TY - JOUR T1 - Planck 2018 results: V. CMB power spectra and likelihoods A1 - Aghanim,N. A1 - Akrami,Y. A1 - Ashdown,M. A1 - Aumont,J. A1 - Baccigalupi,C. A1 - Ballardini,M. A1 - Banday,A. J. A1 - Barreiro,R. B. A1 - Bartolo,N. A1 - Basak,S. A1 - Benabed,K. A1 - Bernard,J. -P. A1 - Bersanelli,M. A1 - Bielewicz,P. A1 - Bock,J. J. A1 - Bond,J. R. A1 - Borrill,J. A1 - Bouchet,F. R. A1 - Boulanger,F. A1 - Bucher,M. A1 - Burigana,C. A1 - Butler,R. C. A1 - Calabrese,E. A1 - Cardoso,J. -F. A1 - Carron,J. A1 - Casaponsa,B. A1 - Challinor,A. A1 - Chiang,H. C. A1 - Colombo,L. P. L. A1 - Combet,C. A1 - Crill,B. P. A1 - Cuttaia,F. A1 - de Bernardis,P. A1 - de Rosa,A. A1 - de Zotti,G. A1 - Delabrouille,J. A1 - Delouis,Jean Marc A1 - Di Valentino,E. A1 - Diego,J. M. A1 - Dore,O. A1 - Douspis,M. A1 - Ducout,A. A1 - Dupac,X. A1 - Dusini,S. A1 - Efstathiou,G. A1 - Elsner,F. A1 - Ensslin,T. A. A1 - Eriksen,H. K. A1 - Fantaye,Y. A1 - Fernandez-Cobos,R. A1 - Finelli,F. A1 - Frailis,M. A1 - Fraisse,A. A. A1 - Franceschi,E. A1 - Frolov,A. A1 - Galeotta,S. A1 - Galli,S. A1 - Ganga,K. A1 - Genova-Santos,R. T. A1 - Gerbino,M. A1 - Ghosh,T. A1 - Giraud-Heraud,Y. A1 - Gonzalez-Nuevo,J. A1 - Gorski,K. M. A1 - Gratton,S. A1 - Gruppuso,A. A1 - Gudmundsson,J. E. A1 - Hamann,J. A1 - Handley,W. A1 - Hansen,F. K. A1 - Herranz,D. A1 - Hivon,E. A1 - Huang,Z. A1 - Jaffe,A. H. A1 - Jones,W. C. A1 - Keihanen,E. A1 - Keskitalo,R. A1 - Kiiveri,K. A1 - Kim,J. A1 - Kisner,T. S. A1 - Krachmalnicoff,N. A1 - Kunz,M. A1 - Kurki-Suonio,H. A1 - Lagache,G. A1 - Lamarre,J. -M. A1 - Lasenby,A. A1 - Lattanzi,M. A1 - Lawrence,C. R. A1 - Le Jeune,M. A1 - Levrier,F. A1 - Lewis,A. A1 - Liguori,M. A1 - Lilje,P. B. A1 - Lilley,M. A1 - Lindholm,V. A1 - Lopez-Caniego,M. A1 - Lubin,Pm A1 - Ma,Y. -Z. A1 - Macias-Perez,J. F. A1 - Maggio,G. A1 - Maino,D. A1 - Mandolesi,N. A1 - Mangilli,A. A1 - Marcos-Caballero,A. A1 - Maris,M. A1 - Martin,Pg A1 - Martinez-Gonzalez,E. A1 - Matarrese,S. A1 - Mauri,N. A1 - McEwen,J. D. A1 - Meinhold,P. R. A1 - Melchiorri,A. A1 - Mennella,A. A1 - Migliaccio,M. A1 - Millea,M. A1 - Miville-Deschenes,M. -A. A1 - Molinari,D. A1 - Moneti,A. A1 - Montier,L. A1 - Morgante,G. A1 - Moss,A. A1 - Natoli,P. A1 - Norgaard-Nielsen,H. U. A1 - Pagano,L. A1 - Paoletti,D. A1 - Partridge,B. A1 - Patanchon,G. A1 - Peiris,H. V. A1 - Perrotta,F. A1 - Pettorino,V. A1 - Piacentini,F. A1 - Polenta,G. A1 - Puget,J. -L. A1 - Rachen,J. P. A1 - Reinecke,M. A1 - Remazeilles,M. A1 - Renzi,A. A1 - Rocha,G. A1 - Rosset,C. A1 - Roudier,G. A1 - Rubino-Martin,J. A. A1 - Ruiz-Granados,B. A1 - Salvati,L. A1 - Sandri,M. A1 - Savelainen,M. A1 - Scott,D. A1 - Shellard,E. P. S. A1 - Sirignano,C. A1 - Sirri,G. A1 - Spencer,L. D. A1 - Sunyaev,R. A1 - Suur-Uski,A. -S. A1 - Tauber,J. A. A1 - Tavagnacco,D. A1 - Tenti,M. A1 - Toffolatti,L. A1 - Tomasi,M. A1 - Trombetti,T. A1 - Valiviita,J. A1 - Van Tent,B. A1 - Vielva,P. A1 - Villa,F. A1 - Vittorio,N. A1 - Wandelt,B. D. A1 - Wehus,I. K. A1 - Zacchei,A. A1 - Zonca,A. AD - Univ Paris Diderot, Univ Paris Saclay, Sorbonne Paris Cite, AIM,CEA,CNRS, F-91191 Gif Sur Yvette, France. AD - Univ Paris Diderot, AstroParticule & Cosmol, CNRS, IN2P3,CEA Irfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. AD - African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. AD - Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France. AD - Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. AD - Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. AD - Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. AD - CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. AD - CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. AD - CALTECH, Pasadena, CA 91125 USA. 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AD - Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. AD - Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki, Finland. AD - Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. AD - Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. AD - Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. AD - Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy. AD - Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. AD - Univ Roma La Sapienza, Dipartimento Fis, Ple Moro 2, Rome, Italy. AD - Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy. AD - Univ Trieste, Dipartimento Fis, Via A Valerio 2, Trieste, Italy. AD - Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, Rome, Italy. AD - European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid, Spain. AD - European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. 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AD - Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. UR - https://archimer.ifremer.fr/doc/00654/76634/ DO - 10.1051/0004-6361/201936386 KW - cosmic background radiation KW - cosmology: observations KW - cosmological parameters KW - methods: data analysis N2 - We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (l< 30) and high (l >= 30) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the Lambda CDM reionization optical-depth parameter tau to better than 15% (in combination with the TT low-l data and the high-l temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with tau. We also update the weaker constraint on tau from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the Lambda CDM constraints on the parameters theta(MC), omega(c), omega(b), and H-0 by more than 30%, and n(s) by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5 sigma level on the Lambda CDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3 sigma levels we achieved in 2015 for the temperature data alone on Lambda CDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit Lambda CDM parameters for the l< 800 and l> 800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in Lambda CDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations. Y1 - 2020/09 PB - Edp Sciences S A JF - Astronomy & Astrophysics SN - 0004-6361 VL - 641 IS - A5 ID - 76634 ER -