GeV such that there will be enough radiation into the 93 GHz band, however cutoff energies larger than that will only serve to increase the required average efficiency per pulsar to reproduce the haze. Additionally, a soft spectrum, corresponding to a large $\alpha$, will not give rise to a large enough amplitude in the high frequency bands to reproduce the haze. Lastly, the fit in the angular direction results by allowing the characteristic distance over which the magnetic field is damped from the galactic center, $z_b$ in Eq. \[eq:B-field\], to vary.

As shown in Fig. \[fig:E100alpha1p6\], we find that with reasonable choices of these parameters, a galactic source of pulsars can explain both the amplitude and frequency dependence of the WMAP haze. The plotted synchrotron fluxes are averages over 20 degrees in longitude for below the galactic plane. We find that $z_b = 2$ kpc gives a good fit to the angular distribution. In detail, the shape of the haze depends on both the distribution of the injected pairs as well as the magnetic field profile. Future Planck data might provide an avenue to constrain these distributions better.

The cutoff energy ${E_{\rm cut}}= 100$ GeV taken from the CZ01 model 