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@article{Aghanim:2016:0004-6361/201526926,
author = {Aghanim, N and Arnaud, M and Ashdown, M and Aumont, J and Baccigalupi, C and Banday, AJ and Barreiro, RB and Bartlett, JG and Bartolo, N and Battaner, E and Benabed, K and Benoît, A and Benoit-Lévy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bock, JJ and Bonaldi, A and Bonavera, L and Bond, JR and Borrill, 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 Chiang, HC and Christensen, PR and Clements, DL and Colombo, LPL and Combet, C 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 Delabrouille, J and Désert, F-X and Di, Valentino E and Dickinson, C and Diego, JM and Dolag, K and Dole, H and Donzelli, S and Doré, O and Douspis, M and Ducout, A and Dunkley, J and Dupac, X and Efstathiou, G and Elsner, F and Enßlin, TA and Eriksen, HK and Fergusson, J and Finelli, F and },
doi = {0004-6361/201526926},
journal = {Astronomy & Astrophysics},
title = {Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters},
url = {http://dx.doi.org/10.1051/0004-6361/201526926},
volume = {594},
year = {2016}
}

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TY  - JOUR
AB  - This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlationfunctions of the cosmic microwave background (CMB) temperature and polarization fluctuations that account for relevant uncertainties, both instrumental and astrophysical in nature. They are based on the same hybrid approach used for the previous release, i.e., a pixel-based likelihood at low multipoles (< 30) and a Gaussian approximation to the distribution of cross-power spectra at higher multipoles. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. The increased redundancy brought by more than doubling the amount of data analysed enables further consistency checks and enhanced immunity to systematic effects. It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. Progress in the modelling of foreground emission enables the retention of a larger fraction of the sky to determine the properties of the CMB, which also contributes to the enhanced precision of the spectra. Improvements in data processing and instrumental modelling further reduce uncertainties. Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. For temperature, we also perform a full likelihood analysis of realistic end-to-end simulations of the instrumental response to the sky, which were fed into the actual data processing pipeline; this does not reveal biases from residual low-level instrumental systematics. Even with the increase in precision and robustness, the ΛCDM cosmological model continues to offer a very good fit to the Planck data. The slope of the primordial scalar fluctuations, ns, is confirmed smaller than unity at more than 5σ from Planck alone. We further validate the robustn
AU  - Aghanim,N
AU  - Arnaud,M
AU  - Ashdown,M
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartlett,JG
AU  - Bartolo,N
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoît,A
AU  - Benoit-Lévy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bock,JJ
AU  - Bonaldi,A
AU  - Bonavera,L
AU  - Bond,JR
AU  - Borrill,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  - Chiang,HC
AU  - Christensen,PR
AU  - Clements,DL
AU  - Colombo,LPL
AU  - Combet,C
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  - Delabrouille,J
AU  - Désert,F-X
AU  - Di,Valentino E
AU  - Dickinson,C
AU  - Diego,JM
AU  - Dolag,K
AU  - Dole,H
AU  - Donzelli,S
AU  - Doré,O
AU  - Douspis,M
AU  - Ducout,A
AU  - Dunkley,J
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  - Galeotta,S
AU  - Galli,S
AU  - Ganga,K
AU  - Gauthier,C
AU  - Gerbino,M
AU  - Giard,M
AU  - Gjerløw,E
AU  - González-Nuevo,J
AU  - Górski,KM
AU  - Gratton,S
AU  - Gregorio,A
AU  - Gruppuso,A
AU  - Gudmundsson,JE
AU  - Hamann,J
AU  - Hansen,FK
AU  - Harrison,DL
AU  - Helou,G
AU  - Henrot-Versillé,S
AU  - Hernández-Monteagudo,C
AU  - Herranz,D
AU  - Hildebrandt,SR
AU  - Hivon,E
AU  - Holmes,WA
AU  - Hornstrup,A
AU  - Huffenberger,KM
AU  - Hurier,G
AU  - Jaffe,AH
AU  - Jones,WC
AU  - Juvela,M
AU  - Keihänen,E
AU  - Keskitalo,R
AU  - Kiiveri,K
AU  - Knoche,J
AU  - Knox,L
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lagache,G
AU  - Lähteenmäki,A
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Lattanzi,M
AU  - Lawrence,CR
AU  - Le,Jeune M
AU  - Leonardi,R
AU  - Lesgourgues,J
AU  - Levrier,F
AU  - Lewis,A
AU  - Liguori,M
AU  - Lilje,PB
AU  - Lilley,M
AU  - Linden-Vørnle,M
AU  - Lindholm,V
AU  - López-Caniego,M
AU  - Macías-Pérez,JF
AU  - Maffei,B
AU  - Maggio,G
AU  - Maino,D
AU  - Mandolesi,N
AU  - Mangilli,A
AU  - Maris,M
AU  - Martin,PG
AU  - Martínez-González,E
AU  - Masi,S
AU  - Matarrese,S
AU  - Meinhold,PR
AU  - Melchiorri,A
AU  - Migliaccio,M
AU  - Millea,M
AU  - Mitra,S
AU  - Miville-Deschênes,M-A
AU  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Mortlock,D
AU  - Mottet,S
AU  - Munshi,D
AU  - Murphy,JA
AU  - Narimani,A
AU  - Naselsky,P
AU  - Nati,F
AU  - Natoli,P
AU  - Noviello,F
AU  - Novikov,D
AU  - Novikov,I
AU  - Oxborrow,CA
AU  - Paci,F
AU  - Pagano,L
AU  - Pajot,F
AU  - Paoletti,D
AU  - Partridge,B
AU  - Pasian,F
AU  - Patanchon,G
AU  - Pearson,TJ
AU  - Perdereau,O
AU  - Perotto,L
AU  - Pettorino,V
AU  - Piacentini,F
AU  - Piat,M
AU  - Pierpaoli,E
AU  - Pietrobon,D P
DO  - 0004-6361/201526926
PY  - 2016///
SN  - 0004-6361
TI  - Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters
T2  - Astronomy & Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201526926
UR  - http://hdl.handle.net/10044/1/43707
VL  - 594
ER  -

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