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Oxborrow, C. Armitage-Caplan, C. Baccigalupi, C. B. Netterfield, C. Burigana, C. Dickinson, C. Gauthier, C. Hernandez-Monteagudo, C. Renault, C. R. Lawrence, C. Rosset, D. Hanson, D. Harrison, D. Herranz, D. J. Marshall, D. L. Clements, D. Maino, D. Mortlock, D. Munshi, D. Novikov, D. Paoletti, D. Pietrobon, D. Santos, D. Scott, D. Sutton, D. Tavagnacco, D. Yvon, E. Battaner, E. Calabrese, E. Franceschi, E. Hivon, E. Keihanen, E. Martinez-Gonzalez, E. Pierpaoli, E. Pointecouteau, E. P. S. Shellard, F. Atrio-Barandela, F. Couchot, F. Cuttaia, F. Finelli, F. K. Hansen, F. Matthai, F. Nati, F. Noviello, F. Paci, F. Pajot, F. Pasian, F. Perrotta, F. Piacentini, F. R. Bouchet, F. Sureau, F. Villa, F.-X. Desert, G. de Zotti, G. Efstathiou, G. Giardino, G. Lagache, G. Morgante, G. Patanchon, G. Polenta, G. Prezeau, G. Rocha, G. Roudier, G. Savini, G. W. Pratt, H. C. Chiang, H. Dole, H. K. Eriksen, H. Kurki-Suonio, H. U. Norgaard-Nielsen, H. V. Peiris, I. J. O'Dwyer, I. Novikov, I. Ristorcelli, J. A. Murphy, J. A. Rubino-Martin, J. A. Tauber, J. Aumont, J. Bobin, J. Borrill, J. Delabrouille, J. Dunkley, J.-F. Cardoso, J. F. Macias-Perez, J.-F. Sygnet, J. G. Bartlett, J. Gonzalez-Nuevo, J. Hamann, J. J. Bock, J. Knoche, J. Lesgourgues, J.-L. Puget, J.-L. Starck, J.-M. Delouis, J. M. Diego, J.-M. Lamarre, J.-P. Bernard, J. P. Leahy, J. P. Rachen, J. P. Zibin, J. R. Bond, J. Treguer-Goudineau, J. Tuovinen, J. Valiviita, J. Varis, K. Benabed, K. Ganga, K. M. Gorski, K. M. Huffenberger, L. A. Wade, L. Danese, L. D. Spencer, L. Knox, L. Mendes, L. Montier, L. Pagano, L. Perotto, L. P. L. Colombo, L. Popa, L. Terenzi, L. Toffolatti, L. Valenziano, L.-Y Chiang, M.-A. Miville-Deschenes, M. Arnaud, M. Ashdown, M. Bersanelli, M. Bridges, M. Bucher, M. Douspis, M. D. Seiffert, M. Frailis, M. Giard, M. Hobson, M. Juvela, M. Kunz, M. Liguori, M. Linden-Vernle, M. Lopez-Caniego, M. Maris, M. Massardi, M. Migliaccio, M. Piat, M. Reinecke, M. Remazeilles, M. Rowan-Robinson, M. Sandri, M. Savelainen, M. Tomasi, M. Tristram, M. Tucci, M. White, N. Aghanim, N. Bartolo, N. Mandolesi, N. Ponthieu, N. Vittorio, O. Dore, O. Forni, O. Perdereau, P. Bielewicz, P. B. Lilje, P. De Bernardis, P. G. Martin, Planck Collaboration: P. A. R. Ade, P. Mazzotta, P. M. Lubin, P. Naselsky, P. Natoli, P. R. Christensen, P. R. Meinhold, P. Vielva, R. B. Barreiro, R. C. Butler, R. D. Davies, R. J. Davis, R. J. Laureijs, R. Keskitalo, R. Kneissl, R. Leonardi, R. Paladini, R. Rebolo, R. Stompor, R. Sudiwala, R. Sunyaev, S. Church, S. Colombi, S. Donzelli, S. Galeotta, S. Gratton, S. Henrot-Versille, S. Leach, S. Masi, S. Matarrese, S. Mitra, S. Osborne, S. Pandolfi, S. Plaszczynski, S. Prunet, S. R. Hildebrandt, S. Ricciardi, T. A. Ensslin, T. Poutanen, T. Riller, T. R. Jaffe, T. S. Kisner, V. Stolyarov, W. A. Holmes, W. C. Jones, W. Hovest, X. Dupac, Y. Giraud-Hiraud","submitted_at":"2013-03-20T20:10:22Z","abstract_excerpt":"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 $\\sigma$. Planck establishes an upper bound on the tensor-to-scalar ratio of r < 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models, preferring potentials with V\" < 0. 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Keihanen, E. Martinez-Gonzalez, E. Pierpaoli, E. Pointecouteau, E. P. S. Shellard, F. Atrio-Barandela, F. Couchot, F. Cuttaia, F. Finelli, F. K. Hansen, F. Matthai, F. Nati, F. Noviello, F. Paci, F. Pajot, F. Pasian, F. Perrotta, F. Piacentini, F. R. Bouchet, F. Sureau, F. Villa, F.-X. Desert, G. de Zotti, G. Efstathiou, G. Giardino, G. Lagache, G. Morgante, G. Patanchon, G. Polenta, G. Prezeau, G. Rocha, G. Roudier, G. Savini, G. W. Pratt, H. C. Chiang, H. Dole, H. K. Eriksen, H. Kurki-Suonio, H. U. Norgaard-Nielsen, H. V. Peiris, I. J. O'Dwyer, I. Novikov, I. Ristorcelli, J. A. Murphy, J. A. Rubino-Martin, J. A. Tauber, J. Aumont, J. Bobin, J. Borrill, J. Delabrouille, J. Dunkley, J.-F. Cardoso, J. F. Macias-Perez, J.-F. Sygnet, J. G. Bartlett, J. Gonzalez-Nuevo, J. Hamann, J. J. Bock, J. Knoche, J. Lesgourgues, J.-L. Puget, J.-L. Starck, J.-M. Delouis, J. M. Diego, J.-M. Lamarre, J.-P. Bernard, J. P. Leahy, J. P. Rachen, J. P. Zibin, J. R. Bond, J. Treguer-Goudineau, J. Tuovinen, J. Valiviita, J. Varis, K. Benabed, K. Ganga, K. M. Gorski, K. M. Huffenberger, L. A. Wade, L. Danese, L. D. Spencer, L. Knox, L. Mendes, L. Montier, L. Pagano, L. Perotto, L. P. L. Colombo, L. Popa, L. Terenzi, L. Toffolatti, L. Valenziano, L.-Y Chiang, M.-A. Miville-Deschenes, M. Arnaud, M. Ashdown, M. Bersanelli, M. Bridges, M. Bucher, M. Douspis, M. D. Seiffert, M. Frailis, M. Giard, M. Hobson, M. Juvela, M. Kunz, M. Liguori, M. Linden-Vernle, M. Lopez-Caniego, M. Maris, M. Massardi, M. Migliaccio, M. Piat, M. Reinecke, M. Remazeilles, M. Rowan-Robinson, M. Sandri, M. Savelainen, M. Tomasi, M. Tristram, M. Tucci, M. White, N. Aghanim, N. Bartolo, N. Mandolesi, N. Ponthieu, N. Vittorio, O. Dore, O. Forni, O. Perdereau, P. Bielewicz, P. B. Lilje, P. De Bernardis, P. G. Martin, Planck Collaboration: P. A. R. Ade, P. Mazzotta, P. M. Lubin, P. Naselsky, P. Natoli, P. R. Christensen, P. R. Meinhold, P. Vielva, R. B. Barreiro, R. C. Butler, R. D. Davies, R. J. Davis, R. J. Laureijs, R. Keskitalo, R. Kneissl, R. Leonardi, R. Paladini, R. Rebolo, R. Stompor, R. Sudiwala, R. Sunyaev, S. Church, S. Colombi, S. Donzelli, S. Galeotta, S. Gratton, S. Henrot-Versille, S. Leach, S. Masi, S. Matarrese, S. Mitra, S. Osborne, S. Pandolfi, S. Plaszczynski, S. Prunet, S. R. Hildebrandt, S. Ricciardi, T. A. Ensslin, T. Poutanen, T. Riller, T. R. Jaffe, T. S. Kisner, V. Stolyarov, W. A. Holmes, W. C. Jones, W. Hovest, X. Dupac, Y. Giraud-Hiraud","submitted_at":"2013-03-20T20:10:22Z","abstract_excerpt":"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 $\\sigma$. Planck establishes an upper bound on the tensor-to-scalar ratio of r < 0.11 (95% CL). 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