  Mapping the dark matter distribution across our Galaxy represents a central
challenge for the near future as a new generation of space-borne and
ground-based astronomical surveys swiftly comes online. Here we present a
synopsis of the present status of the field, reviewing briefly the baryonic
content and the kinematics of the Milky Way and outlining the methods used to
infer the dark matter component. The discussion then proceeds with some of the
latest developments based on our own work. In particular, we present a new
compilation of kinematic measurements tracing the rotation curve of the Galaxy
and an exhaustive array of observation-based baryonic models setting the
contribution of stellar bulge, stellar disc and gas to the total gravitational
potential. The discrepancy between these two components is then quantified to
derive the latest constraints on the dark matter distribution and on modified
Newtonian dynamics. We shall end with an overview of future directions to
improve our mapping of the dark matter distribution in the Milky Way.
