We report analysis of echelle spectra (R = 17,000, S/N almost-equal-to 50) of 12 Galactic bulge K giants in Baade's window from the sample of Rich ( 1988). We perform an abundance analysis for 11 stars ranging from [Fe/H] = -1 to [Fe/H] = 0.45. The accuracy of our abundance scale is confirmed relative to the disk super-metal-rich stars via the metal-rich giant mu Leonis, and to the Galactic globular clusters using a star in NGC 5927. We investigate the effects of CN blends on abundance analysis for stars more metal-rich than [Fe/H] = -0.3, through spectrum synthesis of the region from 6140 to 7600 angstrom, including in excess of 8000 (CN)-C-12 and (CN)-C-13 lines. We confirm Peterson's assertion that blends of atomic lines with CN vibration-rotation lines can affect abundance results at R = 17,000; failure to reject affected Fe lines would have resulted in a spurious 0.3 dex increase in the derived Fe abundances of our most metal-rich stars. We find that one of the most metal-rich Baade's window stars (BW IV-167) has approximately the same metallicity as the super-metal-rich disk giant mu Leo. The abundance scale of Rich (1988), based on measurement of strong Fe and Mg lines, is almost-equal-to 0.3 dex high but may agree with our results if Rich's [M/H] actually measures [(Fe + Mg)/H]. Using our abundances to transform Rich's [M/H] distribution, we find that the mean [Fe/H] is -0.25 for the bulge, slightly less than, but not appreciably different from, the mean [Fe/H] for solar neighborhood G and K giants. Surprisingly, this is not in conflict with the Galactic metallicity gradient found for the solar neighborhood. The extant data on [Fe/H] with Galactocentric radius are completely consistent with a zero gradient within the solar circle. Infrared flux temperatures for a sample of 34 Baade's window K giants observed by Frogel & Whitford ( 1987) show that the bulge (J - K) versus T(eff) relation is identical to that of the solar neighborhood. We assert that the observed infrared colors reflect the actual effective temperatures, and that infrared colors affected by molecular blanketing cannot explain why the bulge giant branch is as blue as that of 47 Tuc. Verification of the (J - K) temperature scale, and use of our average [Fe/H] results, suggest that the Frogel & Whitford ( 1987) infrared H-R diagram requires that the mean mass of Baade's window giants can be no less than about 1.1 M.. Abundances for the alpha-elements are based on spectrum synthesis of lines due to Mg, Ti, Ca, and Si. We find a puzzling pattern in the trends of element abundance ratios with [ Fe/ H 1. Mg and Ti are enhanced by almost-equal-to 0.3 dex relative to solar over almost the full [Fe/H] range. In contrast, Ca and Si closely follow the normal trends for disk giants, with solar ratios occurring above [Fe/H] almost-equal-to -0.2. The enrichment pattern of bulge giants sets them clearly apart from disk giants of the same [Fe/H]. For a subset of the sample we estimate [O/Fe] almost-equal-to O using the [O I] line at 6300 angstrom; the absence of a carbon abundance indicator requires us to assume a solar C/Fe ratio. We speculate that the high Mg abundances seen in ellipticals (Worthey, Faber, & Gonzalez 1992) may reflect a common enrichment process for bulges and ellipticals. We further propose that the high Ti abundances may largely account for the tendency for Baade's window M giants to have later spectral types than solar neighborhood M giants of the same infrared color (Frogel & Whitford 1987). Other noteworthy results include enhanced Al abundances similar to those seen in globular cluster giants, and (tentatively) enhancement of the r-process element Eu in the metal-rich bulge stars. The iron-peak and s-process elements appear normal relative to Fe. We find one super-Li-rich giant, BW I-194. We also identify BW I-155 as a spectroscopic double. This work also presents the following results of general use to investigators in the field: (1) In order to obtain a complete set of g f values for our Fe i lines, we find transformations between numerous log g f sources. In total we provide a list of 208 atomic g f values, for Fe I and numerous other species. (2) We present a list of uncontaminated continuum regions appropriate for use in metal-rich stars, as well as atomic lines clear from severe CN blending at a variety of metallicities.
