English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Context: Currently, detection of the primordial gravitational waves by theB-mode of Cosmic Microwave Background (CMB) is primarily limited by ourknowledge of the polarized microwave foreground emissions. Thus improvements ofthe foreground analysis are necessary. As revealedin~\cite{2018arXiv180410382L}, the E-mode and B-mode of the polarizedforeground have noticeable different properties, both in morphology andfrequency spectrum, suggesting that they arise from different physicalprocesses, and need to be studied separately.  Aims: I will study the polarized emission from Galactic loops, especiallyLoop I, and mainly focus on the following issues: Does it contributepredominantly to the E-mode or B-mode? In which frequency bands and in whichsky regions can it be identified?  Methods: Based on a well known result about the magnetic field alignment insupernova explosions, a theoretical expectation is established that the looppolarizations should be predominantly E-mode. In particular, the expectedpolarization angles of Loop I are compared with those from the real microwaveband data of WMAP and Planck.  Results and conclusions: The comparison between model and data showsremarkable consistency between data and expectation at all bands and for alarge area of the sky. This result suggests that the polarized emission ofGalactic Loop I is a major polarized component in all microwave bands from 23to 353 GHz, and a considerable part of the polarized foreground is likelyoriginated from a local bubble associated with Loop I, instead of the far moredistant Galactic emission. The result also provides a possible way to explainthe reported E-to-B excess~\citep{2016A&A...586A.133P} by contribution of theloops. Finally, this work may also provide the first geometrical evidence thatthe Earth was hit by a supernova explosion.

Fingerprint of Galactic Loop I on polarized microwave foregrounds