the colors and magnitudes of the M31 stars that make up the majority of field stars at POS1. The POS1 coordinates were chosen so that the nucleus of M32 was roughly centered in WF3. The Planetary Camera (PC) image (00455 per pixel) covers a region extending from 1 to 2 arcminutes almost due south of the center of M32 (see Figure \[fig:plate1\] = Plate 1). The POS2 field is situated $\approx 5$6 NE of POS1 in an area originally intended to match the background surface brightness of M31 underlying M32. Four 500s exposures were taken in each of F555W ([*V*]{}) and F814W ([*I*]{}) in each pointing. An additional three 1000s exposures were taken through F300W, but we defer discussion of these data to a later paper. The coadded F814W image is shown in Figure \[fig:plate2\] (Plate 2).

Stellar photometry was carried out using the crowded-field, PSF-fitting package ALLFRAME (Stetson 1994), the most recent development in the DAOPHOT series of photometry packages. ALLFRAME differs from its predecessors primarily in its ability to use information from many individual frames simultaneously. The extra geometric and photometric information available from multiple frames extends the range of magnitudes and crowding conditions for which useful photometry 