Constraints on dark matter annihilation in Milky Way halo from spherical harmonics of Fermi gamma-rays

          @misc{ scivideos_PIRSA:11020115,
            doi = {10.48660/11020115},
            url = {https://pirsa.org/11020115},
            author = {Malyshev, Dmitry},
            keywords = {Particle Physics},
            language = {en},
            title = {Constraints on dark matter annihilation in Milky Way halo from spherical harmonics of Fermi gamma-rays},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2011},
            month = {feb},
            note = {PIRSA:11020115 see, \url{https://scivideos.org/pirsa/11020115}}
          }
          

Abstract

Gamma-ray production by dark matter annihilation is one of the most universal indirect dark matter signals. In order to avoid intensive astrophysical background, one can study the gamma-rays away from the Galactic plane. The problems is that the dark matter annihilation signal at high latitudes is smooth and most probably subdominant to Galactic and extragalactic fluxes. I will discuss the use of spherical harmonics decomposition as a tool to distinguish a large scale small amplitude dark matter signal from astrophysical fluxes. The sensitivity of this method for currently available Fermi data is similar to the signal from thermal WIMP dark matter annihilation into W+W- or b-bbar.