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We propose to test the dark matter (DM) interpretation of the positron excessobserved by the PAMELA cosmic-ray (CR) detector through the identification of aGalactic diffuse gamma-ray component associated to DM-induced prompt andradiative emission. The goal is to present an analysis based on minimal sets ofassumptions and extrapolations with respect to locally testable or measurablequantities. We discuss the differences between the spatial and spectralfeatures for the DM-induced components (with an extended, possibly spherical,source function) and those for the standard CR contribution (with sourcesconfined within the stellar disc), and propose to focus on intermediate andlarge latitudes. We address the dependence of the signal to background ratio onthe model adopted to describe the propagation of charged CRs in the Galaxy, andfind that, in general, the DM-induced signal can be detected by the FermiGamma-ray Space Telescope at energies above 100 GeV. An observational result inagreement with the prediction from standard CR components only, would implyvery strong constraints on the DM interpretation of the PAMELA excess. On theother hand, if an excess in the diffuse emission above 100 GeV is identified,the angular profile for such emission would allow for a clean disentanglementbetween the DM interpretation and astrophysical explanations proposed for thePAMELA excess. We also compare to the radiative diffuse emission at lowerfrequencies, sketching in particular the detection prospects at infraredfrequencies with the Planck satellite.

Testing the Dark Matter Interpretation of the PAMELA Excess through Measurements of the Galactic Diffuse Emission