Speaker
Description
Weak-scale Dark Matter (DM) particles annihilating into lepton-rich channels in the Galaxy not only produce $\gamma$-rays via prompt radiation, but also generate abundant energetic $e^\pm$, which subsequently emit through inverse Compton scattering or bremsstrahlung (collectively called `secondary-radiation photons'). While the prompt $\gamma$-rays concentrate at high-energy, the secondary emission falls in the MeV range, which a number of upcoming experiments (e.g., AMEGO, E-ASTROGAM and MAST) will be able to probe. I shall discuss the sensitivity of these future telescopes for weak-scale DM, focusing for definiteness on observations of the galactic center. I shall show that they have the potential of probing a wide region of the DM parameter space which is currently unconstrained, precisely thanks to the significant leverage provided by their sensitivity to secondary emissions. I shall also comment on astrophysical and methodological uncertainties, and compare with the reach of future high-energy $\gamma$-ray experiments.
