  An accurate knowledge of the dark matter distribution in the Milky Way is of
crucial importance for galaxy formation studies and current searches for
particle dark matter. In this paper we set new dynamical constraints on the
Galactic dark matter profile by comparing the observed rotation curve, updated
with a comprehensive compilation of kinematic tracers, with that inferred from
a wide range of observation-based morphologies of the bulge, disc and gas. The
generalised Navarro-Frenk-White (NFW) and Einasto dark matter profiles are
fitted to the data in order to determine the favoured ranges of local density,
slope and scale radius. For a representative baryonic model, a typical local
circular velocity of 230 km/s and a distance of the Sun to the Galactic centre
of 8 kpc, we find a local dark matter density of 0.420+0.021-0.018 (2 sigma) +-
0.025 GeV/cm^3 (0.420+0.019-0.021 (2 sigma) +- 0.026 GeV/cm^3) for NFW
(Einasto), where the second error is an estimate of the systematic due to
baryonic modelling. Apart from the Galactic parameters, the main sources of
uncertainty inside and outside the solar circle are baryonic modelling and
rotation curve measurements, respectively. Upcoming astronomical observations
are expected to reduce all these uncertainties substantially over the coming
years.
