K giants in Baade's window

Our sample was selected from the proper motion study of Spaenhauer et al. (1992AJ....103..297S). We have measured radial velocities for most of the sample, as well as line-strength indices on the system of Faber et al. (1985ApJS...57..711F).

We analyze the random and systematic errors in velocities and line strengths, and show that the bright (V<16.0) stars in our sample are predominantly foreground disk stars along the line of sight toward Baade's Window. We find that most of the bulge K giants have stronger Mg absorption at a given color than do stars in the solar neighborhood. If the K giants in our sample are moderately old, we suggest that on average they may have [Mg/Fe] approximately +0.3, consistent with the results of recent high-resolution spectroscopy in Baade's Window.