Stellar Ages through the Corners of the Boxy Bulge
  In some scenarios for the formation of the Milky Way bulge the stellar
population at the edges of the boxy bulge may be younger than those on the
minor axis, or close to the Galactic center. So far the only bulge region where
deep color-magnitude diagrams have been obtained is indeed along the minor
axis. To overcome this limitation, we aim at age-dating the bulge stellar
populations far away from the bulge minor axis. Color-magnitude diagrams and
luminosity functions have been obtained from deep near-IR VLT/HAWK-I images
taken at the two Southern corners of the boxy bulge, i.e., near the opposite
edges of the Galactic bar. The foreground disk contamination has been
statistically removed using a pure disk field observed with the same instrument
and located approximately at similar Galactic latitudes of the two bulge
fields, and 30deg in longitude away from the Galactic center. For each bulge
field, mean reddening and distance are determined using the position of red
clump stars, and the metallicity distribution is derived photometrically using
the color distribution of stars in the upper red giant branch. The resulting
metallicity distribution function of both fields peaks around [Fe/H] -0.1 dex,
with the bulk of the stellar population having a metallicity within the range:
-1 dex < [Fe/H] <+0.4 dex, quite similar to that of other inner bulge fields.
Like for the inner fields previously explored, the color-magnitude diagrams of
the two bar fields are consistent with their stellar population being older
than ~10 Gyr, with no obvious evidence for the presence of a younger
population.
