Right: Very-high-enegy (E>100 GeV) gamma-ray sky map of the Galactic Centre region seen by H.E.S.S. from 10 year observations with H.E.S.S. phase I
Bottom: Constraints (95% C.L.) on the velocity-weighted annihilation cross section as a function of the WIMP mass for the W+W- (bottom right) and tau+tau- annihilation channels, from observations taken over 10 years of the inner 300 pc of the GC region with H.E.S.S. The dark matter distribtuion assmes to follow a Einsato profile.
Top: Very-high-enegy (E>100 GeV) gamma-ray image of the Galactic Centre seen by H.E.S.S. (logarithmic scale). The black lines outline the regions used to calculate the cosmic-ray energy density throughout
the central molecular zone. White contour lines indicate the density distribution of molecular gas, as traced by its CS line emission30. Black star, location of the supermassicve black hole Sgr A* .
Left: Spatial distribution of the cosmic-ray density above 10 TeV versus projected distance from Sgr A*. The vertical and horizontal error bars show the 1σ statistical plus systematic errors and the bin size, respectively. The 1/r radial profile is clearly preferred for the HESS data.
Strongest contraints on the velocity-weighted annihilation cross section versus the WIMP mass. The H.E.S.S. 2016 constraints from Galactic Center observations together with those from Fermi observations of dwarf galaxy satellites of the Milky Way are potted. Conservative H.E.S.S. 2018 and CTA sensitivities are shown. Figure adapted from the CTa dark matter programme of the CTA Science Technical Design Report.