1 Introduction

Accounts of the discovery of optical and radio emission from the supernova SN1998bw has been given elsewhere (Galama et al. 1998; Kulkarni et al. 1998). The primary link between SN1998bw and GRB980425 is the coincidence of the two events in space and time (Galama et al. 1998). Unfortunately, the coincidence window (16-arcmin error circle, $\pm$ 1 day) is not sufficiently small to make a firm claim of the association.

BeppoSAX NFI observations show that there are two sources, a secularly fading source coincident (within the NFI error radius of 1.5 arcmin) with SN1998bw and a source which is not coincident with the SN and which appeared to fade by the end of the first NFI observation (initiated 10 h after the burst and total duration of 40 h). The latter source has not been detected in subsequent NFI observations (see GCN 151 for summary; also contribution by E. Pian in these proceedings). A simple interpretation is that the transient source is the X-ray afterglow of GRB980425. Another possibility is that the transient source is unrelated to GRB980425. Upcoming ASCA observations may clarify this confusing situation.

What has been lost in all the exciting developments is that SN1998bw is an unusual supernovae, regardless of its association to GRB980425. Indeed, it's claimed and controversial association tends to overshadow the unusual nature of this SN. We now exclusively focus on the radio properties of this SN. The radio observations were conducted with the Australia Telescope Compact Array (ATCA) as a part of our GRB effort.