Electrons generated by DM lose essentially all their energy via Inverse Compton scattering, e ± γ → e ± γ , on ambient light with average energy E γ ∼ eV. Such scatterings give rise to photons with larger energy E γ ∼ E γ (E e /m e ) 2 ∼ 10 GeV, which is in the energy range being probed by FERMI. As discussed below, this DM ICS γ flux is only marginally affected by astrophysical and DM distribution uncertainties. The reasons for this can be traced back to two observations: (i) Far away from the Galactic Center, the DM uncertainties are relatively mild. (ii) As we will see in Section 4, all DM models that fit the **data** predict roughly the same e ± spectrum, as it is now mostly fixed by the new measurements (given the new FERMI and HESS results). Thereby the DM ICS spectrum is well predicted. As already illustrated in fig. 1 it is not much below the first FERMI diffuse γ-ray data, released for energies ≤ 10 GeV in a specific angular region. Therefore, if the e ± excess is due to DM, FERMI is expected to observe an associated γ excess which is not sensitive to the specific DM model or DM density profile. Whether such an excess is seen or not, will decisively implicate on the DM (or any other mechanisms that produces e ± in a spherical region away from the galactic plane) interpretation of the measured excesses. Alternative scenarios involve e ± generated locally (e.g. by a powerful pulsar) or along the galactic plane (e.g. by supernovae).