  We combine spectroscopic metallicity values with integrated narrowband
continuum colors to explore the internal metallicity distribution in early-type
galaxies. The different techniques for determining metallicity (indices versus
colors) allows for an estimate of the contribution from metal-poor stars in a
predominantly metal-rich population which, in turn, places constraints on the
shape and width of a galaxy's metallicity distribution function (MDF). The
color-spectroscopic data is compared to the closed box, infall and
inhomogeneous chemical evolution models. The G-dwarf problem, a deficiency in
metal-poor stars as compared to closed box models, is evident in the dataset
and indicates this deficiency is common to all early-type galaxies. However,
even simple infall models predict galaxy colors which are too blue compared to
the observations. A simple analytic model is proposed which matches the
elliptical data and recent HST observations of M31 (Worthey et al 2005) and NGC
5128 (Harris & Harris 2000) by reducing the number of metal-poor stars in a
systematic fashion. While without physical justification, the shape of these
models are similar to predictions of inhomogeneous enrichment scenarios.
