Polarized galactic synchrotron and dust emission and their correlation

Abstract

We present an analysis of the level of polarized dust and synchrotron emission using the WMAP9 and Planck data. The primary goal of this study is to inform the assessment of foreground contamination in the cosmic microwave background (CMB) measurements below $\ell \sim 200$ from 23 to 353 GHz. We compute angular power spectra as a function of sky cut based on the Planck 353 GHz polarization maps. Our primary findings are the following. (1) There is a spatial correlation between the dust emission as measured by Planck at 353 GHz and the synchrotron emission as measured by WMAP at 23 GHz with $\rho \approx 0.4$ or greater for $\ell <20$ and $f_{\mathrm{sky}}\ge 0.5$, dropping to $\rho \approx 0.2$ for $30<\ell <200$. (2) A simple foreground model with dust, synchrotron, and their correlation fits well to all possible cross spectra formed with the WMAP and Planck 353 GHz data given the current uncertainties. (3) In the 50$\%$ cleanest region of the polarized dust map, the ratio of synchrotron to dust amplitudes at 90 GHz for 50 $\le \ell \le$110 is $0.3_{-0.2}^{+0.3}$. Smaller regions of sky can be cleaner although the uncertainties in our knowledge of synchrotron emission are larger. A high-sensitivity measurement of synchrotron below 90 GHz will be important for understanding all the components of foreground emission near 90 GHz.

10 pages, 8 figures; Published in JCAP. Source masks updated, minor changes

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• BICEP2 / Keck Array x: Constraints on Primordial Gravitational Waves using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season
• CMB-S4: Forecasting Constraints on Primordial Gravitational Waves
• The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra at 98 and 150 GHz
• Planck 2018 results. XI. Polarized dust foregrounds
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• QUIJOTE scientific results -- IV. A northern sky survey in intensity and polarization at 10-20GHz with the Multi-Frequency Instrument
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• Constraining Cosmic Inflation with Observations: Prospects for 2030
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• Forecast analysis and focal plane optimization for a multi-frequency CMB B-modes polarization experiment: the case of LSPE