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

被引:56
作者
Ponthieu, N
Macías-Pérez, JF
Tristram, M
Ade, P
Amblard, A
Ansari, R
Aumont, J
Aubourg, É
Benoît, A
Bernard, JP
Blanchard, A
Bock, JJ
Bouchet, FR
Bourrachot, A
Camus, P
Cardoso, JF
Couchot, F
de Bernardis, P
Delabrouille, J
Désert, FX
Douspis, M
Dumoulin, L
Filliatre, P
Fosalba, P
Giard, M
Giraud-Héraud, Y
Gispert, R
Grain, J
Guglielmi, L
Hamilton, JC
Hanany, S
Henrot-Versillé, S
Kaplan, J
Lagache, G
Lange, AE
Madet, K
Maffei, B
Masi, S
Mayet, F
Nati, F
Patanchon, G
Perdereau, O
Plaszczynski, S
Piat, M
Prunet, S
Puget, JL
Renault, C
Rosset, C
Santos, D
Vibert, D
机构
[1] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France
[2] Lab Phys Subatom & Cosmol, F-38026 Grenoble, France
[3] Cardiff Univ, Dept Phys, Cardiff CF24 3YB, Wales
[4] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
[5] Lab Accelerateur Lineaire, F-91898 Orsay, France
[6] CEA CE Saclay, DAPNIA, Serv Phys Particules, F-91191 Gif Sur Yvette, France
[7] Univ Paris 07, Federat Rech APC, Paris, France
[8] Ctr Rech Tres Basses Temp, F-38042 Grenoble, France
[9] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France
[10] UPS, OMP, CNRS, Lab Astrophys Tarbes Toulouse,UMR 5572, F-31400 Toulouse, France
[11] CALTECH, Pasadena, CA 91125 USA
[12] Jet Prop Lab, Pasadena, CA 91109 USA
[13] Inst Astrophys, F-75014 Paris, France
[14] Coll France, F-75231 Paris, France
[15] Univ Roma La Sapienza, Dipartimento Fis, Grp Cosmol Sperimentale, I-00185 Rome, Italy
[16] Obs Grenoble, Astrophys Lab, F-38041 Grenoble, France
[17] CSNSM, IN2P3, F-91405 Orsay, France
[18] CEA CE Saclay, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France
[19] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA
[20] Univ Paris 06, LPHNE, F-75252 Paris, France
[21] Univ Paris 07, LPHNE, F-75252 Paris, France
[22] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA
[23] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada
关键词
cosmology : cosmic microwave background; cosmology : observations; polarization; ISM; dust; extinction;
D O I
10.1051/0004-6361:20052715
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 Finkbeiner et al. (1999, ApJ, 524, 867) model number 8. For Galactic latitudes vertical bar b vertical bar >= 5 deg we report a 4 sigma detection of large scale (3 <= l <= 8) temperature-polarization cross-correlation (l + 1) C-l(TE)/2 pi = 76 +/- 21 mu K-RJ(2) and set upper limits to the E and B mode polarization at 11 mu K-RJ(2). For Galactic latitudes vertical bar b vertical bar >= 10 deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation (l + 1)C-l(TE)/2 pi = 24 +/- 13 mu 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 +/- 0.5 and 0.5 +/- 0.3 mu K-CMB(2) for vertical bar b vertical bar >= 5 and 10 deg respectively. The upper limit on E and B mode polarization becomes 0.2 mu K-CMB(2) (2 sigma). If the physical properties of dust radiation on the fraction of the sky observed by Archeops are representative of the whole sky, and if the actual level of E and B mode polarization is close to this upper limit, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz.
引用
收藏
页码:327 / 336
页数:10
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