is obtainable. ALLFRAME is applied to the data [*after*]{} object detection and aperture photometry are carried out using DAOPHOT II (Stetson 1987). The global characteristics of the CM diagram produced using DAOPHOT II and ALLSTAR were essentially identical to those found using ALLFRAME. However, the latter produced fewer outliers and gave a cleaner-looking result.

To push the star detection limit to as faint a level as possible, we coadded all images taken through the same filter. ALLFRAME was then applied to the F555W and F814W images simultaneously. While analyzing the coadded images does not make full use of the information available in all 8 individual frames, experiments using both methods showed that our completeness fraction was significantly higher when coadding frames prior to object detection.

Neither POS1 nor POS2 had a sufficient number of bright and reasonably isolated stars to allow proper characterization of the PSF. The PSF was consequently derived from F555W and F814W images of the globular cluster NGC 6397 observed with [*HST*]{} approximately two months prior to the date of the M32 observations. No focus changes were commanded during the intervening period, and desorption of volatiles will not have significantly altered the focus over this time.

Owing 