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

The polarized thermal emission from Galactic dust is the main foregroundpresent in measurements of the polarization of the cosmic microwave background(CMB) at frequencies above 100GHz. We exploit the Planck HFI polarization datafrom 100 to 353GHz to measure the dust angular power spectra $C_\ell^{EE,BB}$over the range $40<\ell<600$ well away from the Galactic plane. These willbring new insights into interstellar dust physics and a precise determinationof the level of contamination for CMB polarization experiments. We show thatstatistical properties of the emission can be characterized over largefractions of the sky using $C_\ell$. For the dust, they are well described bypower laws in $\ell$ with exponents $\alpha^{EE,BB}=-2.42\pm0.02$. Theamplitudes of the polarization $C_\ell$ vary with the average brightness in away similar to the intensity ones. The dust polarization frequency dependenceis consistent with modified blackbody emission with $\beta_d=1.59$ and$T_d=19.6$K. We find a systematic ratio between the amplitudes of the Galactic$B$- and $E$-modes of 0.5. We show that even in the faintest dust-emittingregions there are no "clean" windows where primordial CMB $B$-mode polarizationcould be measured without subtraction of dust emission. Finally, we investigatethe level of dust polarization in the BICEP2 experiment field. Extrapolation ofthe Planck 353GHz data to 150GHz gives a dust power$\ell(\ell+1)C_\ell^{BB}/(2\pi)$ of $1.32\times10^{-2}\mu$K$_{CMB}^2$ over the$40<\ell<120$ range; the statistical uncertainty is $\pm0.29$ and there is anadditional uncertainty (+0.28,-0.24) from the extrapolation, both in the sameunits. This is the same magnitude as reported by BICEP2 over this $\ell$ range,which highlights the need for assessment of the polarized dust signal even inthe cleanest windows of the sky.

Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes