Palestrante
Descrição
Presently, it is widely accepted that the predominant component of the Universe's matter density is an enigmatic constituent referred to as Dark Matter (DM), believed to consist of a neutral, stable particle, non-baryonic in nature. In dense regions of the Universe, DM may undergo self-annihilation or decay processes, producing distinctive gamma-ray signatures. Particularly, dwarf galaxies, galaxy clusters, and the Galactic Center (GC) are compelling candidates for hosting substantial high-energy gamma-ray signals. The adiabatic growth of a black hole at the center of some of these objects can lead to a significant increase in DM density near the hole, consequently enhancing the expected gamma-ray flux. Notably, the central region of the Milky Way harbors a supermassive black hole (SMBH) known as Sagittarius (Sgr) A* and an observable gamma-ray source named J1745-290, whose position is consistent with the SMBH. In this study we performed a statistical fit of parameters concerning the DM particle and its distribution in the Milky Way. We show that the formation of an adiabatic spike in the GC and the DM self-annihilation "boost" effect around Sgr A* cannot alone explain the observed gamma-ray source in this region, and discuss how the inclusion of background emission from other non-thermal radiative models can account for this emission.
