Evidence for a metal-poor population in the inner Galactic Bulge
  The inner Galactic Bulge has, until recently, been avoided in chemical
evolution studies due to extreme extinction and stellar crowding. Large,
near-IR spectroscopic surveys, such as APOGEE, allow for the first time the
measurement of metallicities in the inner region of our Galaxy. We study
metallicities of 33 K/M giants situated in the Galactic Center region from
observations obtained with the APOGEE survey. We selected K/M giants with
reliable stellar parameters from the APOGEE/ASPCAP pipeline. Distances,
interstellar extinction values, and radial velocities were checked to confirm
that these stars are indeed situated in the inner Galactic Bulge. We find a
metal-rich population centered at [M/H] = +0.4 dex, in agreement with earlier
studies of other bulge regions, but also a peak at low metallicity around $\rm
[M/H] = -1.0\,dex$, suggesting the presence of a metal-poor population which
has not previously been detected in the central region. Our results indicate a
dominant metal-rich population with a metal-poor component that is enhanced in
the $\alpha$-elements. This metal-poor population may be associated with the
classical bulge and a fast formation scenario.
