variable IMF schemes that result in fewer metal poor stars) may be required to mimic chemical enrichment in the real universe. However, it is also possible that metal-poor stars could be present at larger radii. Large-radius storage of metal poor stars is a prediction of models of monolithic galaxy collapse (e.g. Larson 1975, Matteucci & Tornambè 1987, Arimoto & Yoshii 1987) in which the metal poor stars are created at large radius and enrichment proceeds at smaller and smaller radii until most of the gas is consumed. The abundance distribution at a given radius predicted by these models is always narrower than the closed-box model (Larson 1975).

The predicted number of metal-poor stars in the collapse model can be expressed as a fraction of total galaxy mass. In M32, the radius of the POS1 field encloses about 75% of the total light, using the parameters of Kent (1987) and assuming a deVaucouleurs $r^{1/4}$ profile. Conversion to mass requires a $M/L$ ratio as a function of radius. Older ages and higher metallicities drive $M/L$ up, so most galaxies are inferred to have a higher $M/L$ in the nucleus. However, M32 is likely to be an exception to this general rule owing 