the 3 brightest stars, and the faint, compact group of galaxies $\sim 4''$ SW of . We used C as the origin of coordinates, because it is more isolated than A1, A2 or B, and suffers less contamination from the arc. The differences between the $R$ and $I$ coordinate offsets of the images of the core are $\leq 0\farcs015$. The maximum errors for centroiding the images of the core, as determined with IRAF, were 002; we adopted these values as the standard errors for their coordinate offsets in the tables. There is also very good agreement between our estimates for the latter offsets, and the analogous estimates of KH93: the two sets differ by $\leq 0\farcs045$, the size of a PC1 pixel.

Our magnitude estimates and those in AVHM94 for A1$+$A2 (unresolved in their observations), B, C and X differ by $< 3\sigma$, using their errors, which are larger than ours by factors of $\sim 5-10$. Thus, our measurements should represent a substantial refinement of the estimates of the colors of the images of the core and of X that were discussed in AVHM94. Our magnitude estimates for G are fainter than those in AVHM94 by $\sim 0.7$ and $\sim 