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This paper explores the integrated-light characteristics of the Milky Way(MW) bulge and to what extent they match those of elliptical galaxies in thelocal universe. We model composite stellar populations with realistic abundancedistribution functions (ADFs), tracking the trends of individual elements as afunction of overall heavy element abundance as actually observed in MW bulgestars. The resultant predictions for absorption feature strengths from the MWbulge mimic elliptical galaxies better than solar neighborhood stars do, butthe MW bulge does not match elliptical galaxies, either. Comparing bulge versuselliptical galaxies, Fe, Ti, and Mg trend about the same for both but C, Na,and Ca seem irreconcilably different.  Exploring the behavior of abundance compositeness leads to the concepts of"red lean" where a narrower ADF appears more metal rich than a wide one, and"red spread" where the spectral difference between wide and narrow ADFsincreases as the ADF peak is moved to more metal-rich values. Tests on thesystematics of recovering abundance, abundance pattern, and age from compositestellar populations using single stellar population models were performed. Thechemical abundance pattern was recovered adequately, though a few minorsystematic effects were uncovered. The prospects of measuring the width of theADF of an old stellar population were investigated and seem bright using UV toIR photometry.

Composite Stellar Populations and Element by Element Abundances in the Milky Way Bulge and Elliptical Galaxies