HAL: in2p3-00023663, version 1

arXiv: astro-ph/0501427

DOI: 10.1051/0004-6361:20052715

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Astronomy and Astrophysics 444 (2005) 327-336

Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

N. Ponthieu1, 2, J.F. Macias-Perez1, M. Tristram1, P. Ade, A. Amblard, R. Ansari3, J. Aumont1, E. Aubourg4, 5, A. Benoît6, J.-Ph. Bernard7, A. Blanchard8, J. J. Bock, F.R. Bouchet9, A. Bourrachot3, P. Camus6, J.-F. Cardoso4, 10, F. Couchot3, P. De Bernardis, J. Delabrouille4, 10, F.-X. Désert11, M. Douspis8, L. Dumoulin12, Ph. Filliatre5, P. Fosalba, M. Giard7, Y. Giraud-Héraud4, 10, R. Gispert2, J. Grain1, L. Guglielmi4, 10, J.-C. Hamilton13, S. Hanany, S. Henrot-Versillé3, J. Kaplan4, 10, G. Lagache2, A. E. Lange, K. Madet6, B. Maffei, S. Masi, F. Mayet1, F. Nati, G. Patanchon, O. Perdereau3, S. Plaszczynski3, M. Piat4, 10, S. Prunet, J.-L. Puget2, C. Renault1, C. Rosset4, 10, D. Santos1, D. Vibert9, D. Yvon4, 5, 10

For the ARCHEOPS collaboration(s)

(2005)

We present the first measurement of temperature and polarization angular power spectra of the diffuse emission of Galactic dust at 353 GHz as seen by Archeops on 20% of the sky. The temperature angular power spectrum is compatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBE maps using \cite{fds} model number 8. For Galactic latitudes $|b| \geq 5$ deg we report a 4 sigma detection of large scale ($3\leq \ell \leq 8$) temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 76\pm 21 \mu\rm{K_{RJ}}^2$ and set upper limits to the $E$ and $B$ modes at $11 \mu\rm{K_{RJ}}^2$. For Galactic latitudes $|b| \geq 10$ deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation $(\ell+1)C_\ell^{TE}/2\pi = 24\pm 13 \mu\rm{K_{RJ}}^2$. These results are then extrapolated to 100 GHz to estimate the contamination in CMB measurements by polarized diffuse Galactic dust emission. The $TE$ signal is then $1.7\pm0.5$ and $0.5\pm0.3 \mu\rm{K^2_{CMB}}$ for $|b| \geq 5$ and 10 deg. respectively. The upper limit on $E$ and $B$ becomes $0.2 \mu\rm{K^2_{CMB}} (2\sigma)$. If polarized dust emission at higher Galactic latitude cuts is similar to the one we report here, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz.

1:	LPSC - Laboratoire de Physique Subatomique et de Cosmologie
2:	IAS - Institut d'astrophysique spatiale
3:	LAL - Laboratoire de l'Accélérateur Linéaire
4:	APC - AstroParticule et Cosmologie
5:	DAPNIA - Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée
6:	CRTBT - Centre de Recherches sur les Très Basses Températures
7:	CESR - Centre d'étude spatiale des rayonnements
8:	LATT - Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées
9:	IAP - Institut d'Astrophysique de Paris
10:	PCC - Physique Corpusculaire et Cosmologie - Collège de France
11:	LAOG - Laboratoire d'Astrophysique de Grenoble
12:	CSNSM - Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse
13:	LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies

Subject(s)

:

Sciences of the Universe/Astrophysics Physics/Astrophysics/Cosmology and Extra-Galactic Astrophysics

Keyword(s) : Cosmic Microwave Background – Cosmology – Observations – Submillimetre – Polarization – Dust – Extinction – Foreground

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From: Simone Lantz <>

Submitted on: Tuesday, 12 December 2006 13:11:53

Updated on: Friday, 9 February 2007 16:17:44