COMMISSIONS 27 AND 42 OF THE IAU 
              INFORMATION BULLETIN ON VARIABLE STARS 
                           Number 3756 
 
                                           Konkoly Observatory 
                                           Budapest 
                                           10 August 1992 
 
                                           HU ISSN 0374 - 0676 
 
 
          ON SEVERAL VARIABLE STARS IN THE FIELD OF M33 
 
 Having met some difficulties in locating variables discovered by 
Romano (1978), we decided to remeasure co-ordinates of these stars. 
The measurements, carried out by V. P. Goranskij by means of an 
"ASCORECORD" machine, have led to the following results (equinox 
1950.0, epoch 1990.05, accuracy about 0".5 in both co-ordinates): 
 
                   Table I. 
 
GCVS     GR          R.A.             Decl. 
 
AI Psc   282   1h 26m 27s .78      +32d27'46".6 
AK Psc   283   1  26  39  .35      +28 56 57 .6 
AL Psc   284   1  27  37  .52      +29 43 16 .4 
AM Psc   285   1  28  02  .60      +31 23 21 .4 
TT Tri   286   1  29  11  .54      +29 33 58 .9 
TU Tri   287   1  36  24  .68      +31 09 05 .1 
TV Tri   288   1  30  20  .83      +32 20 15 .9 
TW Tri   292   1  33  46  .41      +31 45 19 .3 
         289   1  30  34  .72      +32 12 14 .4 
         291   1  32  43  .75      +31 15 29 .4 
 
 Thus, the co-ordinates published by Romano for GR 283 are wrong by 1deg
in delta, and those for GR 287 - by almost 7m in alpha. As a 
result, the discovery of a new variable, in fact identical with GR 
287, was announced by Sharov (1991). Note that the finding chart for 
TU Tri = GR 287 published by Khruzina and Shugarov (1991) is wrong, 
again because of their attempt to find the star at the published 
position. Our identification of TU Tri is quite sure, though a bright 
star in the field is missing in the chart by Romano (1978). 
 
 AL Psc = GR 284 was attributed by Romano (1978) to RR Lyrae stars; he 
indicated the range 15.3m-16.8m pg. 
 
 One of us (A. S. Sh.) has estimated the brightness of AL Psc on 273 
B plates taken with the 50 cm Maksutov camera of the Sternberg 
Institute Crimean Laboratory (J.D. 2437556-2448573). Figure 1 shows 
the finding chart with comparison stars indicated; their B magnitudes 
(a = 15.15, b = 16.05, c = 16.60, d = 17.58) rely upon the 
photoelectric standard (Sandage and Johnson,1974). 


                             [FIGURE 1]

                  Figure 1. Finding chart of AL Psc

                             [FIGURE 2]

                   Figure 2. Light curve of AL Psc

 
 We have determined the period of AL Psc using a computer program 
(Lafler-Kinman algorithm) written by S. Yu. Shugarov.  The star is 
really an RR Lyrae variable (subtype ab) with the following light 
elements: 
 
                  Max = 2448524.12 + 0.456782d x E, 
 
the period being apparently constant during the whole time interval 
covered with our observations. The range is 15.6m-17.1mB, M-m = 
0.25p. The mean light curve is shown in Figure 2. 
 
 
                     A. S. SHAROV 
                     V. P. GORANSKIJ 
                     Sternberg Astronomical Institute 
                     13, University Avenue, Moscow 119899 
                     Russia 

                     N. N. SAMUS 
                     Institute for Astronomy 
                     of Russian Academy of Science 
                     48, Pyatnitskaya Str., Moscow 109017 
                     Russia 
 
 
 
References: 
 
Khruzina, T. S., Shugarov, S. Yu.: 1991, An Atlas of Cataclysmic 
  Variables. U Gem Type Stars.  Part 2. University of Moscow Press. 
 
Romano, G.: 1978, IBVS, No. 1421. 
 
Sandage, A., Johnson, H. R.: 1974, Astrophys. J., 191, 63.  [BIBCODE 1974ApJ...191...63S ]
 
Sharov, A. S.: 1991, Astron. Tsirk., No. 1550, 16.  [BIBCODE 1991ATsir1550...16S ]

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