of such stars in POS2 argues that these stars must be associated with M32, they do not appear to be as strongly concentrated towards the center of M32 as the integrated light. Freedman finds 91 stars brighter than $I = 20.4$ in her inner field (a 1.42 arcmin$^2$ region of her field which encompasses POS1 — see Figure \[fig:plate1\]), giving a very similar surface density of 64 arcmin$^{-2}$.

However, whereas our [*I*]{}-band luminosity function goes essentially to zero at $I = 19.8,$ both Freedman (1989) and Davidge & Nieto (1992) see significant numbers of stars [*brighter*]{} than $I = 19.8$ extending to $I\approx18$. Since Freedman’s inner field overlaps with our own, we can test directly the hypothesis that this inconsistency is due to differences in resolution. We therefore convolved our PC image with a Gaussian kernel of FWHM= 06 to match Freedman’s CHFT resolution. We then integer-binned the data to a scale of 018 pix$^{-1}$, reasonably close to the 02 pix$^{-1}$ scale at the prime focus of the CFHT. Finally, we scaled the counts to match the exposure times used by Freedman, adding $\sim3$ “background" counts per pixel as well as noise to match the gain and readout noise characteristics 