THE 75th NAME-LIST OF VARIABLE STARS. E.V. Kazarovets *, N.N. Samus *, O.V. Durlevich **. * Institute of Astronomy, Russian Academy of Sciences, 48, Pyatnitskaya Str., Moscow 109017, Russia [samus@sai.msu.ru,elena_k@sai.msu.ru] ** Sternberg Astronomical Institute, University of Moscow, 13, University Ave., Moscow 119899, Russia [gcvs@sai.msu.ru]. IBVS 4870, 31 March 2000 ___________________________________________________________________________ We present the next regular Name-List of variable stars containing information on 916 variable stars recently designated in the system of the General Catalogue of Variable Stars. Key: variable stars; catalogues The present 75th Name-List of Variable Stars, compiled basically in the manner first introduced in the 67th Name-List (IBVS No. 2681, 1985), contains all data necessary for identification of 916 new variables finally designated in 1999. The total number of designated variable stars, not counting designated non-existing stars or stars subsequently identified with earlier-designated variables, has now reached 35985. The 75th Name-List consists of two tables. Table 1 contains the list of new variables arranged in the order of their right ascensions. It gives the ordinal number and the designation of each variable; its equatorial coordinates for the equinox 1950.0 (we present right ascensions to 0.1 sec and declinations to 1". The coordinates were found in the literature, taken from positional catalogues, including USNO A1.0/A2.0 and GSC, or determined by the authors); the range of variability (sometimes the column "Min" gives, in parentheses, the amplitude of light variation; the symbol "(" means that the star, in minimum light, becomes fainter, than the magnitude indicated); and the system of magnitudes used ("P" are photographic magnitudes the symbols "Rc", "Ic" designate magnitudes in Cousins's RI system; the symbols "b", "v" mean Stroemgren's b, v magnitudes; "Hp" stands for magnitudes in the system of the Hipparcos catalog; "L'" are infrared magnitudes at 3.8 mkm; the rest of designations are standard Johnson UBVRIJKLM magnitudes); the type of variability according to the classification system described in the forewords to the first three volumes of the 4th GCVS edition (with the additions introduced in the 68th Name-List, IBVS No. 3058, 1987, in the 69th Name-List, IBVS No.3323, 1989, and in the 72nd Name-List, IBVS No.4140, and two additions described below; see also the description of variability types and distribution of stars over variability types at http://www.sai.msu.su/groups/cluster/gcvs/gcvs/iii/vartype.txt; two references to the list of papers which follows Table 2 (the first reference is to the investigation of the star, the second one indicates the paper containing a finding chart, or the corresponding Durchmusterung - BD, CoD, or CPD - containing the variable, or the Hubble Space Telescope Guide Star Catalog - GSC - or the USNO A1.0/A2.0 catalog - USNO - if the star can be found using one of them). In a small number of cases, the value of the variability amplitude (column "Min", in parentheses) could not be expressed in the same system of magnitudes as the star's brightness; in such cases we indicate the photometric band for the amplitude separately. For KL Dra, V1010 Her, and V370 Peg, the magnitudes in maximum brightness are from unfiltered CCD observations. In the present Name-List, we have introduced two new variability types for pulsating variables. GDOR - gamma Doradus stars. Early type F dwarfs showing (multiple) periods from several tenths of a day to slightly in excess of one day. Amplitudes usually do not exceed 0.1 mag. Presumably low degree g-mode non-radial pulsators. Prototype: gamma Dor. RPHS. Very rapidly pulsating hot (subdwarf B) stars. Typical periods are hundreds of seconds, amplitudes are within several hundredths of a magnitude. Prototype: V361 Hya = EC 14026-2647. Suggestions of a better designation for the new type are welcome. A version of Table 1 given in the electronic supplement to this paper (file 4870-t1.txt) contains also coordinates for the equinox 2000.0. In the electronic table, no spaces are left between hour and minutes, minutes and seconds of right ascension or between degrees and minutes, minutes and seconds of declination. Table 2 contains the list of variables arranged in the order of their variable star names within constellations. After the designation of a variable, its ordinal number from Table 1 is given, as well as identifications with several major catalogues and identifications necessary to find this star in the papers referred to in Table 1 or in the papers with the first (or independent) announcement of the discovery of its variability, referred to (in some cases) in square brackets after the corresponding identification in Table 2. In variance with our earlier practice, we did not include names of discoverers different from the name of the author(s) of the paper referred to. After the identifications, some minimal remarks are given if necessary. Table 2 and the list of references are also presented in the form of ASCII files in the electronic supplement to this paper (files 4870-t2.txt and 4870-t3.txt). The abbreviated names of the catalogues in Table 2 generally follow conventions of the GCVS or of the SIMBAD data base; in its electronic version, "Name" stands for non-standard names or abbreviations, mainly from discovery announcements, and "Rmrk", for remarks. The small table below contains corrected coordinates for two stars from the Name-List No.73 (IBVS No. 4471, 1997). 73283 FI UMa 11 09 50.6 +55 09 59 73684 V389 Cep 21 27 13.0 +55 45 14 Note that corrected coordinates for many GCVS variable stars and NSV catalog suspected variables can be found at our web site http://www.sai.msu.su/groups/cluster/gcvs/gcvs/ so that we recommend variable star researchers to retrieve updated versions of our catalogs from time to time. Thanks are due to M.S. Frolov and S.V. Antipin for their help during the preparation of the present Name-List and to all members of the GCVS team who prepared information for the variable star data base. We would like to thank many scientists who immediately responsed to our requests to provide missing data or correct erroneous data necessary for this Name-List. This study was supported in part by Russian Foundation for Basic Research through grant 99-02-16333, by the Russian Federal Scientific and Technological Programme "Astronomy", and by the Support Programme for Leading Scientific Schools of Russia. ======================================================================= March 2000.