that time.

As discussed by Gaensler et al. (1997), it is not easy to account for the observed asymmetry of SNR 1987A. Models involving the annular structure of the circumstellar material (e.g. Chevalier & Dwarkadas 1995) have difficulty accounting for the degree of enhancement in the lobes and the east-west asymmetry. Similar difficulties are encountered in trying to explain the optical hotspots. Lawrence et al. (2000) conclude that “fingers or jets” in the distribution of ejecta from the supernova is the most plausible explanation.

In a recent publication, Ball et al. (2001) have analysed the 843 MHz flux densities observed with MOST to 2000 May (day 4820). They find a transition from a declining rate of increase observed from about mid-1991 (day $\sim 1600$) to early-1995 (day $\sim 2900$), to a larger and constant rate of increase, $62.7 \pm 0.5 \;\mu$Jy day$^{-1}$, since then. This change in slope occurred at about the same time as the appearance of the first optical hotspot (Lawrence et al. 2000), suggesting a possible connection.

In this paper, we extend the ATCA observational data base from 1995 to February 2001 (day 5100) and discuss these results in conjunction with those of Ball et al. (2001). 