›Direct dark matter detection and astrophysical uncertainties

In analyzing data from dark matter direct detection experiments, usually
the Standard Halo Model with a Maxwellian velocity distribution is
assumed. However, very little is known about the dark matter velocity
distribution, and this results in significant uncertainty in interpreting
direct dark matter detection data. In this talk I will present two
different approaches to address this problem. In the first part of my talk
I will discuss astrophysics independent methods, focusing on the
consistency of the inelastic scattering interpretation of the DAMA annual
modulation signal and its tension with the bound from XENON100. In the
second part, I will discuss how to use information from kinematical data
on the Milky Way to constrain the properties of the dark matter phase
space distribution, based on assumptions motivated by the results of
N-body simulations. Finally, I will discuss the impact of astrophysical
uncertainties on the interpretation of direct detection data.