Planck 2013 results. XV. CMB power spectra and likelihood
Creators: name: Planck Collaboration
name: Ade, P. A. R.
name: Aghanim, N.
name: Armitage-Caplan, C.
name: Arnaud, M.
name: Ashdown, M.
name: Atrio-Barandela, F.
name: Aumont, J.
name: Baccigalupi, C.
name: Banday, A. J.
name: Barreiro, R. B.
name: Bartlett, J. G.
name: Battaner, E.
name: Benabed, K.
name: Benoit, A.
name: Benoit-Levy, A.
name: Bernard, J. -P.
name: Bersanelli, M.
name: Bielewicz, P.
name: Bobin, J.
name: Bock, J. J.
name: Bonaldi, A.
name: Bonavera, L.
name: Bond, J. R.
name: Borrill, J.
name: Bouchet, F. R.
name: Boulanger, F.
name: Bridges, M.
name: Bucher, M.
name: Burigana, C.
name: Butler, R. C.
name: Calabrese, E.
name: Cardoso, J. -F.
name: Catalano, A.
name: Challinor, A.
name: Chamballu, A.
name: Chiang, L. -Y
name: Chiang, H. C.
name: Christensen, P. R.
name: Church, S.
name: Clements, D. L.
name: Colombi, S.
name: Colombo, L. P. L.
name: Combet, C.
name: Couchot, F.
name: Coulais, A.
name: Crill, B. P.
name: Curto, A.
name: Cuttaia, F.
name: Danese, L.
name: Davies, R. D.
name: Davis, R. J.
name: de Bernardis, P.
name: de Rosa, A.
name: de Zotti, G.
name: Delabrouille, J.
name: Delouis, J. -M.
name: Desert, F. -X.
name: Dickinson, C.
name: Diego, J. M.
name: Dole, H.
name: Donzelli, S.
name: Dore, O.
name: Douspis, M.
name: Dunkley, J.
name: Dupac, X.
name: Efstathiou, G.
name: Elsner, F.
name: Ensslin, T. A.
name: Eriksen, H. K.
name: Finelli, F.
name: Forni, O.
name: Frailis, M.
name: Fraisse, A. A.
name: Franceschi, E.
name: Gaier, T. C.
name: Galeotta, S.
name: Galli, S.
name: Ganga, K.
name: Giard, M.
name: Giardino, G.
name: Giraud-Heraud, Y.
name: Gjerlow, E.
name: Gonzalez-Nuevo, J.
name: Gorski, K. M.
name: Gratton, S.
name: Gregorio, A.
name: Gruppuso, A.
name: Gudmundsson, J. E.
name: Hansen, F. K.
name: Hanson, D.
name: Harrison, D.
name: Helou, G.
name: Henrot-Versille, S.
name: Hernandez-Monteagudo, C.
name: Herranz, D.
name: Hildebrandt, S. R.
name: Hivon, E.
name: Hobson, M.
name: Holmes, W. A.
name: Hornstrup, A.
name: Hovest, W.
name: Huffenberger, K. M.
name: Hurier, G.
name: Jaffe, T. R.
name: Jaffe, A. H.
name: Jewell, J.
name: Jones, W. C.
name: Juvela, M.
name: Keihanen, E.
name: Keskitalo, R.
name: Kiiveri, K.
name: Kisner, T. S.
name: Kneissl, R.
name: Knoche, J.
name: Knox, L.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Lagache, G.
name: Lahteenmaki, A.
name: Lamarre, J. -M.
name: Lasenby, A.
name: Lattanzi, M.
name: Laureijs, R. J.
name: Lawrence, C. R.
name: Jeune, M. Le
name: Leach, S.
name: Leahy, J. P.
name: Leonardi, R.
name: Leon-Tavares, J.
name: Lesgourgues, J.
name: Liguori, M.
name: Lilje, P. B.
name: Lindholm, V.
name: Linden-Vornle, M.
name: Lopez-Caniego, M.
name: Lubin, P. M.
name: Macias-Perez, J. F.
name: Maffei, B.
name: Maino, D.
name: Mandolesi, N.
name: Marinucci, D.
name: Maris, M.
name: Marshall, D. J.
name: Martin, P. G.
name: Martinez-Gonzalez, E.
name: Masi, S.
name: Matarrese, S.
name: Matthai, F.
name: Mazzotta, P.
name: Meinhold, P. R.
name: Melchiorri, A.
name: Mendes, L.
name: Menegoni, E.
name: Mennella, A.
name: Migliaccio, M.
name: Millea, M.
name: Mitra, S.
name: Miville-Deschenes, M. -A.
name: Molinari, D.
name: Moneti, A.
name: Montier, L.
name: Morgante, G.
name: Mortlock, D.
name: Moss, A.
name: Munshi, D.
name: Naselsky, P.
name: Nati, F.
name: Natoli, P.
name: Netterfield, C. B.
name: Norgaard-Nielsen, H. U.
name: Noviello, F.
name: Novikov, D.
name: Novikov, I.
name: O'Dwyer, I. J.
name: Orieux, F.
name: Osborne, S.
name: Oxborrow, C. A.
name: Paci, F.
name: Pagano, L.
name: Pajot, F.
name: Paladini, R.
name: Paoletti, D.
name: Partridge, B.
name: Pasian, F.
name: Patanchon, G.
name: Paykari, P.
name: Perdereau, O.
name: Perotto, L.
name: Perrotta, F.
name: Piacentini, F.
name: Piat, M.
name: Pierpaoli, E.
name: Pietrobon, D.
name: Plaszczynski, S.
name: Pointecouteau, E.
name: Polenta, G.
name: Ponthieu, N.
name: Popa, L.
name: Poutanen, T.
name: Pratt, G. W.
name: Prezeau, G.
name: Prunet, S.
name: Puget, J. -L.
name: Rachen, J. P.
name: Rahlin, A.
name: Rebolo, R.
name: Reinecke, M.
name: Remazeilles, M.
name: Renault, C.
name: Ricciardi, S.
name: Riller, T.
name: Ringeval, C.
name: Ristorcelli, I.
name: Rocha, G.
name: Rosset, C.
name: Roudier, G.
name: Rowan-Robinson, M.
name: Rubino-Martin, J. A.
name: Rusholme, B.
name: Sandri, M.
name: Sanselme, L.
name: Santos, D.
name: Savini, G.
name: Scott, D.
name: Seiffert, M. D.
name: Shellard, E. P. S.
name: Spencer, L. D.
name: Starck, J. -L.
name: Stolyarov, V.
name: Stompor, R.
name: Sudiwala, R.
name: Sureau, F.
name: Sutton, D.
name: Suur-Uski, A. -S.
name: Sygnet, J. -F.
name: Tauber, J. A.
name: Tavagnacco, D.
name: Terenzi, L.
name: Toffolatti, L.
name: Tomasi, M.
name: Tristram, M.
name: Tucci, M.
name: Tuovinen, J.
name: Turler, M.
name: Valenziano, L.
name: Valiviita, J.
name: Van Tent, B.
name: Varis, J.
name: Vielva, P.
name: Villa, F.
name: Vittorio, N.
name: Wade, L. A.
name: Wandelt, B. D.
name: Wehus, I. K.
name: White, M.
name: White, S. D. M.
name: Yvon, D.
name: Zacchei, A.
name: Zonca, A.
Publisher: name: arXiv
Year: 2013
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present the Planck likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations. We use this likelihood to derive the Planck CMB power spectrum over three decades in l, covering 2 &lt;= l &lt;= 2500. The main source of error at l &lt;= 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher l's. For l &lt; 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz through a physically motivated Bayesian component separation technique. At l &gt;= 50, we employ a correlated Gaussian likelihood approximation based on angular cross-spectra derived from the 100, 143 and 217 GHz channels. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on cosmological parameters. We find good internal agreement among the high-l cross-spectra with residuals of a few uK^2 at l &lt;= 1000. We compare our results with foreground-cleaned CMB maps, and with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. The best-fit LCDM cosmology is in excellent agreement with preliminary Planck polarisation spectra. The standard LCDM cosmology is well constrained by Planck by l &lt;= 1500. For example, we report a 5.4 sigma deviation from n_s /= 1. Considering various extensions beyond the standard model, we find no indication of significant departures from the LCDM framework. Finally, we report a tension between the best-fit LCDM model and the low-l spectrum in the form of a power deficit of 5-10% at l
description: This paper is one of a set associated with the 2013 release of data from the Planck mission. 62 pages, 64 figures, 12 tables