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We analyze a high-resolution spectrum of a microlensed G-dwarf in theGalactic bulge, acquired when the star was magnified by a factor of 110. Wemeasure a spectroscopic temperature, derived from the wings of the Balmerlines, that is the same as the photometric temperature, derived using the colordetermined by standard microlensing techniques. We measure [Fe/H]=0.36 +/-0.18,which places this star at the upper end of the Bulge giant metallicitydistribution. In particular, this star is more metal-rich than any bulge Mgiant with high-resolution abundances. We find that the abundance ratios ofalpha and iron-peak elements are similar to those of Bulge giants with the samemetallicity. For the first time, we measure the abundances of K and Zn for astar in the Bulge. The [K/Mg] ratio is similar to the value measured in thehalo and the disk, suggesting that K production closely tracks alphaproduction. The [Cu/Fe] and [Zn/Fe] ratios support the theory that thoseelements are produced in Type II SNe, rather than Type Ia SNe. We also measuredthe first C and N abundances in the Bulge that have not been affected by firstdredge-up. The [C/Fe] and [N/Fe] ratios are close to solar, in agreement withthe hypothesis that giants experience only canonical mixing.

A High-Resolution Spectrum of the Highly Magnified Bulge G-Dwarf MOA-2006-BLG-099S