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abstract: 'The WMAP haze is an excess in the 22 to 93 GHz frequency bands of WMAP extending about 10 degrees from the galactic center. We show that synchrotron emission from electron-positron pairs injected into the interstellar medium by the galactic population of pulsars with energies in the 1 to 100 GeV range can explain the frequency spectrum of the WMAP haze and the drop in the average haze power with latitude. The same spectrum of high energy electron-positron pairs from pulsars, which gives rise to the haze, may also generate the observed excesses in AMS, HEAT and PAMELA. We discuss the spatial morphology of the pulsar synchrotron signal and its deviation from spherical symmetry, which may provide an avenue to determine the pulsar contribution to the haze.'
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MCTP-09-12\

Pulsars as a Source of the WMAP Haze\

Manoj Kaplinghat$^{a}$, Daniel J. Phalen$^{b}$, and Kathryn M. Zurek$^{b,c}$\

$^a$ Center for Cosmology, Department of Physics and Astronomy\
University of California, Irvine, CA, USA\
${^b}$ Department of Physics, University of Michigan\
Ann Arbor, Michigan 48109, USA\
$^c$ Particle Astrophysics Center, Fermi National Accelerator Laboratory\
Batavia, Illinois 60510, USA

Introduction
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The measurements of the temperature anisotropies in the Cosmic Microwave Background 