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Tristram, M.; Patanchon, G.; Macías-Pérez, J. F.; Ade, P.; Amblard, A.; Ansari, R.; Aubourg, É.; Benoît, A.; Bernard, J.-Ph; Blanchard, A.; Bock, J. J.; Bouchet, F. R.; Bourrachot, A.; Camus, P.; Cardoso, J.-F.; Couchot, F.; de Bernardis, P.; Delabrouille, J.; Désert, F.-X.; Douspis, M.; Dumoulin, L.; Filliatre, Ph; Fosalba, P.; Giard, M.; Giraud-Héraud, Y.; Gispert†, R.; Guglielmi, L.; Hamilton, J.-Ch; Hanany, S.; Henrot-Versillé, S.; Kaplan, J.; Lagache, G.; Lamarre, J.-M.; Lange, A. E.; Madet, K.; Maffei, B.; Magneville, Ch; Masi, S.; Mayet, F.; Nati, F.; Perdereau, O.; Plaszczynski, S.; Piat, M.; Ponthieu, N.; Prunet, S.; Renault, C.; Rosset, C.; Santos, D.; Vibert, D.; Yvon, D.
Astronomy & astrophysics, 06/2005, Volume: 436, Issue: 3Journal Article
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.
