Starts 28 Aug 2018 14:30
Ends 28 Aug 2018 16:00
Central European Time
ICTP
Leonardo Building - Luigi Stasi Seminar Room
Abstract. For simplicity, experimental dark matter (DM) direct detection exclusion curves in the literature are almost always calculated by assuming a naive Standard Halo Model (SHM) expectation for the Milky Way (MW) DM halo. There have been a number of attempts that have tried to go beyond the SHM and assess the impact of astrophysical uncertainties on DM direct detection experiments. Most of these attempts have examined the impact of an uncertain local dark matter density which results in a trivial re-scaling of the exclusion curves. Others have attempted to look at the effect of the DM velocities via changes in the local DM escape speed and the local DM velocity dispersion, or have tried to incorporate the local DM velocity distribution but have mainly restricted to ansatzes or simulations.

We claim that the right approach should be to use an observationally inferred determination, along with the related uncertainties, of the local DM phase-space in a self- consistent manner. In this talk, I will present a detailed look at this fundamentally important element of DM detection results. We start by constructing the MW DM rotation curves and end with re-estimates of the direct detection DM exclusion limits. On the way, we present the tightest constraint on local DM density till date.