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 be n(s) = 0.9603 +/- 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. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n >= 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn(s)/dln k = -0.0134 +/- 0.0090. We verify these conclusions through a numerical analysis, which makes no slowroll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by delta 2 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 Planck bounds on fNL. Planck constrains with unprecedented accuracy the amplitude and possible correlation (with the adiabatic mode) of non-decaying isocurvature fluctuations. The fractional primordial contributions of cold dark matter (CDM) isocurvature modes of the types expected in the curvaton and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelated isocurvature component can improve the 2 by approximately 4 as a result of slightly lowering the theoretical prediction for the 40 multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions.

Planck 2013 results. XXII. Constraints on inflation / J., Tauber; P., Ade; N., Aghanim; C., Armitage Caplan; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A., Banday; R., Barreiro; J., Bartlett; N., Bartolo; E., Battaner; K., Benabed; A., Benoît; A., Benoit Lévy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; J., Bock; A., Bonaldi; J., Bond; J., Borrill; F., Bouchet; M., Bridges; M., Bucher; C., Burigana; R., Butler; Calabrese, Elisabetta; J., Cardoso; Catalano, Andrea; A., Challinor; A., Chamballu; H., Chiang; L., Chiang; P., Christensen; S., Church; D., Clements; S., Colombi; L., Colombo; F., Couchot; A., Coulais; B., Crill; A., Curto; F., Cuttaia; L., Danese; R., Davies; R., Davis; DE BERNARDIS, Paolo; A. D., Rosa; G. D., Zotti; J., Delabrouille; J., Delouis; F., Désert; C., Dickinson; J., Diego; H., Dole; S., Donzelli; O., Doré; M., Douspis; J., Dunkley; X., Dupac; G., Efstathiou; T., Enßlin; H., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; C., Gauthier; M., Giard; G., Giardino; Y., Giraud Héraud; J., González Nuevo; K., Górski; S., Gratton; A., Gregorio; A., Gruppuso; J., Hamann; F., Hansen; D., Hanson; D., Harrison; S., Henrot Versillé; C., Hernández Monteagudo; D., Herranz; S., Hildebrandt; E., Hivon; M., Hobson; W., Holmes; A., Hornstrup; W., Hovest; K., Huffenberger; A., Jaffe; T., Jaffe; W., Jones; M., Juvela; E., Keihänen; R., Keskitalo; T., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., Lähteenmäki; J., Lamarre; A., Lasenby; R., Laureijs; C., Lawrence; S., Leach; J., Leahy; R., Leonardi; J., Lesgourgues; A., Lewis; M., Liguori; P., Lilje; M., Linden Vørnle; M., López Caniego; P., Lubin; J., Maciás Pérez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; D., Marshall; P., Martin; E., Martínez González; Masi, Silvia; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; P., Meinhold; Melchiorri, Alessandro; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Deschênes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; A., Moss; D., Munshi; J., Murphy; P., Naselsky; Nati, Federico; P., Natoli; C., Netterfield; H., Nørgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; I., O'Dwyer; S., Osborne; C., Oxborrow; F., Paci; Pagano, Luca; F., Pajot; R., Paladini; S., Pandolfi; D., Paoletti; B., Partridge; F., Pasian; G., Patanchon; H., Peiris; O., Perdereau; L., Perotto; F., Perrotta; Piacentini, Francesco; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; Polenta, Gianluca; N., Ponthieu; L., Popa; T., Poutanen; G., Pratt; G., Prézeau; S., Prunet; J., Puget; J., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; Ricciardi, Sara; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; M., Rowan Robinson; J., Rubinõ Martín; B., Rusholme; M., Sandri; D., Santos; M., Savelainen; Savini, Giorgio; D., Scott; M., Seiffert; E., Shellard; L., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J., Tauber; D., Tavagnacco; L., Terenzi; L., Toffolatti; M., Tomasi; J., Tréguer Goudineau; M., Tristram; M., Tucci; J., Tuovinen; L., Valenziano; J., Valiviita; B. V., Tent; J., Varis; P., Vielva; F., Villa; N., Vittorio; L., Wade; B., Wandelt; M., White; A., Wilkinson; D., Yvon; A., Zacchei; J., Zibin; A., Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - STAMPA. - 571:(2014), p. A22. [10.1051/0004-6361/201321569]

Planck 2013 results. XXII. Constraints on inflation

CALABRESE, ELISABETTA;CATALANO, Andrea;DE BERNARDIS, Paolo;MASI, Silvia;MELCHIORRI, Alessandro;NATI, FEDERICO;PAGANO, LUCA;PIACENTINI, Francesco;POLENTA, GIANLUCA;RICCIARDI, Sara;SAVINI, Giorgio;
2014

Abstract

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 be n(s) = 0.9603 +/- 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. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n >= 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn(s)/dln k = -0.0134 +/- 0.0090. We verify these conclusions through a numerical analysis, which makes no slowroll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by delta 2 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 Planck bounds on fNL. Planck constrains with unprecedented accuracy the amplitude and possible correlation (with the adiabatic mode) of non-decaying isocurvature fluctuations. The fractional primordial contributions of cold dark matter (CDM) isocurvature modes of the types expected in the curvaton and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelated isocurvature component can improve the 2 by approximately 4 as a result of slightly lowering the theoretical prediction for the 40 multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions.
2014
cosmic background radiation; inflation, early Universe
01 Pubblicazione su rivista::01a Articolo in rivista
Planck 2013 results. XXII. Constraints on inflation / J., Tauber; P., Ade; N., Aghanim; C., Armitage Caplan; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A., Banday; R., Barreiro; J., Bartlett; N., Bartolo; E., Battaner; K., Benabed; A., Benoît; A., Benoit Lévy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; J., Bock; A., Bonaldi; J., Bond; J., Borrill; F., Bouchet; M., Bridges; M., Bucher; C., Burigana; R., Butler; Calabrese, Elisabetta; J., Cardoso; Catalano, Andrea; A., Challinor; A., Chamballu; H., Chiang; L., Chiang; P., Christensen; S., Church; D., Clements; S., Colombi; L., Colombo; F., Couchot; A., Coulais; B., Crill; A., Curto; F., Cuttaia; L., Danese; R., Davies; R., Davis; DE BERNARDIS, Paolo; A. D., Rosa; G. D., Zotti; J., Delabrouille; J., Delouis; F., Désert; C., Dickinson; J., Diego; H., Dole; S., Donzelli; O., Doré; M., Douspis; J., Dunkley; X., Dupac; G., Efstathiou; T., Enßlin; H., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; C., Gauthier; M., Giard; G., Giardino; Y., Giraud Héraud; J., González Nuevo; K., Górski; S., Gratton; A., Gregorio; A., Gruppuso; J., Hamann; F., Hansen; D., Hanson; D., Harrison; S., Henrot Versillé; C., Hernández Monteagudo; D., Herranz; S., Hildebrandt; E., Hivon; M., Hobson; W., Holmes; A., Hornstrup; W., Hovest; K., Huffenberger; A., Jaffe; T., Jaffe; W., Jones; M., Juvela; E., Keihänen; R., Keskitalo; T., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., Lähteenmäki; J., Lamarre; A., Lasenby; R., Laureijs; C., Lawrence; S., Leach; J., Leahy; R., Leonardi; J., Lesgourgues; A., Lewis; M., Liguori; P., Lilje; M., Linden Vørnle; M., López Caniego; P., Lubin; J., Maciás Pérez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; D., Marshall; P., Martin; E., Martínez González; Masi, Silvia; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; P., Meinhold; Melchiorri, Alessandro; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Deschênes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; A., Moss; D., Munshi; J., Murphy; P., Naselsky; Nati, Federico; P., Natoli; C., Netterfield; H., Nørgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; I., O'Dwyer; S., Osborne; C., Oxborrow; F., Paci; Pagano, Luca; F., Pajot; R., Paladini; S., Pandolfi; D., Paoletti; B., Partridge; F., Pasian; G., Patanchon; H., Peiris; O., Perdereau; L., Perotto; F., Perrotta; Piacentini, Francesco; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; Polenta, Gianluca; N., Ponthieu; L., Popa; T., Poutanen; G., Pratt; G., Prézeau; S., Prunet; J., Puget; J., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; Ricciardi, Sara; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; M., Rowan Robinson; J., Rubinõ Martín; B., Rusholme; M., Sandri; D., Santos; M., Savelainen; Savini, Giorgio; D., Scott; M., Seiffert; E., Shellard; L., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J., Tauber; D., Tavagnacco; L., Terenzi; L., Toffolatti; M., Tomasi; J., Tréguer Goudineau; M., Tristram; M., Tucci; J., Tuovinen; L., Valenziano; J., Valiviita; B. V., Tent; J., Varis; P., Vielva; F., Villa; N., Vittorio; L., Wade; B., Wandelt; M., White; A., Wilkinson; D., Yvon; A., Zacchei; J., Zibin; A., Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - STAMPA. - 571:(2014), p. A22. [10.1051/0004-6361/201321569]
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11573/784295
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