Echelle Spectroscopy of a Metal-Rich K Giant in Baade's Window Using the Keck High-Resolution Spectrograph
We analyze echelle spectra of the metal-rich disk giant μ Leo and the Baade's Window giant BW IV-167, obtained with the Keck high-resolution spectrograph. We perform an abundance analysis using three different methods, and using two different grids of metal-rich model atmospheres from Kurucz and the Marcs group. We find that μ Leo and BW IV- 167 have nearly identical surface gravities, effective temperatures, equivalent widths, and microturbulent velocities. We determine [Fe/H]=+0.46±0.14 for μ Leo and [Fe/H]=+0.47±0.17 for BW IV-167 (relative to a Solar ɛ(Fe)=7.52). The full range of derived abundances (using the three methods and two grids of model atmospheres) is 0.40<[Fe/H]<0.49 for μ Leo and 0.40<[Fe/H]<0.55 for BW IV-167. We confirm the measurement of McWilliam & Rich [ApJS, 91, 749 (1994)] of [Fe/H]=+0.44 for BW IV-167. This analysis strongly supports the reality of enhanced Fe abundance in some populations of stars. Many properties of the Baade's Window giant are identical to those of μ Leo, but we caution that further study of elements other than Fe in BW IV-167 remains to be done.