Alpha Enhancement and the Metallicity Distribution Function of Plaut's Window

We present Fe, Si, and Ca abundances for 61 giants in Plaut's window (l = -1°, b = -8fdg5) and Fe abundances for an additional 31 giants in a second, nearby field (l = 0°, b = -8°) derived from high-resolution (R ≈ 25,000) spectra obtained with the Blanco 4 m telescope and Hydra multifiber spectrograph. The median metallicity of red giant branch (RGB) stars in the Plaut's field is ~0.4 dex lower than those in Baade's window, and confirms the presence of an iron abundance gradient along the bulge minor axis. The full metallicity range of our (biased) RGB sample spans -1.5 < [Fe/H] < +0.3, which is similar to that found in other bulge fields. We also derive a photometric metallicity distribution function for RGB stars in the (l = -1°, b = -8°.5) field and find very good agreement with the spectroscopic metallicity distribution. The radial velocity (RV) and dispersion data for the bulge RGB stars are in agreement with previous results of the Bulge Radial Velocity Assay survey, and we find evidence for a decreasing velocity dispersion with increasing [Fe/H]. The [α/Fe] enhancement in Plaut field stars is nearly identical to that observed in Baade's window, and suggests that an [α/Fe] gradient does not exist between b = -4° and -8°. Additionally, a subset of our sample (23 stars) appears to be foreground red clump stars that are very metal rich, exhibit small metallicity and RV dispersions, and are enhanced in α elements. While these stars likely belong to the Galactic inner disk population, they exhibit [α/Fe] ratios that are enhanced above the thin and thick disk.