Gammaldi, VivianaÁvila-Reese, V.Valenzuela, O.González-Morales, A.X.2023-06-172023-06-172016-12-222470-001010.1103/PhysRevD.94.121301https://hdl.handle.net/20.500.14352/17767© 2016 American Physical Society. This work has been supported by Beca Iberoamérica Jóvenes Profesores e Investigadores by Santander Universidades, by the Ministerio de Economía, Industria y Competividad (Spain) Project No. FIS2014-52837-P and Consolider-Ingenio Multimessenger Approach to Dark Matter (MULTIDARK) CSD2009-00064 and partially by the Horizon 2020 Coordination & Support Action (H2020 CSA) Twinning Project No. 692194, Ruder Boskovic Institute (RBI) Twinning, and QGSKY. V. G. is grateful to P. Ullio for useful discussions and to the Mainz Institute for Theoretical Physics for its hospitality and its partial support during the completion of this work. A. X. G. M. acknowledges the CATEDRA Consejo Nacional de Ciencia y Tecnología (CONACYT/ CONACyT) program, the University of California Institute for Mexico and the United States (UCMEXUS) collaborative project, and the Universidad de Guanajuato (UGTO) basic science Project No. 878/2016. O. V. acknowledges CONACyT/Fronteras de la Ciencias 281. The authors also acknowledge S. Roca-Fabrega and B. Villaseñor for providing the Garrotxa simulation data and fits, and M. Schaller for providing the fit parameters of the APOSTLEEAGLE simulations.We analyze the possibility that the HESS γ-ray source at the Galactic center could be explained as the secondary flux produced by annihilation of TeV dark matter (DM) particles with locally enhanced density, in a region spatially compatible with the HESS observations themselves. We study the inner 100 pc considering (i) the extrapolation of several density profiles from state-of-the-art N-body þ hydrodynamics simulations of Milky Way-like galaxies, (ii) the DM spike induced by the black hole, and (iii) the DM particles scattering off by bulge stars. We show that in some cases the DM spike may provide the enhancement in the flux required to explain the cutoff in the HESS J1745-290γ-ray spectra as TeV DM. In other cases, it may help to describe the spatial tail reported by HESS II at angular scales ≲0.54° toward Sgr A*.engjournal articlehttp://dx.doi.org/10.1103/PhysRevD.94.121301https://journals.aps.orgopen access53Galactic-centerHigh-energyCosmological simulationsContractionDirectionGalaxiesBaryonsCoresHalosMassFísica-Modelos matemáticos