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| Title: |
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Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops |
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| Author: |
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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 |
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| Abstract: |
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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. |
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| Collaboration/Project: |
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ARCHEOPS |
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| Document of the type: |
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Article in peer-reviewed journal |
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Publication or writing
date: |
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2005 |
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| Journal: |
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| Astronomy and Astrophysics (Astron. Astrophys.) |
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EDP Sciences |
| ISSN |
0004-6361 (eISSN : 1432-0756) |
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| Volume: |
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444 |
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| Page/Article: |
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327-336 |
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| Copyright: |
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The European Southern Observatory (ESO) 2005 - the original publication is avalaible at http://www.aanda.org |
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| Internal call number: |
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APC-PCC 05-01,LPSC 0502, LAL 05-182 |
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| Keyword(s): |
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Cosmic Microwave Background – Cosmology – Observations – Submillimetre – Polarization – Dust – Extinction – Foreground |
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