to V, but if a star is a supergiant, more detailed classification information is given in the remarks to the published catalog. The following symbols are used: AF A-F AM Am AP Ap BE Be E emission spectrum EA e sub alpha EV variable emission in spectrum FG F-G KM K-M OF Of PD Pd T characteristics of T Tauri stars Note on Ref2: The coding for the numbers is similar to that used in the variability references described above, except that there are no letter codes. These are references to papers containing identification charts if no charts are given in the papers cited for the variability references. Note on VarName: 1) The alternative name of the variable. All necessary information on the star is to be found under that alternative name, in the gcvs.dat file. 2) The star's name in the GCVS Vol. V (see the file v.zip, where the explanation of the designations is also given). In this case, the symbol "*" in column 89 means the presence of remarks in Vol. V. ------------------------------------------------------------------------------ Acknowledgement: The ADC thanks Drs. Samus and Durlevich for providing us with the up-to-date, machine-readable version of the GCVS and the Name Lists. This ReadMe is based on the one prepared by them and the four *.txt. History of the Machine-Readable Catalogs: This catalogue gathers the files previously numbered <II/139> (GCVS4, vols I-III), <II/172> (GCVS4, vol, IV), <II/205> (GCVS4, vol. V), <II/140> (New Suspected Variables), and <II/195> (Name-Lists). Catalogues <II/139> and <II/140> were first documented by Warren (1988, 1989); the documentation for the catalogues <II/172> and <II/205> was prepared by N.N. Samus and O.V. Durlevich (Moscow), with F. Ochsenbein (CDS). The first version of this Combined Catalogue (September 1997) was prepared by N. Roman (ADC) with the help of N.N. Samus and O.V. Durlevich (Moscow). The second version of this Combined Catalogue (August 1998), which incorporates the 73rd Name-List of Variable Stars and improved equatorial positions in Andromeda, Antlia and Apus, was prepared by N.N. Samus and O.V. Durlevich. Files were slightly reformatted at CDS (F. Ochsenbein) to have searchable epochs. The version 1.2 of the file "crossid.dat" was included on 22 May 1999. A further correction (QW Nor = NSV 7374 instead of NSV 7334) was applied on 16-Jun-1999 at CDS (message from N.N. Samus to F. Ochsenbein) Acknowledgements in original documents: The computer-readable version of the Name-List files has been compiled by O.V. Durlevich, N.A.Gorynya, E.V.Kazarovets, and N.N. Samus, with the assistance of E.N.Pastukhova. We wish to thank O.Yu.Malkov for his kind consultations during the preparation of the first computer-readable version of Name-Lists. Thanks are due to S.V. Antipin for his assistance during GSC identifications and positional determinations. The crossid.dat was supported in part by the Russian Foundation for Basic Research (grant 95-02-05189) and by the Federal Program 'Astronomy' (grant 93-3-182). The authors gratefully acknowledge the financial support of the work on variable star catalogues by the International Astronomical Union until 1994. The final stage of the work on evs*.dat and sn*.dat was also supported by the European Southern Observatory (grant ESO C&EE A-02-047). The variable star studies were also sponsored through a grant of the Russian Federation programme "Astronomy". The authors are grateful to the American Association of Variable Star Observers who provided a grant for us in 1994. The printing of the book version was supported by the Russian Foundation for Basic Research. The Sternberg Institute part of the author team is grateful for the grant supplied through the program "Universities of Russia" in 1993. They wish to thank all astronomers who sent us their results prior to publication, gave us good advice, helped practically or with ideas. We would like to thank specially Drs. S.V. Antipin, V.P. Arkhipova, M. Bessell, Yu.N. Efremov, M.P. Galkina, Sh. Hughes, K.V. Kuimov, V.G. Kurt, T. Lloyd Evans, C. Lopez, R.I. Noskova, A.S. Sharov, Yu.A. Shokin, D.Yu. Tsvetkov, A.V. Zharov, A.V. Zharova. Authors' addresses: N.N. Samus [Moscow Inst. Astron.] O.V. Durlevich [Sternberg Astron. Inst., Moscow] <gcvs@sai.msu.su> References: Aitken, R. G. 1932, "New General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington Pub. 417 (Washington, D.C.: Carnegie Institution of Washington). Argelander, F. 1859-62, "Bonner Sternverzeichnis. Erste bis dritte Sektion", Astronomischen Beobachtungen auf der Sternwarte der Koeniglichen Rhein. (Cat. <I/122>) Artiukhina N.M., Durlevich O.V., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kholopov P.N., Kireeva N.N., Kurochkin N.E., Lipunova N.A., Medvedeva G.I., Pastukhova E.N., Samus N.N., Tsvetkova T.M., 1995, General Catalogue of Variable Stars, 4rd ed., vol.V. Extragalactic Variable Stars, "Kosmosinform", Moscow Cannon, A. J. and Pickering, E. C. 1918-1924, "The Henry Draper Catalogue", Ann. Astron. Obs. Harvard College 91-99. (Cat. <III/135>) Dreyer, J. L. E. 1888, "New General Catalogue of Nebulae and Clusters of Stars", Mem. Roy. Astron. Soc. 49, Part I (reprinted 1962, London: Royal Astronomical Society) (see Cat. <VII/1>) Durlevich O.V., Frolov M.S., Kazarovets E.V., Samus N.N, 1996, Bull. Inf. CDS 48, 35 Durlevich O.V., Frolov M.S., Kazarovets E.V., Samus N.N., 1994, The list of errors in the GCVS, 4th edition. I. Volumes I-III, Bull. Inf. CDS, 45, 19 Gill, D. and Kapteyn, J. C. 1895-1900, "Cape Photographic Durchmusterung, Ann. Cape Obs." 3 (1895, Part I: zones -18 to -37); 4 (1897, Part II: zones -38 to -52); 5 (1900, Part III: zones -53 to -89; Cat. <I/108>). Hoffleit, D. (with the collaboration of Jaschek, C.) 1982, "The Bright Star Catalogue" (New Haven: Yale University Observatory; see Cat. <V/50>). Kazarovets E.V., Samus N.N., Goranskij V.P., 1993IBVS.3840....1K Kazarovets E.V., Samus N.N., 1995IBVS.4140....1K Kholopov P.N., Samus N.N., Durlevich O.V., Kazarovets E.V., Kireeva N.N., Tsvetkova T.M., 1990, General Catalogue of Variable Stars, 4rd ed., vol.IV(Moscow, Nauka Publishing House, Cat. <II/205>) Kholopov P.N., Samus N.N., Durlevich O.V., Kazarovets E.V., Kireeva N.N., Tsvetkova T.M., 1992, Bull. Inf. CDS, 40, 15. Kholopov P.N., Samus N.N., Frolov M.S., Goranskij V.P., Gorynya N.A., Karitskaya E.A., Kazarovets E.V., Kireeva N.N., Kukarkina N.P., Kurochkin N.E., Medvedeva G.I., Pastukhova E.N., Perova N.B., Rastorguev A.S., Shugarov S.Yu., 1985 -- 1988, General Catalogue of Variable Stars, 4rd ed., vols. I -- III, Nauka, Moscow; Cat. <II/139>. Kuestner, F. 1903, "Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage", Bonn Universitats Sternwarte. (Cat. <I/122>) 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., and Shugarov S.Yu. 1982, Moscow: Nauka Publishing House Office. (Cat. <II/140>) Kukarkin, B. V., Kholopov, P. N., Efremov, Yu. N., and Kurochkin, N. E. 1965, "Second Catalogue of Stars Suspected of Variability" (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). Kukarkin, B. V., Parenago, P. P., Efremov, Yu. N., and Kholopov, P. N. 1951, "Catalogue of Stars Suspected of Variability" (Moscow: Publishing House of the Academy of Sciences of the U.S.S.R.). Neugebauer, G. and Leighton, R. B. 1969, "Two-Micron Sky Survey, A Preliminary Catalog", NASA SP-3047 (Washington, D.C.: National Aeronautics and Space Administration; cat. <II/2>). Parenago, P. P. 1954, Trudy Sternberg Astron. Inst. No. 25. Prager, R. 1934, Ergaenz. Astron. Nachr. 9, No. 3. Prager, R. 1937, Ergaenz. Astron. Nachr. 10, No. 1. Schoenfeld, E. 1886, "Bonner Sternverzeichniss" , Vierte Sektion, Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitat zu Bonn 8, Part IV (Bonn: Adolph Marcus; cat. <I/119>). Smithsonian Astrophysical Observatory Staff 1966, "Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0", Publ. of the Smithsonian Institution of Washington, D.C., No. 4652 (Washington: Smithsonian Institution); see cat. <I/131> Sulentic, J. W. and Tifft, W. G. 1973, "The Revised New General Catalogue of Nonstellar Astronomical Objects" (Tucson: The University of Arizona Press); cat. <VII/1>. Thome, J. M. 1892-1932, "Cordoba Durchmusterung, Resultados del Observatorio Nacional Argentino" 16 (1892, Part I: -22 to -32 Degrees), 17 (1894, Part II: -32 to -42 Degrees), 18 (1900, Part III: -42 to -52 Degrees), 21 (Part I) (1914, Part IV, -52 to -62 Degrees), 21 (Part II) (1932, Part V: -61 to -90 Degrees); cat. <I/114>. Warren, W.H., Jr. 1988, "New Catalogue of Suspected Variable Stars", Documentation for the Machine-Readable Version, NSSDC/WDC-A-R&S 88-24. Warren, W.H., Jr. 1989, "General Catalogue of Variable Stars", 4th edition, Documentation for the Machine-Readable Version, NSSDC/WDC-A-R&S 88-23 Zinner, E. 1929, Ergaenz. Astron. Nachr. 8, No. 1. ================================================================================ (End) N.N. Samus, O.V. Durlevich [Moscow Inst.], F. Ochsenbein [CDS] 21-Apr-1999 II/219 New Catalogue of Suspected Variable Stars Supplement (Kazarovets+ 1998) ================================================================================ 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 (1988)> =1998IBVS.4655....1K ================================================================================ ADC_Keywords: Stars, variable; Description: This catalog is a compilation of 11206 stars suspected of variability and not finally designated as variables prior to 1997. It is the supplementary part to the "New Catalogue of Suspected Variable Stars" published in 1982 (Kukarkin et al., file "nsv.dat" included here). Data contained in the present catalog include positions, magnitudes, variability types, references to the literature, spectra and cross-identifications. The computer version of the NSV Supplement contains principally the same data as the printed catalog, the data tables with the textual material (bibliography, remarks) are included. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file nsvs.dat 114 11206 The NSV Supplement Catalog ident.dat 99 39175 Identifications remark.dat 80 6195 Remarks refs.dat 80 2784 References nsv.dat 89 14811 *New Suspected Variables (Kukarkin et al. 1982) -------------------------------------------------------------------------------- Note on nsv.dat: NSV 7334 was corrected in June 1999 (see "History" section below) See also: II/214 : The combined GCVS4.1 (Kholopov+, 1998) ftp://ftp.sai.msu.su, /pub/groups/cluster/gcvs/gcvs/nsvsup/ : (anonymous) http://www.sai.msu.su/groups/cluster/gcvs/gcvs/ : GCVS pages Byte-by-byte Description of file: nsvs.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- NSV [15001/26206]+ NSV number 6 A1 --- RemFlag *[*] indicates a remark in file remark.dat 8- 9 I2 h RAh Hours RA, equinox 1950.0 10- 11 I2 min RAm Minutes RA, equinox 1950.0 12- 15 F4.1 s RAs Seconds RA, equinox 1950.0 16 A1 --- DE- Sign Dec, equinox 1950.0 17- 18 I2 deg DEd Degrees Dec, equinox 1950.0 19- 20 I2 arcmin DEm Minutes Dec, equinox 1950.0 21- 22 I2 arcsec DEs Seconds Dec, equinox 1950.0 23 A1 --- u_DEs *[:*] accuracy flags 25- 26 I2 h RA2000h Hours RA, equinox 2000.0 27- 28 I2 min RA2000m Minutes RA, equinox 2000.0 29- 32 F4.1 s RA2000s Seconds RA, equinox 2000.0 33 A1 --- DE2000- Sign Dec, equinox 2000.0 34- 35 I2 deg DE2000d Degrees Dec, equinox 2000.0 36- 37 I2 arcmin DE2000m Minutes Dec, equinox 2000.0 38- 39 I2 arcsec DE2000s Seconds Dec, equinox 2000.0 41- 46 A6 --- VarType *Type of variability 48 A1 --- l_magMax [><] "<" if magMax is a bright limit, ">" if magMax is a faint limit, 49- 53 F5.2 mag magMax *? Magnitude at maximum brightness 54 A1 --- u_magMax [:]Uncertainty flag on magMax 56- 57 A2 --- l_magMin [><( ] "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit 58- 63 F6.3 mag magMin *? Minimum magnitude or amplitude 64 A1 --- n_magMin *The photometric system for amplitudes 65 A1 --- f_magMin [)] ")" if magMin is an amplitude 66 A1 --- u_magMin Uncertainty flag (:) on magMin or amplitude 68- 69 A2 --- magCode *The photometric system for magnitudes and amplitudes 71- 74 A4 --- r_NSV *Reference to a study of the star (see file refs.dat) 76- 79 A4 --- Ref2 *Chart reference (see file refs.dat) 81- 95 A15 --- SpType1 *Spectral type 97-104 A8 --- SpType2 Spectral type from HD catalog in brackets 106-114 A9 --- VarName *Designation in GCVS --------------------------------------------------------------------------- Note on RemFlag: There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are machine readable, they do contain much supplemental information. There, one will find information covering situations like, 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 catalogued 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 semimajor 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 machine-readable table.) Note on u_DEs: The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. Note on magMax, magMin: The star's magnitude in minimum and maximum brightness. Instead of the magnitude in minimum, the star's amplitude of variation may be indicated (in brackets). 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. Note on n_magMin and magCode: The photometric system in which magMin and magMax are reported. The main codes are V (visual, photovisual, or Johnson's V), B (Johnson's B) and P (photographic magnitudes). The designations u, v, b, y refer to the Stroemgren system. The symbols Ic, Rc mean magnitudes in Cousins' I, R system; Hp, T - in Hipparcos and Tycho mission systems; J, H, K, L, M - infrared magnitudes. Note on VarType: Type of variability. The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67-72 and in the GCVS vol.V. Brief descriptions only are given here: ACV, ACVO Alpha2 Canum Venaticorum ACYG Alpha Cygni BCEP, BCEPS Beta Cephei BE Be BL BL Lacertae BY BY Draconis CEP Cepheid CST constant CW W Virginis DCEP Delta Cephei DSCT, DSCTC Delta Scuti E eclipsing EA Algol (Beta Persei) EB Beta Lyrae EW W Ursae Majoris ELL ellipsoidal FKCOM FK Comae Berenices FU FU Orionis GAL galaxy GCAS Gamma Cassiopejae I irregular IA, INA white irregular IB, INB red irregular IN irregular in a nebula IT, INT irregular of the T Tauri type IS, ISA rapid irregular L slow LB slow red LBV long-period pulsating B star M Mira (Omicron Ceti) type N Nova NL nova-like NR recurrent Nova QSO quasistellar object RR RR Lyrae RS RS Canum Venaticorum RV RV Tauri S rapid SN supernova SR, SRA, SRB, SRD semiregular SXARI SX Arietis SXPHE SX Phoenicis UG U Geminorum UGSS SS Cygni UV UV Ceti VAR variable WR Wolf-Rayet star XM X-ray system with a strong magnetic field XNA X-ray nova-like ZAND Z Camelopardalis ZZA, ZZO ZZ Ceti Note on r_NSV: The four digits give the number in the list of references contained in the catalog, which is generally the first publication announcing the possible variability. Note on Ref2: The coding for the numbers is similar to that used in the variability references described above, except that there are also letter codes. These are references to papers containing identification chart or photograph of the field with the suspected variable marked. If the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (BD,CD,CPD) or in the Hubble Space Telescop Guide Star Catalog (GSC), then corresponding letter codes DM or GSC are given. Note on SpType1: Spectral types, subtypes and luminosity classes are given. More detailed classification information is given in the remarks to the catalog. Also the following symbols are used: AF A-F cont continuum e emission spectrum ea e sub alpha FG F-G KM K-M * see Sp type in remarks Note on VarName: The alternative name of the variable. All necessary information on the star is to be found under that alternative name in Cat. <II/214> (file gcvs.dat) -------------------------------------------------------------------------------- Byte-by-byte Description of file: ident.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- NSV [15001/26206]+= NSV number 7 A1 --- --- [=] Equality sign 9- 99 A91 --- ID *Identifications -------------------------------------------------------------------------------- Note on ID: all identifications needed to find the star in the papers with the first (or independent) announcement of the discovery of its variability. References to these papers (see file refs.dat) are given in square brackets after the corresponding identification. The name of the discoverer accompanies the reference only in the case of its being different from the name of the author(s) of the paper referred to. Designations of components of double or multiple system: A, B, C, ..., A1, A2, ..., p - preceding, f - following, s - southern, n - northern. The transliterations of greek letters are used: alpha, beta, gamma,..., omega, etc., kappa 2, omicr 1. Different identifications of the same star with catalogs and lists are separated with equality sings (=). Symbol (?) marks the doubtful identification. The following catalogs abbreviations are used (abbreviated names for some of them are presented): Bayer - Greek and Roman letters in the Bayer Atlas, Flamsteed - Baily, F. 1835, "Association of J.Flamsteed, British Catalogue of Stars". BS (HR) - Hoffleit, D. (with the collaboration of Jaschek, C.) 1982, "The Bright Stars Catalogue" (New Haven: Yale University Observatory) (HR numbers are adopted from Pickering, E. C., 1908, "Harvard Revised Photometry", Ann. Astron. Obs. Harvard College 50). (See Cat. <V/50>) HD - Cannon, A. J. and Pickering, E. C. 1918-1924, "The Henry Draper Catalogue", Ann. Astron. Obs. Harvard College 91-99. (See Cat. <III/135>) BD - Argelander, F. 1859-62, "Bonner Sternverzeichniss. Erste bis dritte Sektion", Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rhein. Friedrich-Wilhelms-Universitaet zu Bonn, Bande 3-5. Revision of Argelander's first edition: Schoenfeld, E. 1886, "Bonner Sternverzeichniss", Vierte Sektion, Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitaet zu Bonn 8, Part IV (Bonn: Adolph Marcus); Kuestner, F. 1903, "Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage", Bonn Universitaets-Sternwarte. (See Cats <I/122> and <I/119>) CoD - Thome, J. M. 1892-1932, "Cordoba Durchmusterung, Resultados del Observatorio Nacional Argentino" 16 (1892, Part I: -22 to -32 Degrees), 17 (1894, Part II: -32 to -42 Degrees), 18 (1900, Part III: -42 to -52 Degrees), 21 (Part I) (1914, Part IV, -52 to -62 Degrees), 21 (Part II) (1932, Part V: -61 to -90 Degrees). (See Cat. <I/114>) CPD - Gill, D. and Kapteyn, J. C. 1895-1900, "Cape Photographic Durchmusterung", Ann. Cape Obs. 3 (1895, Part I: zones -18 to -37); 4 (1897, Part II: zones -38 to -52); 5 (1900, Part III: zones -53 to -89). (See Cat. <I/108>) GSC - Lasker, B. M., et al. 1990, "The Guide Star Catalog. I. Astronomical Foundations and Image Processing", A. J. 99, 2019; The Space Telescope Science Institute 1992, "The Guide Star Catalog Version 1.1 (An all-sky astrometric and photometric catalog to support the operation of the Hubble Space Telescope)" on two CD-ROMs. (See Cat. <I/220>) HIP - European Space Agency 1997, "The Hipparcos and Tycho Catalogues", SP-1200, Vols. 1-17. (See Cat. <I/239>) SAO - Smithsonian Astrophysical Observatory Staff 1966, "Star Catalog. Positions and Proper Motions of 258,997 Stars for the Epoch and Equinox of 1950.0", Publ. of the Smithsonian Institution of Washington, D.C., No. 4652. (See Cat. <I/131>) ADS - Aitken, R. G. 1932, "New General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington, Publ. no. 417 (Washington, D.C.: Carnegie Institution of Washington). IDS - Jefers, H. M., Van den Bos, W. H., Greeby, F. M. 1963, "Index Catalogue of Visual Double Stars", Publ. Lick Obs. 21. BDS - Burnham, S. W. 1906, "A General Catalogue of Double Stars within 120 Degrees of the North Pole", Carnegie Institution of Washington, Publ. No. 5 (Washington, D.C.: Carnegie Institution of Washington). CCDM - Dommanget, J., Nys, O. 1994, "The Catalogue of Components of Double and Multiple Stars", Comm. Obs. R. de Belg., Serie A No.115 (catalog CDS <I/211>). IRC - Neugebauer, G. and Leighton, R. B. 1969, "Two-Micron Sky Survey, A Preliminary Catalog", NASA SP-3047 (Washington, D.C.: National Aeronautics and Space Adminstration). (See Cat. <II/2>) AFGL/RAFGL - Walker, R. G., Price, S. D. 1975, "Air Force Cambridge Research Laboratory Infrared Sky Survey", U.S. Air Force Report No. AFCRL-TR-0373; Price, S. D., Walker, R. G. 1976 "The AFGL Four Color Infrared Sky Survey", AFGL-TR-0208, and 1977 "The AFGL Four Color Infrared Sky Survey Supplement", AFGL-TR-0160. IRAS - The Joint IRAS Science Working Group 1988, "Infrared Astronomical Satellite (IRAS) catalogs and atlases" 2-6, NASA RP-1190 (Washington, D.C.: National Aeronautics and Space Adminstration). (See Cat. <II/125>) MWC - Merrill, P. W., Sunford, R. F., Burwell, C. G. 1933-1949, "Mount Wilson Catalogue of stars of classes B and A whose spectra have bright hydrogen lines", P.A.S.P. 45, 306; P.A.S.P 54, 107; Ap. J. 78, 87; Ap. J. 98, 153; Ap. J. 110, 387. AS - Merrill, P. W., Burwell, C. G. 1950, "Additional stars whose spectra have a bright H Alpha line", Ap. J. 112, 72. LkHa - Herbig, G. H., et al. 1954-1974, Lists of emission-line stars. MHa - Mount Wilson H Alpha-emission line stars, see references for MWC and AS. He-3 - Henize, K. G. 1976, "Observations of Southern Emission-Line Stars", Ap. J. Suppl. 30, 491. HRC/HBC - Herbig, G. H., Robbin Bell, K. 1988, "Third Catalog of Emission-Line Stars of the Orion Population", Lick Obs. Bull No.1111. Wray - Wray, J. D. 1966, "A study of H Alpha-emission objects in the Southern Milky Way", Table XV-XIX, Univ. Microfilm Inc., Ann Arbor, Michigan. LS - Hardorp, J., et al. 1959-1971, "Luminous Stars in the Northern Milky Way" I-VI, Hamburger Sternwarte - Warner and Swasey Obs., Hamburg-Bergedorf. (See Cat. <III/76>) LSS - Stephenson, C. B., Sanduleak, N. 1971, "Luminous Stars in the Southern Milky Way", Publ. Warner and Swasey Obs. 1, No.1. (See Cat. <III/43>) CCS - Stephenson, C. B. 1973, "A General Catalogue of Cool Carbon Stars", Publ. Warner and Swasey Obs. 1, No.4. (See Cat. <III/156>) Hen - Unpublished list of C-stars by K.G.Henize (given in CCS), CSS - Stephenson, C. B. 1976, "A General Catalogue of S Stars", Publ. Warner and Swasey Obs. 2, No.2. (See Cat. <III/60>) WR - Van der Hucht, K. A., et al. 1981, "The Sixth Catalogue of Galactic Wolf-Rayer Stars", Space Sci. Rev. 28, 227. PG - Green, R. F., et al. 1986, "Cataclysmic Variable Candidates from the Palomar Green Survey", Ap. J. Suppl. 61, 305. (See Cat. <II/207>) WD - McCook, G. P., Sion, E. M. 1987, "A Catalogue of Spectroscopically Identified White Dwarfs", Ap. J. Suppl. 65, 603. (See Cat. <III/129>) G - Giclas, H. L., et al. 1971-1979, "Lowell Proper Motion Survey" (red dwarfs), Lowell Obs. Bull., Flagstaff, Arizona. GD - Giclas, H. L., et al. 1980, "Lowell Proper Motion Survey" (white dwarfs), Lowell Obs. Bull. 8, 157. Eg/Gr - Eggen, O. J., Greenstein, J. L. 1965-1977, "Spectra, Colors, Luminosities and Motions of the White Dwarfs", Ap. J. 141, 83; Ap. J. 142, 925; Ap. J. 150, 927; Ap. J. 158, 281; Ap. J. 162, L55; Ap. J. 189, L131; Ap. J. 196, L117; Ap. J. 207, L119; Ap. J. 218, L21. Gliese - Gliese, W. 1969, "Catalogue of Nearby Stars", Veroeff. Astron. Rechen-Inst. Heidelberg Nr.22; Gliese, W., Jahreiss, H. 1979, "Nearby star data published 1969-1978", Astron. Astrophys. Suppl. 38, 423. (See Cat. <V/70>) He-2 - Henize, K. J. 1964, An extended list of southern planetary nebulae; see PK Nomenclature. PK - Perek, L., Kohoutek, L. 1967, "Catalogue of Galactic Planetary Nebulae", Academia Publishing House of the Czechoslovak Academy of Sciences. NGC - Dreyer, J. L. E. 1888, "New General Catalogue of Nebulae and Clusters of Stars", Mem. Roy. Astron. Soc. 49, Part I (reprinted 1962, London: Royal Astronomical Society); Sulentic, J. W. and Tifft, W. G. 1973, "The Revised New General Catalogue of Nonstellar Astronomical Objects" (Tucson: The University of Arizona Press). (See Cat. <VII/118>) LHS - Luyten, W. J. 1976, "A Catalog of Stars with Proper Motion exceeding 0".5 annually", Publ. of Univ. of Minnesota, Minneapolis, Minnesota; Luyten, W. J., Albers, H. 1979, "An Atlas of Identification Chart for LHS Stars", Publ. of Univ. of Minnesota, Minneapolis, Minnesota. (See Cat. <I/87>) LTT - Luyten, W. J. 1957, "Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motion exceeding 0".2 annually"; Luyten, W. J. 1961, "Catalogue of 7127 Stars in the Northern Hemisphere with Proper Motion exceeding 0".2 annually", The Lund Press, Minneapolis, Minnesota. LFT - Luyten, W. J. 1955, "A Catalog of 1849 Stars with Proper Motion exceeding 0.5" annually", The Lund Press, Minneapolis, Minnesota. L - Luyten, W. J. 1941, "Proper Motion Survey with the fourty-eight inch Schmidt Telescope", XXI, XXV, XXIX, Publ. of Univ. of Minnesota. LP - Luyten, W. J. 1963-1981, "Proper Motion Survey with the 48 inch Schmidt Telescope", Publ. of Univ. of Minnesota, Minneapolis, fasc. 1-57. LDS - Luyten, W. J. 1943, "Catalogue of 832 Double Stars with Common Proper Motion in the Southern Hemisphere", Publ. Astron. Obs. Univ. Minnesota 3, No. 3, 33. BPM - Luyten, W. J. 1963, "Bruce Proper Motion Survey. The general catalogue. Vol. I, II", Publ. of Univ. of Minnesota, Minneapolis, Minnesota. Ross - Ross, F. E. 1925-1939, "New Proper Motion Stars", eleven successive lists, A. J. Vol. 36 to 48. Vys - Vyssotsky, A. N., et al. 1943-1958, "Dwarf M Stars Found Spectrophotometrically", A. J. 61, 201; A. J. 63, 211; Ap. J. 97, 381; Ap. J. 104, 234; Ap. J. 116, 117. Wolf - Wolf, M. 1919, "Katalog von 1053 starken bewegten Fixsternen", Veroeff. Sternwarte zu Heidelberg 7, No. 10, 195; and numerous lists in Astron. Nachr. 209 to 236, 1919 to 1929. OH - OH sources designated by their galactic co-ordinates. HII - Hertzsprung, E. 1947, "Catalogue de 3259 Etoiles dans les Pleiades", Ann. Sterrewacht Leiden 19, part 1A. Par - Parenago, P. P. 1954, "A List of Star in the Region of the Orion Nebula", Trudy Sternberg Astron. Inst. Vol. 25. HV - Preliminary designations of variables discovered at Harvard Observatory. S - Preliminary designations of variables discovered at Sonneberg Observatory. SVS - Soviet variable stars (preliminary designations of Soviet-discovered variables). VV - Preliminary designations of variables discovered at Vatican. VES - Lists of the Vatican H Alpha-emission line stars. -------------------------------------------------------------------------------- Byte-by-byte Description of file: remark.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- NSV [15001/26206]+= NSV number 7- 80 A74 --- Text *Text of remark -------------------------------------------------------------------------------- Note on Text: See Note on RemFlag (nsvs.dat) and Note on ID (ident.dat). -------------------------------------------------------------------------------- Byte-by-byte Description of file: refs.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Ref [1,2022]+= Reference number 6- 80 A75 --- Text *Text of reference -------------------------------------------------------------------------------- Note on Text: We attempted to give Latin transliterations of Russan-language names of astronomical periodicals and books. We did not try to unify the Latin spelling of names with Cyrillic (or other) original forms, but simply tried to reproduce the Latin transcriptions in the publications referred to. When several lines are needed, the reference number is repeated. The "bibcode", if known, is added at the beginning of the text. -------------------------------------------------------------------------------- Byte-by-byte Description of file: nsv.dat ------------------------------------------------------------------------------ Bytes Format Units Label Explanations ------------------------------------------------------------------------------ 1- 5 I5 --- NSV [1,14811]+= NSV number 6 A1 --- m_NSV *NSV letter suffix 7 A1 --- u_NSV [-]Dubitancy flag if a star's variability seems doubtful or erroneous to the catalog compilers 8 A1 --- NoteFlag1 *[*] Notes in published catalog 9- 10 I2 h RAh *? Hours RA, equinox 1950.0 11- 12 I2 min RAm *? Minutes RA, equinox 1950.0 13- 16 F4.1 s RAs *? Seconds RA, equinox 1950.0 17 A1 --- DE- *? Sign Dec, equinox 1950.0 18- 19 I2 deg DEd *? Degrees Dec, equinox 1950.0 20- 21 I2 arcmin DEm *? Minutes Dec, equinox 1950.0 22- 23 I2 arcsec DEs *? Seconds Dec, equinox 1950.0 24 A1 --- u_DEs *[:*] accuracy flags 25- 29 A5 --- VarType *Type of variability 31- 35 F5.2 mag magMax *? Magnitude at maximum brightness 36 A1 --- u_magMax [:] Uncertainty flag on magMax 38- 39 A2 --- l_magMin [><( ] "<" if magMin is a bright limit "(" if magMin is an amplitude; with "><" prefix, the amplitude in the table is a lower or upper limit. 40- 45 F6.3 mag magMin *? Minimum magnitude or amplitude 46- 47 A2 --- u_magMin [st:] a light amplitude is reported for the minimum and it is given in steps Uncertainty flag (:) on magMin 48 A1 --- f_magMin [)] ")" if magMin is an amplitude 49 A1 --- magCode *The photometric system for magnitudes 51-57 A7 --- Ref1 *Reference to a study of the star see the document by Kukarkin et al.(1982) 59-67 A9 --- Desig *Designation in paper Ref1 69-70 A2 --- SpType *Spectral type 72-77 A6 --- Ref2 *Chart reference see the document by Kukarkin et al.(1982) 79-88 A10 --- VarName *Designation in GCVS 89 A1 --- NoteFlag2 *[*] Notes in catalog GCVS Vol.V ------------------------------------------------------------------------------- Note on m_NSV: The letter "A" is present for one star, NSV 10360A, which is a completely different object from NSV 10360. Note on NoteFlag1: see the document by Kukarkin et al.(1982) There are several data fields that can contain asterisks. These signify that more complete information will be found in the remarks to the published catalog. The remarks are, unfortunately, not machine readable, but they do contain much supplemental information. There, one will find information covering situations like, 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 compilers did not intend to present complete bibliographies for any catalogued stars. 3. Remarks for visual binaries (in parentheses following the number of a star in the corresponding catalog) giving visual magnitudes for the individual components A and B, angular separations, and position angles for faint components (or semimajor axis of a relative orbit and period of orbital motion). Data for other components are then given where applicable. (Combined magnitudes are generally reported in the machine-readable table.) Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs: The position is also listed when the variable is equivalent to a GCVS star (column VarName). Note on u_DEs: The actual accuracy of coordinates is indicated with the symbols: (:) means right ascensions accurate to one second of time and declinations accurate to one tenth of an arcminute; (*) means declinations accurate to one arcminute. Note on VarType: type of variability (see file ...\III\vartype.txt). The system of variable star classification corresponds to the GCVS4, with six additions (ZZO, AM, R, BE, LBV, BLBOO) introduced in the Name-Lists 67- 72 and in the GCVS vol.V. (see "Note on VarType" section above) Note on magMax, magMin: Magnitudes are reported to hundredths if the observations are photoelectric, 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. Note on magCode: the photometric system in which magMin and magMax are reported (see also Note on n_magMax, n_magMin). The main codes are P (photographic magnitudes) and V (visual, photovisual, or Johnson's V). See also the documents by Kholopov et al. (1985-1988) or Warren (1988). Note on Ref1: Usually a 6-digit number coding, as a rule, the reference to the announcement of the discovery of variability. The first two digits give the year (in the 20th century) when the announcement was published (blank for the 19th century). The next four digits give the number in the list of references contained in the published catalog, which is generally the first publication announcing the possible variability. The numbers are followed by a letter code in most cases (byte 75) with the following meanings: K: the cited paper contains a chart or photograph of the field with the suspected variable marked. D: the cited paper does not contain a chart, but the star is catalogued in one of the Durchmusterungen (DM) (BD,CD,CPD). Note on Desig: The identification of the suspected variable in the paper referenced above. DM numbers are given without a prefix, the standard naming convention of "The Henry Draper Catalogue" being used (BD for zones +89 to -22; CD for -23 to -51; CP for -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. An asterisk (*) signifies that a designation is given in the remarks to the published catalog. Stars are sometimes designated with numbers from the catalogs of Zinner (ZI, 1929) and Prager (PR, 1934, 1937) because the original discovery publications were not available to the NSV compilers. The catalogs of Zinner and Prager give detailed references to early observations of such stars. Note on SpType: Spectral types and subtypes only are given. Most luminosity classes are III to V, but if a star is a supergiant, more detailed classification information is given in the remarks to the published catalog. The following symbols are used: AF A-F AM Am AP Ap BE Be E emission spectrum EA e sub alpha EV variable emission in spectrum FG F-G KM K-M OF Of PD Pd T characteristics of T Tauri stars Note on Ref2: The coding for the numbers is similar to that used in the variability references described above, except that there are no letter codes. These are references to papers containing identification charts if no charts are given in the papers cited for the variability references. Note on VarName, NoteFlag2: 1) The alternative name of the variable. All necessary information on the star is to be found under that alternative name, in the iii.zip and nl.zip files. 2) The star's name in the GCVS Vol. V (see the file v.zip, where the explanation of the designations is also given). In this case, the symbol "*" in column 89 means the presence of remarks in Vol. V. -------------------------------------------------------------------------------- History: * 16-Jun-1999: in file nsv.dat, the star NSV 7334 = HV 10762 which was erroneously cross-identified with QW Nor, was corrected at CDS (the original data of the 1982 version of the NSV catalogue were inserted for this star) QW Nor is identical to NSV 7374. References: Kholopov, P. N., Samus, N. N., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kazarovets, E. V., Kireeva, N. N., Kukarkina, N. P., Kurochkin, N. E., Medvedeva, G. I., Perova, N. B., Rastorguev, A. S., and Shugarov, S. Yu. 1985-1988, "General Catalogue of Variable Stars", 4th Edition, Volumes I-III, (Moscow: Nauka Publishing House). 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., and Shugarov, S. Yu. 1982, "New Catalogue of Suspected Variable Stars", (Moscow: Nauka Publishing House). Kholopov, P. N., Samus, N. N., Durlevich, O. V., Kazarovets, E. V., Kireeva, N. N., Tsvetkova, T. M. 1990, "General Catalogue of Variable Stars", 4th Edition, Vol. IV, (Moscow: Nauka Publishing House). Kholopov, P. N., Samus, N. N., Frolov, M. S., Goranskij, V. P., Kazarovets, E. V., Kireeva, N. N., Perova, N. B. 1985-1995, "Name-lists of variable stars Nos. 67-72". Artyukhina, N. M., Durlevich, O. V., Frolov, M. S., Goranskij, V. P., Gorynya, N. A., Karitskaya, E. A., Kazarovets, E. V., Kholopov, P. N., Kireeva, N. N., Kurochkin, N. E., Lipunova, N. A., Medvedeva, G. I., Pastukhova, E. N., Samus, N. N., Tsvetkova, T. M. 1995, "General Catalogue of Variable Stars", 4th Edition, Vol. V: Extragalactic Variable Stars (Moscow: "Kosmosinform"). ================================================================================ (End) E.V. Kazarovets, O.V. Durlevich [Moscow & Sternberg] 10-May-1999