Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters
Creators: name: Planck Collaboration
name: Aghanim, N.
name: Arnaud, M.
name: Ashdown, M.
name: Aumont, J.
name: Baccigalupi, C.
name: Banday, A. J.
name: Barreiro, R. B.
name: Bartlett, J. G.
name: Bartolo, N.
name: Battaner, E.
name: Benabed, K.
name: Benoît, A.
name: Benoit-Lévy, A.
name: Bernard, J. -P.
name: Bersanelli, M.
name: Bielewicz, P.
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: Bucher, M.
name: Burigana, C.
name: Butler, R. C.
name: Calabrese, E.
name: Cardoso, J. -F.
name: Catalano, A.
name: Challinor, A.
name: Chiang, H. C.
name: Christensen, P. R.
name: Clements, D. L.
name: Colombo, L. P. L.
name: Combet, C.
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: Désert, F. -X.
name: Di Valentino, E.
name: Dickinson, C.
name: Diego, J. M.
name: Dolag, K.
name: Dole, H.
name: Donzelli, S.
name: Doré, O.
name: Douspis, M.
name: Ducout, A.
name: Dunkley, J.
name: Dupac, X.
name: Efstathiou, G.
name: Elsner, F.
name: Enßlin, T. A.
name: Eriksen, H. K.
name: Fergusson, J.
name: Finelli, F.
name: Forni, O.
name: Frailis, M.
name: Fraisse, A. A.
name: Franceschi, E.
name: Frejsel, A.
name: Galeotta, S.
name: Galli, S.
name: Ganga, K.
name: Gauthier, C.
name: Gerbino, M.
name: Giard, M.
name: Gjerløw, E.
name: González-Nuevo, J.
name: Górski, K. M.
name: Gratton, S.
name: Gregorio, A.
name: Gruppuso, A.
name: Gudmundsson, J. E.
name: Hamann, J.
name: Hansen, F. K.
name: Harrison, D. L.
name: Helou, G.
name: Henrot-Versillé, S.
name: Hernández-Monteagudo, C.
name: Herranz, D.
name: Hildebrandt, S. R.
name: Hivon, E.
name: Holmes, W. A.
name: Hornstrup, A.
name: Huffenberger, K. M.
name: Hurier, G.
name: Jaffe, A. H.
name: Jones, W. C.
name: Juvela, M.
name: Keihänen, E.
name: Keskitalo, R.
name: Kiiveri, K.
name: Knoche, J.
name: Knox, L.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Lagache, G.
name: Lähteenmäki, A.
name: Lamarre, J. -M.
name: Lasenby, A.
name: Lattanzi, M.
name: Lawrence, C. R.
name: Jeune, M. Le
name: Leonardi, R.
name: Lesgourgues, J.
name: Levrier, F.
name: Lewis, A.
name: Liguori, M.
name: Lilje, P. B.
name: Lilley, M.
name: Linden-Vørnle, M.
name: Lindholm, V.
name: López-Caniego, M.
name: Macías-Pérez, J. F.
name: Maffei, B.
name: Maggio, G.
name: Maino, D.
name: Mandolesi, N.
name: Mangilli, A.
name: Maris, M.
name: Martin, P. G.
name: Martínez-González, E.
name: Masi, S.
name: Matarrese, S.
name: Meinhold, P. R.
name: Melchiorri, A.
name: Migliaccio, M.
name: Millea, M.
name: Mitra, S.
name: Miville-Deschênes, M. -A.
name: Moneti, A.
name: Montier, L.
name: Morgante, G.
name: Mortlock, D.
name: Mottet, S.
name: Munshi, D.
name: Murphy, J. A.
name: Narimani, A.
name: Naselsky, P.
name: Nati, F.
name: Natoli, P.
name: Noviello, F.
name: Novikov, D.
name: Novikov, I.
name: Oxborrow, C. A.
name: Paci, F.
name: Pagano, L.
name: Pajot, F.
name: Paoletti, D.
name: Partridge, B.
name: Pasian, F.
name: Patanchon, G.
name: Pearson, T. J.
name: Perdereau, O.
name: Perotto, L.
name: Pettorino, V.
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: Pratt, G. W.
name: Prunet, S.
name: Puget, J. -L.
name: Rachen, J. P.
name: Reinecke, M.
name: Remazeilles, M.
name: Renault, C.
name: Renzi, A.
name: Ristorcelli, I.
name: Rocha, G.
name: Rossetti, M.
name: Roudier, G.
name: d'Orfeuil, B. Rouillé
name: Rubiño-Martín, J. A.
name: Rusholme, B.
name: Salvati, L.
name: Sandri, M.
name: Santos, D.
name: Savelainen, M.
name: Savini, G.
name: Scott, D.
name: Serra, P.
name: Spencer, L. D.
name: Spinelli, M.
name: Stolyarov, V.
name: Stompor, R.
name: Sunyaev, R.
name: Sutton, D.
name: Suur-Uski, A. -S.
name: Sygnet, J. -F.
name: Tauber, J. A.
name: Terenzi, L.
name: Toffolatti, L.
name: Tomasi, M.
name: Tristram, M.
name: Trombetti, T.
name: Tucci, M.
name: Tuovinen, J.
name: Umana, G.
name: Valenziano, L.
name: Valiviita, J.
name: Van Tent, F.
name: Vielva, P.
name: Villa, F.
name: Wade, L. A.
name: Wandelt, B. D.
name: Wehus, I. K.
name: Yvon, D.
name: Zacchei, A.
name: Zonca, A.
Publisher: name: arXiv
Year: 2015
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlations of CMB data, using the hybrid approach employed previously: pixel-based at $\ell&lt;30$ and a Gaussian approximation to the distribution of spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models, allowing further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction. Improvements in processing and instrumental models further reduce uncertainties. For temperature, we perform an analysis of end-to-end instrumental simulations fed into the data processing pipeline; this does not reveal biases from residual instrumental systematics. The $Λ$CDM cosmological model continues to offer a very good fit to Planck data. The slope of primordial scalar fluctuations, $n_s$, is confirmed smaller than unity at more than 5σ from Planck alone. We further validate robustness against specific extensions to the baseline cosmology. E.g., the effective number of neutrino species remains compatible with the canonical value of 3.046. This first detailed analysis of Planck polarization concentrates on E modes. At low $\ell$ we use temperature at all frequencies and a subset of polarization. The frequency range improves CMB-foreground separation. Within the baseline model this requires a reionization optical depth $τ=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically O($μ$K$^2$); we recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization allows a separate determination of $Λ$CDM parameters consistent with those from temperature alone.
description: This paper is associated with the 2015 Planck release (see http://www.cosmos.esa.int/web/planck/publications). Likelihood code &amp; data available at http://www.cosmos.esa.int/web/planck/pla. Version accepted by A&amp;A. Substancially extended (104 pages) with analysis of end-to-simulations of systematics further confirming the results. Abstract abridged