work [@Cumberbatch:2009ji] has claimed that the significance of the WMAP haze may depend on the assumptions about the spatial variation of the synchrotron spectral index.

This signal may be even more interesting in light of the recent observations of an excess of high energy cosmic ray positrons and electrons. The excess was originally observed by the HEAT [@HEAT] and AMS [@AMS] experiments, and was confirmed more recently by the PAMELA [@PAMELA] and PPB-BETs [@PPB-BETs] experiments. The Fermi Large Area Telescope also observes excess cosmic ray electrons and positrons over the predicted background [@Fermi], though their excess is not nearly as large as that observed by ATIC [@ATIC] (and seems to indicate that the ATIC excess is instrumental in origin). The source of these positrons is unknown, however, there are several possibilities. Like the WMAP haze, they may be explained by annihilating DM (see [*e.g.*]{} [@Cirelli; @HooperWeiner]). An explanation of the signal in terms of annihilating dark matter (DM), however, has multiple obstacles to overcome. First, it must annihilate with a cross-section significantly larger than that suggested by the thermal abundance, $\sigma v \simeq 3 \times 10^{-24-23} \mbox{
  cm}^3/\mbox{s}$. Second, the DM candidate prefers leptophilic annihilation to avoid overproducing anti-protons [@Cirelli; 