Mass of retained metals within 3 kpc as a function of stellar mass within the same radius. Models that retain less than 80% of their stellar mass are shown as open symbols. For clarity, all dSphs, regardless of how many perigalacticons, are shown as either circles for Fe or squares for Mg. dSphs that suffer substantial mass loss retain more metals than smaller undisturbed systems, a sign of higher metallicity in the core. In undisturbed cases, the model dSphs contain less metal (by a factor of ~3) than the observed dSphs at the same stellar mass, a possible discrepancy that arises from differing IMFs and yields. From left to right the groups of simulation points correspond to Carina-type dSphs (orange), Sextans (green), Sculptor (blue), and Fornax (red). Observed values for Mg and Fe from Kirby et al. (2011c) are shown in magenta.