dark matter models. The energy range of Fermi-LAT is also ideally suited to probing secluded WIMP annihilation with masses of a few hundred GeV, where Milagro loses its sensitivity.

It is also possible for long-lived mediators to decay predominantly to electrons and positrons. It is tempting then to consider the implications of these decays in relation to the anomalous positrons fraction observed by PAMELA. As far as we are aware detailed timing and directional analyses have not yet been performed, leaving open the possibility of an intriguing local explanation for these anomalies within the dark matter framework. Given that the existing magnetic fields affect propagation, and the decay chains of the mediators are model-dependent, one could in principle fit the spectral shapes of the observed signals. We have obtained a rough estimate of the required integrated signal flux by using Fermi electron data with an $\sim E^{-3}$ spectrum to infer an estimate of the background and incorporating a new source with a harder power-law spectrum. Depending on the source as well as where the signal turns on (i.e. how large a component of the PAMELA signal) we find a required flux of \_[e\^+e\^-]{}(E&gt;10   [GeV]{}) \~10\^[-4]{} - 10\^[-6]{}  [cm]{}\^[-2]{} [s]{}\^[-1]{} \[interesting\] 