The comparison between model and data shows remarkable consistency between the data and our expectations at all bands and for a large area of the sky. In particular, the expected polarization angles of Loop I are compared with those from the real microwave band data of WMAP and Planck. Based on a well known result concerning the magnetic field alignment in supernova explosions, a theoretical expectation is established that the loop polarizations should be predominantly E-mode. I study the polarized emission from Galactic loops, especially Loop I, and mainly focus on the following questions: Does the polarized loop emission contribute predominantly to the E-mode or B-mode? In which frequency bands and in which sky regions can the polarized loop emission be identified? As we revealed in an earlier paper, the E-mode and B-mode of the polarized foreground have noticeably different properties, both in morphology and frequency spectrum, suggesting that they arise from different physicalprocesses, and need to be studied separately.Īims. Improvements of the foreground analysis are therefore necessary. Key laboratory of Particle and Astrophysics, Institute of High Energy Physics, CAS, 19B YuQuan Road, Beijing, PR ChinaĮ-mail: Currently, detection of the primordial gravitational waves using the B-mode of cosmic microwave background (CMB) is primarily limited by our knowledge of the polarized microwave foreground emissions. The Niels Bohr Institute & Discovery Center, Blegdamsvej 17, 2100 Astronomical objects: linking to databases.Including author names using non-Roman alphabets. Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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