  We present an abundance analysis based on high dispersion and high
signal-to-noise ratio Keck spectra of a very highly microlensed Galactic bulge
dwarf, OGLE-2007-BLG-349S, with Teff ~ 5400 K. The amplification at the time
the spectra were taken ranged from 350 to 450. This bulge star is highly
enhanced in metallicity with [Fe/H] = +0.51 \pm 0.09 dex. The abundance ratios
for the 28 species of 26 elements for which features could be detected in the
spectra are solar. In particular, there is no evidence for enhancement of any
of the alpha-elements including O and Mg. We conclude that the high [Fe/H] seen
in this star, when combined with the equally high [Fe/H] derived in previous
detailed abundance analysis of two other Galactic bulge dwarfs, both also
microlensed, implies that the median metallicity in the Galactic bulge is very
high. We thus infer that many previous estimates of the metallicity
distribution in the Galactic bulge have substantially underestimated the mean
Fe-metallicity there due to sample bias, and suggest a candidate mechanism for
such. If our conjecture proves valid, it may be necessary to update the
calibrations for the algorithms used by many groups to interpret spectra and
broad band photometry of the integrated light of very metal-rich old stellar
populations, including luminous elliptical galaxies.
