to Johnson $R$ and $I$. We obtained these data on 8 November 1994, all in fine lock mode. We used filter F675W for 4 of the exposures, one of 1800 sec and 3 of 2100 sec. We used filter F814W for the other 5 equal-duration exposures of 2100 sec. The  system was located near the center of PC1; unsaturated stellar objects on PC1 were aligned from exposure to exposure with a resultant rms scatter of 0.13 pixels (each pixel is $\simeq 0\farcs0455$). We combined the exposures for each filter into a single image, to reject most of the numerous cosmic ray “hits” in our exposures. We used standard IRAF[^1] tasks, which eliminated the majority of the “hot” pixels in the combined exposures. The combined images are the means of 4 and 5 images for F675W and F814W, respectively, each scaled by its exposure time. We will refer to these combined images as “R” and “I” images, respectively.

We detected the  system in each band, and found the components that were known from previous ground-based observations (HTLSB92; SM93; Angonin-Willaime et al. 1994, hereafter AVHM94) and from HST observations (Falco 1993). Figures 1 and 2 respectively show $\sim 5\farcs8$ and $\sim 23\farcs3$ 