Galactic dust polarized emission at high latitudes and CMB polarization

1998/03/13 by Shiv K. Sethi, Sethi, Shiv K., S. Prunet +4
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph

paper · pdf · doi:10.48550/arxiv.astro-ph/9803158

Latex document, 4 pages, 2 figures, to appear in "Fundamental parameters in Cosmology", Rencontres de Moriond, 1998

arxiv created 1998/03/13 · openalex publication_date 1998/03/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

We estimate the dust polarized emission in our galaxy at high galactic latitudes, which is the dominant foreground for measuring CMB polarization using the high frequency instrument (HFI) aboard Planck surveyor. We compare it with the level of CMB polarization and conclude that, for angular scales ≤ 1^∘, the scalar-induced CMB polarization and temperature-polarization cross-correlation are much larger than the foreground level at ν≃ 100 GHz. The tensor-induced signals seem to be at best comparable to the foreground level.

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