Angular Spectra of Polarized Galactic Foregrounds

Abstract

It is believed that magnetic field lines are twisted and bend by turbulent motions in the Galaxy. Therefore, both Galactic synchrotron emission and thermal emission from dust reflects statistics of Galactic turbulence. Our simple model of Galactic turbulence, motivated by results of our simulations, predicts that Galactic disk and halo exhibit different angular power spectra. We show that observed angular spectra of synchrotron emission are compatible with our model. We also show that our model is compatible with the angular spectra of star-light polarization for the Galactic disk. Finally, we discuss how one can estimate polarized microwave emission from dust in the Galactic halo using star-light polarimetry.

11 pages, 1 figure; To be published in the proceedings of "The Cosmic Microwave Background and its Polarization", New Astronomy Reviews, (eds. S. Hanany and K.A. Olive)

References in corpus (3)

• Magnetic Fields via Polarimetry: Progress of Grain Alignment Theory
• Statistics of Velocity from Spectral Data: Modified Velocity Centroids
• The galactic foreground angular spectra

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