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 the same as the photometric temperature , derived using the color determined by standard microlensing techniques .
We measure [ Fe/H ] = 0.36 \pm 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 K and 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 C and N abundances 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 .