EDP Sciences
Free Access
Volume 436, Number 3, June IV 2005
Page(s) 785 - 797
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361:20042416
Published online 03 June 2005

A&A 436, 785-797 (2005)
DOI: 10.1051/0004-6361:20042416

The CMB temperature power spectrum from an improved analysis of the Archeops data

M. Tristram1, G. Patanchon2, J. F. Macías-Pérez1, P. Ade3, A. Amblard4, R. Ansari5, É. Aubourg6, 7, A. Benoît8, J.-Ph. Bernard9, A. Blanchard10, J. J. Bock11, 12, F. R. Bouchet13, A. Bourrachot5, P. Camus8, J.-F. Cardoso14, F. Couchot5, P. de Bernardis15, J. Delabrouille7, F.-X. Désert16, M. Douspis10, L. Dumoulin17, Ph. Filliatre18, 7, P. Fosalba19, M. Giard9, Y. Giraud-Héraud7, R. Gispert†20, L. Guglielmi7, J.-Ch. Hamilton21, S. Hanany22, S. Henrot-Versillé5, J. Kaplan7, G. Lagache20, J.-M. Lamarre23, A. E. Lange11, K. Madet8, B. Maffei3, Ch. Magneville6, 7, S. Masi15, F. Mayet1, F. Nati15, O. Perdereau5, S. Plaszczynski5, M. Piat7, N. Ponthieu20, S. Prunet13, C. Renault1, C. Rosset7, D. Santos1, D. Vibert13 and D. Yvon6

1  Laboratoire de Physique Subatomique et de Cosmologie, 53 avenue des Martyrs, 38026 Grenoble Cedex, France
    e-mail: reprints@archeops.org;tristram@lpsc.in2p3.fr
2  Department of Physics & Astronomy, University of British Columbia, Vancouver, Canada
3  Cardiff University, Physics Department, PO Box 913, 5, The Parade, Cardiff, CF24 3YB, UK
4  University of California, Berkeley, Dept. of Astronomy, 601 Campbell Hall, Berkeley, CA 94720-3411, USA
5  Laboratoire de l'Accélérateur Linéaire, BP 34, Campus Orsay, 91898 Orsay Cedex, France
6  CEA-CE Saclay, DAPNIA, Service de Physique des Particules, Bât. 141, 91191 Gif-sur-Yvette Cedex, France
7  APC, 11 Pl. M. Berthelot, 75231 Paris Cedex 5, France
8  Centre de Recherche sur les Très Basses Températures, BP 166, 38042 Grenoble Cedex 9, France
9  Centre d'Étude Spatiale des Rayonnements, BP 4346, 31028 Toulouse Cedex 4, France
10  Laboratoire d'Astrophysique de Tarbes Toulouse, 14 avenue E. Belin, 31400 Toulouse, France
11  California Institute of Technology, 105-24 Caltech, 1201 East California Blvd, Pasadena CA 91125, USA
12  Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109, USA
13  Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
14  CNRS-ENST, 46 rue Barrault, 75634 Paris, France
15  Gruppo di Cosmologia Sperimentale, Dipart. di Fisica, Univ. "La Sapienza", PA Moro, 2, 00185 Roma, Italy
16  Laboratoire d'Astrophysique, Obs. de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
17  CSNSM-IN2P3, Bât. 108, 91405 Orsay Campus, France
18  CEA-CE Saclay, DAPNIA, Service d'Astrophysique, Bât. 709, 91191 Gif-sur-Yvette Cedex, France
19  Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr, Honolulu, HI 96822, USA
20  Institut d'Astrophysique Spatiale, Bât. 121, Université Paris XI, 91405 Orsay Cedex, France
21  LPNHE, Universités Paris VI et Paris VII, 4 place Jussieu, Tour 33, 75252 Paris Cedex 05, France
22  School of Physics and Astronomy, 116 Church St. SE, University of Minnesota, Minneapolis MN 55455, USA
23  LERMA, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France

(Received 23 November 2004 / Accepted 16 February 2005 )

We present improved results on the measurement of the angular power spectrum of the Cosmic Microwave Background (CMB) temperature anisotropies using the data from the last ARCHEOPS flight. This refined analysis is obtained by using the 6 most sensitive photometric pixels in the CMB bands centered at 143 and 217 GHz and 20% of the sky, mostly clear of foregrounds. Using two different cross-correlation methods, we obtain very similar results for the angular power spectrum. Consistency checks are performed to test the robustness of these results paying particular attention to the foreground contamination level which remains well below the statistical uncertainties. The multipole range from $\ell=10$ to $\ell=700$ is covered with 25 bins, confirming strong evidence for a plateau at large angular scales (the Sachs-Wolfe plateau) followed by two acoustic peaks centered around $\ell=220$ and $\ell=550$ respectively. These data provide an independent confirmation, obtained at different frequencies, of the WMAP first year results.

Key words: cosmology: cosmic microwave background -- cosmology: observations -- methodes: data analysis

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© ESO 2005

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