Query : 2015MNRAS.451L..90T

2015MNRAS.451L..90T - Mon. Not. R. Astron. Soc., 451, L90-L94 (2015/July-3)

Searching for inflationary B modes: can dust emission properties be extrapolated from 350 GHz to 150 GHz?


Abstract (from CDS):

Recent Planck results have shown that radiation from the cosmic microwave background passes through foregrounds in which aligned dust grains produce polarized dust emission, even in regions of the sky with the lowest level of dust emission. One of the most commonly used ways to remove the dust foreground is to extrapolate the polarized dust emission signal from frequencies where it dominates (e.g. ∼ 350 GHz) to frequencies commonly targeted by cosmic microwave background experiments (e.g. ∼ 150 GHz). In this Letter, we describe an interstellar medium effect that can lead to decorrelation of the dust emission polarization pattern between different frequencies due to multiple contributions along the line of sight. Using a simple 2-cloud model we show that there are two conditions under which this decorrelation can be large: (a) the ratio of polarized intensities between the two clouds changes between the two frequencies; (b) the magnetic fields between the two clouds contributing along a line of sight are significantly misaligned. In such cases, the 350 GHz polarized sky map is not predictive of that at 150 GHz. We propose a possible correction for this effect, using information from optopolarimetric surveys of dichroicly absorbed starlight.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): polarization - dust, extinction - ISM: magnetic fields - cosmic background radiation - cosmology: observations - inflation

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 185 1
2 HRK 135.3+54.5 Cld 11 51 39 +61 13.3           ~ 23 0
3 NAME Leo Cloud Cld ~ ~           ~ 60 0

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