Galactic dust polarized emission at high latitudes and CMB polarization

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DC Field	Value	Language
dc.contributor.author	Sethi, S.K.	-
dc.contributor.author	Prunet, S.	-
dc.contributor.author	Bouchet, F.R.	-
dc.date.accessioned	2012-07-14T10:13:35Z	-
dc.date.available	2012-07-14T10:13:35Z	-
dc.date.issued	1998-03	-
dc.identifier.citation	Astronomy and Astrophysics, 1998, Vol.339, p187	en
dc.identifier.issn	0004-6361	-
dc.identifier.issn	1432-0746 (Online)	-
dc.identifier.uri	http://hdl.handle.net/2289/4924	-
dc.description	Open Access	en
dc.description.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 $\le 1^{\circ}$, the scalar-induced CMB polarization and temperature-polarization cross-correlation are much larger than the foreground level at $\nu \simeq 100 GHz$. The tensor-induced signals seem to be at best comparable to the foreground level.}	en
dc.language.iso	en	en
dc.publisher	EDP Sciences	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1998astro.ph..3158S	en
dc.relation.uri	http://arxiv.org/abs/astro-ph/9803158	en
dc.relation.uri	http://dx.doi.org/	en
dc.rights	1998 EDP Sciences	en
dc.title	Galactic dust polarized emission at high latitudes and CMB polarization	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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