COMMISSIONS 27 AND 42 OF THE IAU
             INFORMATION BULLETIN ON VARIABLE STARS
                          Number 3897

                                             Konkoly Observatory
                                             Budapest
                                             14 June 1993

                                             HU ISSN 0374 - 0676


                    UBV PHOTOMETRY OF GO Cyg


The short period eclipsing binary GO Cyg (=HD 196628=BD+34d4095) was 
photoelectrically observed during July and September 1992.  The observations were
made using a 40 cm Cassegrain-telescope and a photoelectric photometer equipped
with an unrefrigerated photomultiplier tube RCA 1P21 Johnson's standard U, B, V
filters.  The phases were calculated using

           Min. I.=JD Hel 2445865.4056+0.71776707d * E

(Sezer et al., 1985).  The stars BD +35d 4180 and BD +34d 4098 were used as the
comparison and the check stars respectively.  A total of 192 individual points
were obtained in each colour.  Figures 1, 2 and 3 summarize the results for U,
B and V colours respectively.

The times of minimum light determined with Kwee and Van Woerden's method are
given in Table I.


                              [FIGURE 1]
                              [FIGURE 2]
                              [FIGURE 3]


                    Table I

JD Hel.     Filter   m.e.     rem
2448000.+
855.2584    U        0.0004   II
855.2584    B        0.0004   II
855.2584    V        0.0004   II
856.3347    B        0.0004   I
856.3345    V        0.0003   I

Few observations of GO Cyg have been published to date.  The visual
observations made by Kukarkin (1932) showed beta Lyrae type variations.
Ovenden (1954), Mannino (1963) and Sezer (1985) presented complete two colour
photometric light curves for this star.  Our present light curves show beta
Lyrae type variations with no asymmetry in the minima, no displacement in the
secondary minimum and the maxima are equal.  The depth of the primary minimum
is 0.615, 0.605, 0.600 mag and the depth of the secondary is 0.230, 0.228,
0.200 mag in U, B and V respectively.  The analysis of these light curves is
being carried out and the results will be presented in a further paper.


                          D. M. Z. JASSUR and
                          R. PULADI
                          Center for Astronomical Research
                          Khadjeh Nassir Alddin Tussi
                          Observatory
                          University of Tabriz
                          Tabriz, Iran

References:

Kukarkin, B. W., 1932, N. N. V. S., 4, 19
Mannino, G., 1953, Publ. Univ. Bologna, 8, No. 15
Ovenden, M. W., 1954, Monthly Notices Roy. Astron. Soc., 114, 569 [BIBCODE 1954MNRAS.114..569O ]
Sezer, C., Gulmen, O., Gudur, N., 1985, Inf. Bull. Var. Stars, No. 2743