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Introduction

Supernovae (SNe) are spectacular explosions of some stars which have ran out of their thermonuclear fuel in the process of evolution. According to theoretical models, most massive stars (M > 10-15 M$_{\odot}$) almost inevitably end in such an explosion (Fowler and Hoyle, 1964; Woosley and Weaver, 1986). Since the life cycle of massive stars is very short (<30Myr), one can expect to observe more or less frequent SNe in galaxies where current intensive star formation takes place. Blue Compact Galaxies (BCGs), or HII-galaxies, are low-mass gas-rich galaxies where we are witnessing very intensive star formation (SF) events, lasting not longer than 10 to 100 Myr. Such events are usually called SF bursts since the SF rate during those periods is many times higher than the SF rate averaged over the whole life-time of a galaxy. It is curiuos that despite about 30 years of study the phenomenon of BCGs and various observations of about a thousand such objects, the first SN in BCG was discovered as late as 1995 (SN 1995ah in BCG HS 0016+1449, Popescu et al., 1997).

We report on the second SN in BCG, discovered in observations with the 6 m telescope of SAO (Kniazev et al., 1998). The observations were conducted in the frame of the follow-up spectroscopy of the candidates selected in the Hamburg/SAO Survey (HSS) for emission-line galaxies (Lipovetsky et al., 1996; Ugryumov et al., 1998; Pustilnik et al., 1998), which is based on the digitized plates of the Hamburg Quasar Survey (Hagen et al., 1995). The main goal of the HSS is the creation of a large new BCG sample in a large area of the sky.

The supernova SN 1998bv was discovered on April 6, 1998 in the galaxy HS 1035+4758 selected as an ELG candidate in the HSS. This galaxy had been previously catalogued in literature as NPM1G+47.0175 (Klemola et al., 1987) with the coordinates of the center R.A. = 10 $^{h}38^{m}25\fs71$, Dec. = $+47^{\circ}42^\prime36\farcs5$(J2000) and the estimate of blue magnitude B=$16\fm97$. Both the redshift and the type of this galaxy were unknown. In Fig.1 we present its Digital Sky Survey (DSS) image.

   

Figure 1: DSS image of the galaxy HS 1035+4758. North is up, east is left.
Figure 2: Short exposure spectrum of the central part of the host galaxy HS 1035+4758.