possibility that the WMAP haze may also be generated by $e^+ e^-$ pair production in pulsars. Pulsars produce a significant flux of energetic electrons and positrons spread over the disk of the galaxy, which then emit synchrotron radiation as they traverse outward from the disk in the magnetic field of the galaxy. To explain the haze, the expected signal from pulsars must both reproduce angular dependence of the signal from the galactic center, as well as the frequency dependence through the WMAP bands from 22 to 93 GHz. We show that an energy spectrum which is typical of that necessary for explaining the PAMELA data with pulsars also naturally produces the average variation of WMAP haze with latitude given typical galactic magnetic fields and diffusion parameters. We also discuss reproducing the detailed morphology of the WMAP haze.

In the next section we describe the model for the electron distribution from mature galactic pulsars, and in the following section their propagation through the ISM and the haze calculation.

Injection spectrum of positrons from pulsars
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The mechanism by which pulsars produce electrons and positrons and details about their energy distribution are not very well understood. However, the theoretical models reproduce important 