An estimate of the DM profile in the Galactic bulge region
  We present an analysis of the mass distribution in the region of the Galactic
bulge, which leads to constraints on the total amount and distribution of Dark
Matter (DM) therein. Our results -based on the dynamical measurement of the
BRAVA collaboration- are quantitatively compatible with those of a recent
analysis, and generalised to a vaste sample of observationally inferred
morphologies of the stellar components in the region of the Galactic bulge. By
fitting the inferred DM mass to a generalised NFW profile, we find that cores
(index gamma smaller than 0.6) are forbidden only for very light configurations
of the bulge, and that cusps (index gamma bigger than 1.2) are allowed, but not
necessarily preferred. Interestingly, we find that the results for the bulge
region are compatible with those obtained with dynamical methods (based on the
rotation curve) applied to outer regions of the Milky Way, for all morphologies
adopted. We find that the uncertainty on the shape of the stellar morphology
heavily affects the determination of the DM distribution in the bulge region,
which is gravitationally dominated by baryons, adding up to the uncertainty on
its normalization. The combination of the two hinders the actual possibility to
infer sound conclusions about the distribution of DM in the region of the
Galactic bulge, and only future observations of the stellar census and dynamics
in this region will bring us closer to a quantitatively more definite answer.
