0$\farcs$68 or 2.3 pc at the distance of M31 (690 kpc). The fields measure 23$\farcm$2 on a side or, ignoring projection effects due to inclination, 4.6 $\times$ 4.6 kpc$^{\rm 2}$. The typical resolution of the WB92 data set was 2$\arcsec$, and for the 1997 data set $\sim$1-2$\arcsec$ (which corresponds to a linear resolution of $\sim$4-7 pc). Future papers will provide the entire 1997 data set and its reduction, although we outline some essential reduction details here.

DATA REDUCTION AND CALIBRATION OF 1997 DATA SET
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Initial reduction of the individual frames (bias subtraction and flat fielding) was performed within IRAF$\footnote{IRAF (Image Reduction
and Analysis Facility) is provided by the National Optical Astronomy
Observatories (NOAO). NOAO is operated by the Association of
Universities for Research in Astronomy (AURA), Inc. under cooperative
agreement with the National Science Foundation}$. A twilight “master-flat” was constructed by co-adding twilight flats from several different nights, in each filter. The twilight master-flats successfully removed sensitivity variations across the chip. This could be seen by the uniformity of the dome flats after correcting them with the master-flats. Residual, large-scale variations were of the order 1$\%$ across the field. Registered H$\alpha$+\[\], off-band, and blue images were then combined and 