Ponente
Descripción
In this talk, we present Cherenkov Telescope Array (CTA) prospects for WIMP dark matter (DM) indirect detection through very-high-energy gamma rays originated from DM annihilations in low-mass Galactic DM subhalos. Given their masses, these are not expected to host gas/stars at all and would thus appear in the sky as unidentified gamma-ray sources (unIDs). By using the latest instrumental response functions available, we simulate CTA observations under different array configurations and pointing observation strategies, such as the scheduled CTA Extragalactic Survey. We then predict the sensitivity of CTA to dark subhalos for such scenarios, for which we also use results from N-body cosmological simulations to predict subhalo annihilation fluxes. In the absence of a DM signal, we obtain limits to the DM annihilation cross section as a function of the mass of the WIMP. We do so by also studying and proposing the best type of observation strategy that would be needed in order to derive the best achievable constraints. Our prospects are competitive to those expected for other DM targets, such as dwarf galaxies and galaxy clusters.
