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We present radial velocities and chemical abundances of O, Na, Mg, Al, Si,Ca, Cr, Fe, Co, Ni, and Cu for a sample of 156 red giant branch stars in twoGalactic bulge fields centered near (l,b)=(+5.25,-3.02) and (0,-12). The(+5.25,-3.02) field also includes observations of the bulge globular clusterNGC 6553. The results are based on high resolution (R~20,000), highsignal-to-noise (S/N>70) FLAMES-GIRAFFE spectra obtained through the ESOarchive. However, we only selected a subset of the original observations thatincluded spectra with both high S/N and that did not show strong TiO absorptionbands. The present work extends previous analyses of this data set beyond Feand the alpha-elements Mg, Si, Ca, and Ti. While we find reasonable agreementwith past work, the data presented here indicate that the bulge may exhibit adifferent chemical composition than the local thick disk, especially at[Fe/H]>-0.5. In particular, the bulge [alpha/Fe] ratios may remain enhanced toa slightly higher [Fe/H] than the thick disk and the Fe-peak elements Co, Ni,and Cu appear enhanced compared to the disk. There is also some evidence thatthe [Na/Fe] (but not [Al/Fe]) trends between the bulge and local disk may bedifferent at low and high metallicity. We also find that the velocitydispersion decreases as a function of increasing [Fe/H] for both fields, and donot detect any significant cold, high velocity population. A comparison withchemical enrichment models indicates that a significant fraction of hypernovaeare required to explain the bulge abundance trends, and that initial massfunctions that are steep, top-heavy (and do not include strong outflow), ortruncated to avoid including contributions from stars >40 solar masses areruled out, in particular because of disagreement with the Fe-peak abundancedata. [abridged]

Light, Alpha, and Fe-Peak Element Abundances in the Galactic Bulge