age of 15 Gyr is also shown; the histogram shifts only slightly to lower metallicity.

In Figure \[fig:hist\] we compare the distribution of metal abundance found in M32 with closed-box models of chemical evolution. These simple, one-parameter models are one-zone, with no gas infall or outflow and zero metal content initially, and assume instantaneous recycling of heavy elements (Searle & Sargent 1972). The photometric uncertainties for the stars considered here are relatively small, and the models have not been smoothed. Quite striking is the fact that the observed metallicity distribution is significantly narrower than the closed-box models would predict. This region of M32 appears at first glance to be more monometallic than even the solar cylinder. On the other hand, if the main ridge of stars in the CM diagram is comprised of populations with a spread in age, then the youthful stars may move to the next higher \[Fe/H\] bin, and it is possible that the real abundance distribution resembles that of the solar neighborhood more than it first appears in Figure \[fig:hist\]. For example, the metal abundance of the main red component is \[Fe/H\]$= -0.2$ if one assumes an age of 15 Gyr, \[Fe/H\]$=-0.07$ for 8 Gyr, but 