Abstract
In this work, we present a modelling of the galactic sub-clumps based on statistical estimations of the full Milky Way satellite population. We introduce 10 substructure modellings (SM i , i ∈ {1, … , 10}) with the following varying parameters: a) subhalos inner profile, b) spatial distribution of subhalos, c) mass distribution of subhalos, d) total number of subhalos and e) concentration parameter. The sensitivity curves of CTA for sources in each model are calculated for the τ + τ - and bb̅ decay channels. With both detection of a signal (5σ) with the CTA and no signal observation, no model was effective in accessing the thermal values of 〈σv〉. We analyse the systematic effect introduced by the substructures models.
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