Abstract. The dark matter (DM) density profile in the Milky Way is determined using kinematic tracers of the total gravitational potential and observational inferred three-dimensional density profiles of the visible component (stars and gas). I will show that the accuracy on the reconstructed DM density in the Solar neighbourhood is better than 10%, while the inner DM density slope is poorly reconstructed. I will also show how this data-driven analysis can be used in the interpretation of results from indirect/direct DM searches.
(The slides will be available here)