  Stellar population models with abundance distributions determined from the
analytic Simple model of chemical evolution fail to match observations of the
nuclei of bulge-dominated galaxies in three respects. First, the spectral
energy distribution in the mid-ultraviolet range 2000 < lam < 2400 exceeds
observation by ~ 0.6 mag. Most of that excess is due to metal-poor main
sequence stars. Second, the models do not reproduce metal-sensitive optical
absorption features that arise mainly from red giant stars. Third, the strength
of a Ca II index sensitive to hot stars does not jibe with the predicted number
of A-type horizontal branch stars. The number of metal poor stars in galaxies
is at least a factor of two less than predicted by the Simple model, exactly
similar to the ``G Dwarf problem'' in the solar cylinder. Observations at
larger radii in local group galaxies indicate that the paucity of metal poor
stars applies globally, rather than only in the nuclei. Because of the
dominance of metal rich stars, primordial galaxies will have a plentiful dust
supply early in their star formation history, and thus will probably have weak
Lyman-alpha emission, as is apparently observed. We confirm that early-type
galaxies cannot have been formed exclusively from mergers of small all-stellar
subsystems, a result already established by dynamical simulations. The
constraint of peaked abundance distributions will limit future chemical
evolution models. It will also make age estimates for the stellar populations
in early type galaxies and bulges more secure.
