A high-resolution spectrum of the highly magnified bulge G dwarf MOA-2006-BLG-099S

We analyze a high-resolution spectrum of a microlensed G dwarf in the Galactic bulge, acquired when the star was magnified by a factor of 110. We measure a spectroscopic temperature, derived from the wings of the Balmer lines, that is consistent with the photometric temperature, derived using the color determined by standard microlensing techniques. We measure [Fe/H] = 0.36 +/- 0.18, which places this star at the upper end of the bulge giant metallicity distribution. In particular, this star is more metal-rich than any bulge M giant with high-resolution abundances. We find that the abundance ratios of alpha and iron-peak elements are similar to those of bulge giants with the same metallicity. For the first time, we measure the abundances of Kand Zn for a star in the bulge. The [K/Mg] ratio is similar to the value measured in the halo and the disk, suggesting that K production closely tracks alpha production. The [Cu/Fe] and [Zn/Fe] ratios support the theory that those elements are produced in Type II SNe, rather than Type Ia SNe. We also measured the first CandNabundances in the bulge that have not been affected by first dredge-up. The [C/Fe] and [N/Fe] ratios are close to solar, in agreement with the hypothesis that giants experience only canonical mixing.