The Dark Matter Halo of the Milky Way, AD 2013
  We derive the mass model of the Milky Way (MW) using a cored dark matter (DM)
halo profile and recent data. The method used consists in fitting a spherically
symmetric model of the Galaxy with a Burkert DM halo profile to available data:
MW terminal velocities in the region inside the solar circle, circular velocity
as recently estimated from maser star forming regions at intermediate radii,
and velocity dispersions of stellar halo tracers for the outermost Galactic
region. The latter are reproduced by integrating the Jeans equation for every
modeled mass distribution, and by allowing for different velocity anisotropies
for different tracer populations. For comparison we also consider a
Navarro-Frenk-White profile. We find that the cored profile is the preferred
one, with a shallow central density of rho_H~4x10^7M_s/kpc^3 and a large core
radius R_H~10 kpc, as observed in external spirals and in agreement with the
mass model underlying the Universal Rotation Curve of spirals. We describe also
the derived model uncertainties, which are crucially driven by the poorly
constrained velocity dispersion anisotropies of halo tracers. The emerging
cored DM distribution has implications for the DM annihilation angular profile,
which is much less boosted in the Galactic center direction with respect to the
case of the standard \Lambda CDM, NFW profile. Using the derived uncertainties
we discuss finally the limitations and prospects to discriminate between cored
and cusped DM profile with a possible observed diffuse DM annihilation signal.
The present mass model aims to characterize the present-day description of the
distribution of matter in our Galaxy, which is needed to frame current crucial
issues of Cosmology, Astrophysics and Elementary Particles.
