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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
-