Uncertainties in measuring the dark matter signal from Milky Way satellites using Cherenkov telescopes

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 $\in$ {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 ${\tau }^{+}{\tau }^{-}$ and $b\bar{b}$ annihilation channels. With both detection of a signal (5$\sigma$) with the CTA and no signal observation, no model was effective in accessing the thermal values of <$\sigma$ v>. We analyse the systematic effects introduced by the substructures models.

15 pages, 5 figures

References in corpus (9)

• Beasts of the Southern Wild: Discovery of nine Ultra Faint satellites in the vicinity of the Magellanic Clouds
• The Local Dark Matter Density
• A universal model for halo concentrations
• The Luminosity Function of the Milky Way Satellites
• GammaLib and ctools: A software framework for the analysis of astronomical gamma-ray data
• Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout
• Modeling dark matter subhalos in a constrained galaxy: Global mass and boosted annihilation profiles
• Einasto Profiles and the Dark Matter Power Spectrum
• Sensitivity of the Cherenkov Telescope Array to dark subhalos