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

M. Tristram, G. Patanchon, J. F. Macías-Pérez, P. Ade, A. Amblard, R. Ansari, É Aubourg, A. Benoît, J. Ph Bernard, A. Blanchard, J. J. Bock, F. R. Bouchet, A. Bourrachot, P. Camus, J. F. Cardoso, F. Couchot, P. De Bernardis, J. Delabrouille, F. X. Désert, M. DouspisL. Dumoulin, Ph Filliatre, P. Fosalba, M. Giard, Y. Giraud-Héraud, R. Gispert, L. Guglielmi, J. Ch Hamilton, S. Hanany, S. Henrot-Versillé, J. Kaplan, G. Lagache, J. M. Lamarre, A. E. Lange, K. Madet, B. Maffei, Ch Magneville, S. Masi, F. Mayet, F. Nati, O. Perdereau, S. Plaszczynski, M. Piat, N. Ponthieu, S. Prunet, C. Renault, C. Rosset, D. Santos, D. Vibert, D. Yvon

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51 Scopus citations

Abstract

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 ℓ = 10 to ℓ = 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 ℓ = 220 and ℓ = 550 respectively. These data provide an independent confirmation, obtained at different frequencies, of the WMAP first year results.

Original languageEnglish (US)
Pages (from-to)785-797
Number of pages13
JournalAstronomy and Astrophysics
Volume436
Issue number3
DOIs
StatePublished - Jun 2005

Keywords

  • Cosmology: cosmic microwave background
  • Cosmology: observations
  • Methodes; data analysis

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