COMMISSION 27 OF THE I. A. U.
                 INFORMATION BULLETIN ON VARIABLE STARS
                             Number 3581

                                                       Konkoly Observatory
                                                       Budapest
                                                       20 March 1991

                                                       HU ISSN 0374 - 0676


                   OBSERVATIONS OF SUPERNOVA 1989 B


   The supernova 1989 B was discovered in NGC 3627 (Evans, 1989). Due to
its relative brightness (near 10m V in maxima) we have tried to use traditional 
methods for its observations. The observations were obtained during
16 nights in 1989 in Tian-Shan observatory of Sternberg Astronomical Institute 
with the 19" reflector and a computer controlled WBVR photometer (EMI
9863). The previous processing of these data was reported earlier (Tsvetkov
et al., 1990). But later we have obtained more observations and the new
method for galaxy flux reduction was used. We have measured the precise 
position of the supernova from nearby stars and later, when the supernova 
became invisible, the measurements were repeated with the same diaphragm of
29". So we have obtained the estimation of the galaxy flux in our 
observations of supernova.


                     Table I.

             B,V,R data for SN1989 B


                B       V       R     B-V    V-R

2447587.273   14.07   12.88   12.03   1.19   0.85
    588.412   14.29   12.98   12.10   1.31   0.88
    589.408   14.26   13.00   12.11   1.25   0.89
    590.369   14.32   13.06   12.09   1.26   0.97
    591.350   14.41   13.09   12.13   1.32   0.96
    592.398   14.51   13.25   12.23   1.27   1.02
    597.372   14.65   13.48   12.61   1.17   0.87
    598.345   14.67   13.48   12.55   1.20   0.93
    599.416  (15.22)  13.70:  12.75:   -     0.95:
    611.170   15.36   14.17   13.48   1.19   0.69
    613.209   15.38   14.09   13.54   1.29   0.55
    626.327   15.43   14.56   13.80   0.88   0.76
    628.367   15.19   14.38   13.68   0.81   0.70
    640.163   15.60   14.42   13.72   1.18   0.70
    643.181   15.46   14.62   14.09   0.84   0.54
    644.264   15.40   14.66   13.89   0.74   0.76


                     Table II.

            Ultraviolet data for SN1989 B


                JD          W      W-B

            2447588.363   14.89   0.60
                591.372   14.94   0.62
                597.858   14.88   0.21
                612.189   15.09  -0.28
                627.341   15.61   0.30
                642.534   16.11   0.62


   All observations were corrected for atmospheric extinction and reduced to
WBVR system using the standard star HD85217 (Khaliullin et al., 1985). The B,
V and R magnitudes are given in Table I, where every point is the mean value
from 2 to 5 measurements. The mean errors of these data are of the order of
+-0.1m-0.2m. The counts of our photometer in W (ultraviolet) were too small,
and we have to average even measurements from different nights to obtain
reasonable values. These data are given in Table II. The mean errors are
+-0.3m-0.5m. The observations on JD 2447599 were disturbed by an aurora. The
galaxy flux in the supernova position corresponds to a G0 V star.


                                          I.M. VOLKOV

                               Sternberg State's Astronomical Institute
                                USSR, Moscow, 117899, Universitetsky 13



References:

Evans, R.O.: 1989, IAU Circular, No. 4726. [BIBCODE 1989IAUC.4726....1E ]
Khaliullin, Kh.F., Mironov, A.V., Moshkalev, V.G.: 1985, Astrophys. Space
     Sci., 111, 291. [BIBCODE 1985Ap&SS.111..291K ]
Tsvetkov, D.Yu., Kimeridze, G.N., Volkov, I.M., Bartunov, O.S.,
     Ikonnikova, N.P.: 1990, Astron. Astrophys., 236, 133. [BIBCODE 1990A&A...236..133T ]