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Recent full-sky maps of the Galaxy from the Fermi Gamma-Ray Space Telescopehave revealed a diffuse component of emission towards the Galactic center andextending up to roughly +/-50 degrees in latitude. This Fermi "haze" is theinverse Compton emission generated by the same electrons which generate themicrowave synchrotron haze at WMAP wavelengths. The gamma-ray haze has twodistinct characteristics: the spectrum is significantly harder than emissionelsewhere in the Galaxy and the morphology is elongated in latitude withrespect to longitude with an axis ratio ~2. If these electrons are generatedthrough annihilations of dark matter particles in the Galactic halo, thismorphology is difficult to realize with a standard spherical halo and isotropiccosmic-ray diffusion. However, we show that anisotropic diffusion along orderedmagnetic field lines towards the center of the Galaxy coupled with a prolatedark matter halo can easily yield the required morphology without makingunrealistic assumptions about diffusion parameters. Furthermore, a Sommerfeldenhancement to the self annihilation cross-section of ~30 yields a good fit tothe morphology, amplitude, and spectrum of both the gamma-ray and microwavehaze. The model is also consistent with local cosmic-ray measurements as wellas CMB constraints.

The Fermi Gamma-Ray Haze from Dark Matter Annihilations and Anisotropic Diffusion