Determining the Distribution of Dark Matter in the Milky Way
Maria Benito Castaño, ICTP Sao Paolo
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)