by Falco et al. with WFPC1 (Falco 1993), and by Angonin-Willaime et al. (AVHM94). As the figures show, we, too, detected the lens galaxy with WFPC2. From our data, we are able to determine the spatial distribution of the lens galaxy’s light emission at high significance levels. We also see clearly object X (SM93) near our detection limit, especially in $R$. Furthermore, one can easily see in both $R$ and $I$ (Figures 1 and 2) arc-like extended emission connecting A2 and B, and joining A1 and A2. The arc is unresolved in the direction from the center of brightness of G. Such an arc can be explained as lensed emission from a single, compact source near the QSO core, as we discuss in §4.

We used IRAF to measure the pixel coordinates of the centers of brightness and the aperture magnitudes of objects with peak apparent magnitudes of 22.7 mag/arcsec$^2$ (24.2 mag/arcsec$^2$) above the sky level of the $I$ ($R$) image. The absolute coordinates, e.g., of B, agree with those of Katz & Hewitt (KH93) at the $0\farcs08$ level, consistent with their absolute positional uncertainty of $0\farcs1$. The images of the core and the galaxy were well above our detection 