Pulsars as a Source of the WMAP Haze Kathryn Zurek Fermilab - PowerPoint PPT Presentation

Pulsars as a Source of the WMAP Haze Kathryn Zurek Fermilab Kaplinghat, Phalen, KMZ, arXiv: 0905.0487

Excess cosmic ray electrons Fermi ATIC PAMELA

DM model building fury Problematic with anti- protons gamma rays Cirelli et al Meade et al

But, really just ordinary astrophysics? Possible sources: Blasi Pulsars? Hooper, Blasi, Serpico Secondary e + production in e - e - supernova Biermann et al remnant? New additional acceleration mechanism?

Excess electrons from astrophysical objects Produced at sources Diffuse outwards, lose energy Radiate in magnetic field e + e + WMAP Haze? Gamma Rays (Inverse Compton on starlight) Synchrotron (magnetic field)

The WMAP Haze Is it there? Finkbeiner Finkbeiner and Dobler 2007 Lots of background synchrotron radiation, from dust What causes it? DM annihilation to charged byproducts χ χ which radiate in magnetic field? W - W +

The WMAP Haze from DM Ω c h 2 = 0 . 114 ± 0 . 003 Magic thermal annihilation cross-section 1 TeV 2 ≈ 3 × 10 − 26 cm 3 g 4 Gets right relic σ v ≈ s density Density profile, Magnetic field profile, ratio of energy But annihilation lost by inverse Compton to cross-section synchrotron quite dialable Several orders of magnitude in cross-section

WMAP Haze from Astrophysical Electrons? Total flux of synchrotron Angular profile from galactic center Frequency band dn e dependence ∝ E − α e dE e Morphology -- approximately spherical

WMAP Haze from Astrophysical Electrons? Pulsar contribution Total flux of synchrotron Angular profile from galactic center Frequency band dependence Morphology -- approximately spherical

WMAP Haze from Astrophysical Electrons? Pulsar contribution Total flux of synchrotron Angular profile from galactic center Frequency band dependence Morphology -- approximately spherical

WMAP Haze from Astrophysical Electrons? Pulsar contribution Total flux of synchrotron Angular profile from galactic center Not published for fits Frequency band dependence Morphology -- approximately Courtesy of spherical G. Dobler

WMAP Haze from Astrophysical Electrons? Pulsar contribution Total flux of synchrotron 0 − | z | /z 0 + B 1 B ( r, z ) = B 0 e − r/r ′ r ′ 0 << r 0 Angular profile from galactic center Not published for fits Frequency band dependence Morphology -- approximately Roughly spherical spherical?

Summary Pulsars are a good possible source of the positron excesses observed by PAMELA and Fermi The electron flux and energy distribution from pulsar production well produces Haze flux and spectrum Morphology needs to be further studied; subject to many astrophysical uncertainties such as B-field and pulsar distribution