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 mu 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 mu 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 mu Leo and [Fe/H]=+0.47+/-0.17 for BW IV-167 (relative to a Solar epsilon (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 mu 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 mu Lee, but we caution that further study of elements other than Fe in BW IV-167 remains to be done. (C) 1996 American Astronomical Society.