characteristics like the observed distribution of spins, ages, and photon fluxes from radio to gamma-rays (e.g., [@Zhang:2004bu]). Here, we wish to demonstrate that with a plausible model for pulsar $e^+e^-$ injection spectra (that is consistent with observations), one can reproduce the WMAP haze. We begin by reviewing the model we utilize for the pulsar $e^+ e^-$ injection spectrum.

We consider only pulsars older than $10^5$ years as potential sources of the $e^+e^-$ pairs that create the haze. This is based on the expectation that young pulsars are surrounded by a nebula created by the kinetic energy released from the supernova explosion (almost $10^{51}$ ergs) so that $e^+e^-$ cannot escape from this nebula until the pulsar is sufficiently old. The nebulae have typical sizes in the parsec range, and since a typical pulsar kick at birth is around $\sim 500$ km/s, it would take the pulsar thousands of years to escape the nebula. In addition, the nebulae themselves thin out in tens of thousands of years. For the mature pulsars, we will assume that the nebulae surrounding pulsars do not play a dominant role in shaping the energy spectrum and we neglect the contributions from pairs diffusing out of younger pulsar 