Abstract
If coming from WIMP annihilation, the excess of electrons/positrons observed by the Pamela/ATIC/Fermi experiments gives rise to a noticeable amount of synchrotron and Inverse Compton Scattering (ICS) radiation around 10–100 GeV when the e +e − interact with the Galactic Magnetic Field, and the InterStellar Radiation Field (ISRF). Further, the Pamela/ATIC/Fermi excess can be tested through the shape of the ICS signal, which is expected to show a peculiar and clean “ICS Haze” feature. We discuss the constraints coming from radio observations, as well as the implications of some preliminary Fermi results on the diffuse gamma background in the inner galactic region.
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