of the RCA chip on the CFHT. To characterize the degraded PSF in the standard way, the same process was applied to the NGC 6397 observations, constructing a PSF from 27 stars still visible in the resulting image. We applied two passes of the DAOPHOT II star-detection routine and used ALLSTAR to carry out the PSF-fitting photometry. The results yielded 147 stars detected in both the F555W and F814W frames in the region of overlap between the PC field of view and that of Freedman. Of these, 68 could be matched with the photometry of Freedman, yielding a mean [*I*]{}-band magnitude difference of only $0.03 \pm 0.35$ mag. The fact that we could match only half the stars in the field we attribute to differing completeness levels, which depend on rather small differences in the noise properties.

The resulting CM diagram and luminosity function are remarkably similar to those obtained by Freedman. While the photometry of the original [*HST*]{} image yields only 3 stars brighter than $I = 20,$ smoothing the image results in a total of 19 stars measured to be brighter than this magnitude. Moreover, the mean color measured in the degraded image of the stars brighter than 