although DM present thanks to a baryon-like asymmetry could decay only into anti-leptons. Fig. 5b shows that DM decays can fit the PAMELA, FERMI and HESS e ± excesses as well as DM decays, with some minor differences, mostly due to the fact that only in the DM annihilation case a sizable amount of lower-energy e ± can reach us from the Galactic Center, giving rise to a smoother e ± energy spectrum. Decay modes of fermionic DM into W ± µ ∓ or W ± τ ∓ provide good fits to e ± observations, but together with ap excess which is strongly disfavored by PAMELAp observations [2]. Fig. 10 and 11 show that DM interpretations of the PAMELA, FERMI and HESS e ± **data** in terms of leptonic DM decays are compatible with all the constraints we considered, the strongest one being relative to ICS from the '10 • ÷ 20 • ' region observed by FERMI. Other regions (so far observed only by EGRET, with a problematic energy calibration) offer possibly stronger constraints. In the near future FERMI will release **data** in other regions that can be used to constrain this scenario. As discussed in section 3, one can easily extrapolate the fluxes to other regions using the approximations we have employed.