Pulsars as the Source of the WMAP Haze

Details Pulsars as the Source of the WMAP Haze Pulsars as the Source of the WMAP Haze

2009-05-05

arxiv.org/abs/0905.0487v2

JCAP 0912:010,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

18 pages, 4 figures. Corrected errors in fig 1-3 and added discussion of the detailed spatial morphology of the haze signal

Scientific paper

10.1088/1475-7516/2009/12/010

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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