Speaker
Description
Dwarf Spheroidal (dSph) galaxies are very promising laboratories for the indirect search for Dark Matter (DM), due to their low astrophysical background in radio and gamma-ray frequencies.
For the past several decades, the prompt emission from DM annihilation signatures has been explored through modeling and the setting of limits. In addition to the direct annihilation signatures from neutrinos, gamma-rays, electrons, positrons and antimatter, the secondary emission from radiation processes also contributes to the picture. For instance, synchrotron radiation and inverse Compton scattering of charged DM annihilation products such as electrons and positrons can provide a significant signal. The quantitative modeling of this secondary emission with the astrophysical background is necessary to place stringent constraints on the nature of DM.
In this work, the multiwavelength secondary spectrum of DM annihilation for dSph galaxies is calculated using the open-source code CRPropa 3.2., which allows for the self-consistent treatment of the astrophysical background and secondary emissions. We present a systematic comparison of signatures from conventional astrophysical processes to those expected from DM annihilation. The morphological differences between the two scenarios are investigated and tests of the impact of different magnetic fields, DM masses, and DM profiles are performed.
