Planck 2013 results. XXII. Constraints on inflation
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: Bartolo, N.
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: Bond, J. R.
name: Borrill, J.
name: Bouchet, F. R.
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, H. C.
name: Chiang, L. -Y
name: Christensen, P. R.
name: Church, S.
name: Clements, D. L.
name: Colombi, S.
name: Colombo, L. P. L.
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: Ensslin, T. A.
name: Eriksen, H. K.
name: Finelli, F.
name: Forni, O.
name: Frailis, M.
name: Franceschi, E.
name: Galeotta, S.
name: Ganga, K.
name: Gauthier, C.
name: Giard, M.
name: Giardino, G.
name: Giraud-Hiraud, Y.
name: Gonzalez-Nuevo, J.
name: Gorski, K. M.
name: Gratton, S.
name: Gregorio, A.
name: Gruppuso, A.
name: Hamann, J.
name: Hansen, F. K.
name: Hanson, D.
name: Harrison, D.
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: Jaffe, A. H.
name: Jaffe, T. R.
name: Jones, W. C.
name: Juvela, M.
name: Keihanen, E.
name: Keskitalo, R.
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: Laureijs, R. J.
name: Lawrence, C. R.
name: Leach, S.
name: Leahy, J. P.
name: Leonardi, R.
name: Lesgourgues, J.
name: Lewis, A.
name: Liguori, M.
name: Lilje, P. B.
name: Linden-Vernle, M.
name: Lopez-Caniego, M.
name: Lubin, P. M.
name: Macias-Perez, J. F.
name: Maffei, B.
name: Maino, D.
name: Mandolesi, N.
name: Maris, M.
name: Marshall, D. J.
name: Martin, P. G.
name: Martinez-Gonzalez, E.
name: Masi, S.
name: Massardi, M.
name: Matarrese, S.
name: Matthai, F.
name: Mazzotta, P.
name: Meinhold, P. R.
name: Melchiorri, A.
name: Mendes, L.
name: Mennella, A.
name: Migliaccio, M.
name: Mitra, S.
name: Miville-Deschenes, M. -A.
name: Moneti, A.
name: Montier, L.
name: Morgante, G.
name: Mortlock, D.
name: Moss, A.
name: Munshi, D.
name: Murphy, J. A.
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: Osborne, S.
name: Oxborrow, C. A.
name: Paci, F.
name: Pagano, L.
name: Pajot, F.
name: Paladini, R.
name: Pandolfi, S.
name: Paoletti, D.
name: Partridge, B.
name: Pasian, F.
name: Patanchon, G.
name: Peiris, H. V.
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: Rebolo, R.
name: Reinecke, M.
name: Remazeilles, M.
name: Renault, C.
name: Ricciardi, S.
name: Riller, T.
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: Santos, D.
name: Savelainen, M.
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: Sunyaev, 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: Treguer-Goudineau, J.
name: Tristram, M.
name: Tucci, M.
name: Tuovinen, J.
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: White, M.
name: Wilkinson, A.
name: Yvon, D.
name: Zacchei, A.
name: Zibin, J. P.
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 analyse the implications of the Planck data for cosmic inflation. The Planck nominal mission temperature anisotropy measurements, combined with the WMAP large-angle polarization, constrain the scalar spectral index to $n_s = 0.9603 \pm 0.0073$, ruling out exact scale invariance at over 5 $σ$. Planck establishes an upper bound on the tensor-to-scalar ratio of r &lt; 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models, preferring potentials with V" &lt; 0. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n &gt; 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining $d n_s/d ln k = -0.0134 \pm 0.0090$. Several analyses dropping the slow-roll approximation are carried out, including detailed model comparison and inflationary potential reconstruction. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit $χ^2$ by ~ 10; however, Bayesian evidence does not prefer these models. We constrain several single-field inflation models with generalized Lagrangians by combining power spectrum data with bounds on $f_\mathrm{NL}$ measured by Planck. The fractional primordial contribution of CDM isocurvature modes in the curvaton and axion scenarios has upper bounds of 0.25% or 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelation can improve $χ^2$ by approximatively 4 as a result of slightly lowering the theoretical prediction for the $\ell&lt;40$ multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions.
description: 44 pages, 25 figures, 12 tables; updated version; small changes to match the published version