  We present an R=45,000 Keck spectrum of the microlensed Galactic bulge
G-dwarf OGLE-2006-BLG-265, which has a high (~60) signal-to-noise ratio despite
its short (15 min) exposure time because the source was magnified by A~135.
While it is very metal-rich ([Fe/H]=0.56), the higher temperature of this star
compared with the luminous red giants usually measured in the bulge gives its
spectrum many unblended atomic lines. We measure the abundances of 17 elements,
including the first abundances for S and Cu in a bulge star. The [alpha/Fe]
ratios are subsolar, while the odd-Z elements are slightly supersolar, trends
that are also seen in the more metal-rich stars in the bulge and the local
Galactic disk. Because the star is a dwarf, the [O/Fe], [Na/Fe], and [Al/Fe]
ratios cannot be attributed to internal mixing, as is sometimes claimed for
giants. Similar high-resolution spectra could be obtained for about a dozen
bulge dwarf stars per year by means of well-designed target-of-opportunity
observations.
