In this twofold talk I will first show how it is possible to use Microlensing observations of our Galaxy together with observations of its rotation curve to learn about the distribution of DM. Using this technique it is in fact possible to rule out extreme flavors of NFW or Einasto distribution profiles, as well as obtain an estimate of the local (at Earth and Sun) DM density.
In the second (shorter) part, I will show the updated constraints on DM self-annihilation cross section, obtained with the WMAP7 observations of the CMB.