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@article{Ade:2016:0004-6361/201525898,
author = {Ade, PAR and Aghanim, N and Arnaud, M and Arroja, F and Ashdown, M and Aumont, J and Baccigalupi, C and Ballardini, M and Banday, AJ and Barreiro, RB and Bartolo, N and Battaner, E and Benabed, K and Benoit, A and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bock, JJ and Bonaldi, A and Bonavera, L and Bondi, JR and Borrillu, J and Bouchet, FR and Boulanger, F and Bucher, M and Burigana, C and Butler, RC and Calabrese, E and Cardoso, J-F and Catalano, A and Challinor, A and Chamballu, A and Chary, R-R and Chiang, HC and Christensen, PR and Churchl, S and Clements, DL and Colombi, S and Colombo, LPL and Combet, C and Contreras, D and Couchot, F and Coulais, A and Crill, BP and Curto, A and Cuttaia, F and Danese, L and Davies, RD and Davis, RJ and de, Bernardis P and de, Rosa A and de, Zotti G and Delabrouillei, J and Desert, F-X and Diego, JM and Dole, H and Donzelli, S and Dore, O and Douspis, M and Ducout, A and Dupac, X and Efstathiou, G and Elsner, F and Ens},
doi = {0004-6361/201525898},
journal = {Astronomy and Astrophysics},
title = {Planck 2015 results XX. Constraints on inflation},
url = {http://dx.doi.org/10.1051/0004-6361/201525898},
volume = {594},
year = {2016}
}

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TY  - JOUR
AB  - We present the implications for cosmic inflation of the Planck measurements of the cosmic microwave background (CMB) anisotropies in both temperature and polarization based on the full Planck survey, which includes more than twice the integration time of the nominal survey used for the 2013 release papers. The Planck full mission temperature data and a first release of polarization data on large angular scales measure the spectral index of curvature perturbations to be ns = 0.968 ± 0.006 and tightly constrain its scale dependence to dns/ dlnk = −0.003 ± 0.007 when combined with the Planck lensing likelihood. When the Planck high- polarization data are included, the results are consistent and uncertainties are further reduced. The upper bound on the tensor-to-scalar ratio is r0.002< 0.11 (95% CL). This upper limit is consistent with the B-mode polarization constraint r< 0.12 (95% CL) obtained from a joint analysis of the BICEP2/Keck Array and Planck data. These results imply that V(φ) ∝ φ2 and natural inflation are now disfavoured compared to models predicting a smaller tensor-to-scalar ratio, such as R2 inflation. We search for several physically motivated deviations from a simple power-law spectrum of curvature perturbations, including those motivated by a reconstruction of the inflaton potential not relying on the slow-roll approximation. We find that such models are not preferred, either according to a Bayesian model comparison or according to a frequentist simulation-based analysis. Three independent methods reconstructing the primordial power spectrum consistently recover a featureless and smooth over the range of scales 0.008 Mpc-1  k  0.1 Mpc-1. At large scales, each method finds deviations from a power law, connected to a deficit at multipoles  ≈ 20−40 in the temperature power spectrum, but at an uncompelling statistical significance owing to the large cosmic variance present at these multipoles. By comb
AU  - Ade,PAR
AU  - Aghanim,N
AU  - Arnaud,M
AU  - Arroja,F
AU  - Ashdown,M
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Ballardini,M
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartolo,N
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoit,A
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bock,JJ
AU  - Bonaldi,A
AU  - Bonavera,L
AU  - Bondi,JR
AU  - Borrillu,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Bucher,M
AU  - Burigana,C
AU  - Butler,RC
AU  - Calabrese,E
AU  - Cardoso,J-F
AU  - Catalano,A
AU  - Challinor,A
AU  - Chamballu,A
AU  - Chary,R-R
AU  - Chiang,HC
AU  - Christensen,PR
AU  - Churchl,S
AU  - Clements,DL
AU  - Colombi,S
AU  - Colombo,LPL
AU  - Combet,C
AU  - Contreras,D
AU  - Couchot,F
AU  - Coulais,A
AU  - Crill,BP
AU  - Curto,A
AU  - Cuttaia,F
AU  - Danese,L
AU  - Davies,RD
AU  - Davis,RJ
AU  - de,Bernardis P
AU  - de,Rosa A
AU  - de,Zotti G
AU  - Delabrouillei,J
AU  - Desert,F-X
AU  - Diego,JM
AU  - Dole,H
AU  - Donzelli,S
AU  - Dore,O
AU  - Douspis,M
AU  - Ducout,A
AU  - Dupac,X
AU  - Efstathiou,G
AU  - Elsner,F
AU  - Ensslin,TA
AU  - Eriksen,HK
AU  - Fergusson,J
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Franceschi,E
AU  - Frejsel,A
AU  - Frolov,A
AU  - Galeotta,S
AU  - Galli,S
AU  - Ganga,K
AU  - Gauthier,C
AU  - Giard,M
AU  - Giraud-Heraud,Y
AU  - Gjerlow,E
AU  - Gonzalez-Nuevo,J
AU  - Gorski,KM
AU  - Gratton,S
AU  - Gregorio,A
AU  - Gruppuso,A
AU  - Gudmundsson,JE
AU  - Hamann,J
AU  - Handley,W
AU  - Hansen,FK
AU  - Hanson,D
AU  - Harrison,DL
AU  - Henrot-Versille,S
AU  - Hernandez-Monteagudo,C
AU  - Herranz,D
AU  - Hildebrandt,SR
AU  - Hivon,E
AU  - Hobson,M
AU  - Holmes,WA
AU  - Hornstrup,A
AU  - Hovest,W
AU  - Huang,Z
AU  - Huffenberger,KM
AU  - Hurier,G
AU  - Jaffe,AH
AU  - Jaffe,TR
AU  - Jones,WC
AU  - Juvela,M
AU  - Keihanen,E
AU  - Keskitalo,R
AU  - Kim,J
AU  - Kisner,TS
AU  - Kneissl,R
AU  - Knoche,J
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lagache,G
AU  - Lahteenmaki,A
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Lattanzi,M
AU  - Lawrence,CR
AU  - Leonardi,R
AU  - Lesgourgues,J
AU  - Levrier,F
AU  - Lewis,A
AU  - Liguori,M
AU  - Lilje,PB
AU  - Linden-Vornle,M
AU  - Lopez-Caniego,M
AU  - Lubin,PM
AU  - Ma,Y-Z
AU  - Macias-Perez,JF
AU  - Maggio,G
AU  - Maino,D
AU  - Mandolesi,N
AU  - Mangilli,A
AU  - Maris,M
AU  - Martini,PG
AU  - Martinez-Gonzalez,E
AU  - Masi,S
AU  - Matarrese,S
AU  - McGehee,P
AU  - Meinhold,PR
AU  - Melchiorri,A
AU  - Mendes,L
AU  - Mennella,A
AU  - Migliaccio,M
AU  - Mitra,S
AU  - Miville-Deschenes,M-A
AU  - Molinari,D
AU  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Mortlock,D
AU  - Moss,A
AU  - Munchmeyer,M
AU  - Munshi,D
AU  - Murphy,JA
AU  - Naselsky,P
AU  - Nati,F
AU  - Natoli,P
AU  - Netterfield,CB
AU  - Norgaard-Nielsen,HU
AU  - Noviello,F
AU  - Novikov,D
AU  - Novikov,I
AU  - Oxborrow,CA
AU  - Paci
DO  - 0004-6361/201525898
PY  - 2016///
SN  - 0004-6361
TI  - Planck 2015 results XX. Constraints on inflation
T2  - Astronomy and Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201525898
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000385832200018&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/54267
VL  - 594
ER  -

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