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The excess of electrons/positrons observed by the Pamela and ATIC experimentsgives rise to a noticeable amount of synchrotron and Inverse Compton Scattering(ICS) radiation when the e^+e^- interact with the Galactic Magnetic Field, andthe InterStellar Radiation Field (ISRF). In particular, the ICS signal producedwithin the WIMP annihilation interpretation of the Pamela/ATIC excess showsalready some tension with the EGRET data. On the other hand, 1 yr of Fermi datataking will be enough to rule out or confirm this scenario with a highconfidence level. The ICS radiation produces a peculiar and clean "ICS Haze"feature, as well, which can be used to discriminate between the astrophysicaland Dark Matter scenarios. This ICS signature is very prominent even severaldegrees away from the galactic center, and it is thus a very robust predictionwith respect to the choice of the DM profile and the uncertainties in the ISRF.

Secondary radiation from the Pamela/ATIC excess and relevance for Fermi