TeV γ-radiation from Dark Matter annihilation in the Galactic center

Recent observations of the Galactic center with ground based gamma-ray instruments (CANGAROO-II, VERITAS, H.E.S.S.) have revealed a TeV (1012eV) gamma-ray signal consistent with the position of SgrA*. The observed energy spectrum and angular distribution of the excess could be explained by a massive Dark Matter candidate with a minimum mass of 12 TeV (90% c.l.) and an upper limit on the WIMP density for r<10pc of (1261M⊙pc−3)(〈σv〉/(3×10−26cm3s−1))−1/2. The angular distribution of the excess events is consistent with a cuspy profile with ρ(r)∝r−α with α>1.0 at a confidence level of 90%. Even though the mass and the cross section of the Dark Matter constituents are unexpectedly high in the framework of most models of non-baryonic Dark Matter, it cannot be ruled out.