Sensitivity of the Cherenkov Telescope Array to dark subhalos

In this work, we study the potential of Cherenkov Telescope Array (CTA) for detection Galactic dark matter (DM) subhalos. We focus on low-mass subhalos that do not host any baryonic content and therefore lack multiwavelength counterpart. If DM is made weakly interacting massive particles (WIMPs), these may thus appear in gamma-ray sky as unidentified sources. A detailed characterization instrumental response CTA to performed, which use {\it ctools} analysis software simulate observations under different array configurations pointing strategies, such scheduled extragalactic survey. This, together with information subhalo population inferred from N-body cosmological simulations, allows us predict detectability subhalos, i.e., expected number each considered observational scenarios. absence detection, observation strategy set competitive limits annihilation cross section a function particle mass, are at level $\langle\sigma v\rangle\sim4\times10^{-24}$ ($7\times10^{-25}$) $\mathrm{cm^3s^{-1}}$ $b\bar{b}$ ($\tau^+\tau^-$) channel best case scenario. Interestingly, find latter be reached no dedicated observations, obtain by just accumulating exposure time all programs pointings over first 10 years operation. This way will offer most constraining searches intermediate range between $\sim 1-3$ TeV, complementing previous results \textit{Fermi}-LAT HAWC lower higher energies, respectively.