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Title:
Planck 2013 results. XVI. Cosmological parameters
Authors:
Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cappellini, B.; Cardoso, J.-F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.-R.; Chen, X.; Chiang, H. C.; Chiang, L.-Y.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J.-M.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Gaier, T. C.; Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Haissinski, J.; Hamann, J.; Hansen, F. K.; Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hou, Z.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lattanzi, M.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Lewis, A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Menegoni, E.; Mennella, A.; Migliaccio, M.; Millea, M.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, D.; Pearson, T. J.; Peiris, H. V.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck, J.-L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; White, M.; White, S. D. M.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
Affiliation:
AA(), AB(School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, UK), AC(Institut d'Astrophysique Spatiale, CNRS UMR8617, Université Paris-Sud 11, Bâtiment 121, 91405, Orsay, France), AD(Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK), AE(Laboratoire AIM, IRFU/Service d'Astrophysique - CEA/DSM - CNRS - Université Paris Diderot, Bât. 709, CEA-Saclay, 91191, Gif-sur-Yvette Cedex, France), AF(Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge, CB3 0HE, UK), AG(Departamento de Física Fundamental, Facultad de Ciencias, Universidad de Salamanca, 37008, Salamanca, Spain), AH(Institut d'Astrophysique Spatiale, CNRS UMR8617, Université Paris-Sud 11, Bâtiment 121, 91405, Orsay, France), AI(SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AJ(Université de Toulouse, UPS-OMP, IRAP, 31028, Toulouse Cedex 4, France; CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028, Toulouse Cedex 4, France), AK(Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, 39005, Santander, Spain), AL(APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205, Paris Cedex 13, France; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), AM(University of Granada, Departamento de Física Teórica y del Cosmos, Facultad de Ciencias, 18071, Granada, Spain), AN(Institut d'Astrophysique de Paris, CNRS UMR7095, 98bis Bd Arago, 75014, Paris, France; UPMC Univ Paris 06, UMR7095, 98bis Boulevard Arago, 75014, Paris, France), AO(Institut Néel, CNRS, Université Joseph Fourier Grenoble I, 25 rue des Martyrs, 38042, Grenoble, France), AP(Department of Physics and Astronomy, University College London, London, WC1E 6BT, UK; Institut d'Astrophysique de Paris, CNRS UMR7095, 98bis Bd Arago, 75014, Paris, France; UPMC Univ Paris 06, UMR7095, 98bis Boulevard Arago, 75014, Paris, France), AQ(Université de Toulouse, UPS-OMP, IRAP, 31028, Toulouse Cedex 4, France; CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028, Toulouse Cedex 4, France), AR(Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16, 20133, Milano, Italy; via E. Bassini 15, 20133, Milano, Italy), AS(Université de Toulouse, UPS-OMP, IRAP, 31028, Toulouse Cedex 4, France; CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028, Toulouse Cedex 4, France; SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy), AT(Laboratoire AIM, IRFU/Service d'Astrophysique - CEA/DSM - CNRS - Université Paris Diderot, Bât. 709, CEA-Saclay, 91191, Gif-sur-Yvette Cedex, France), AU(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; California Institute of Technology, Pasadena, California, USA), AV(Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK), AW(CITA, University of Toronto, 60 St. George St., Toronto ON, M5S 3H8, Canada), AX(Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California, USA; Space Sciences Laboratory, University of California, Berkeley, California, USA), AY(Institut d'Astrophysique de Paris, CNRS UMR7095, 98bis Bd Arago, 75014, Paris, France; UPMC Univ Paris 06, UMR7095, 98bis Boulevard Arago, 75014, Paris, France), AZ(Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge, CB3 0HE, UK; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK), BA(APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205, Paris Cedex 13, France), BB(via Gobetti 101, 40129, Bologna, Italy; Dipartimentodi Fisica e Scienze della Terra, Università di Ferrara, via Saragat 1, 44122, Ferrara, Italy), BC(via Gobetti 101, 40129, Bologna, Italy), BD(Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK), BE(via E. 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Valerio 2, 34127, Trieste, Italy; INAF - Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy), DK(via Gobetti 101, 40129, Bologna, Italy), DL(Department of Physics, Princeton University, Princeton, New Jersey, USA), DM(LAL, Université Paris-Sud, CNRS/IN2P3, 91405, Orsay, France), DN(Theory Division, PH-TH, CERN, 1211, Geneva 23, Switzerland), DO(Institute of Theoretical Astrophysics, University of Oslo, Blindern, 0315, Oslo, Norway), DP(McGill Physics, Ernest Rutherford Physics Building, McGill University, 3600 rue University, Montréal, QC, H3A 2T8, Canada; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA; CITA, University of Toronto, 60 St. George St., Toronto ON, M5S 3H8, Canada), DQ(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, UK), DR(LAL, Université Paris-Sud, CNRS/IN2P3, 91405, Orsay, France), DS(Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan 1, planta 2, 44001, Teruel, Spain; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741, Garching, Germany), DT(Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avda. de los Castros s/n, 39005, Santander, Spain), DU(California Institute of Technology, Pasadena, California, USA), DV(Institut d'Astrophysique de Paris, CNRS UMR7095, 98bis Bd Arago, 75014, Paris, France; UPMC Univ Paris 06, UMR7095, 98bis Boulevard Arago, 75014, Paris, France), DW(Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge, CB3 0HE, UK), DX(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA), DY(DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, 2800, Kgs. 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Publication:
Astronomy & Astrophysics, Volume 571, id.A16, 66 pp. (A&A Homepage)
Publication Date:
11/2014
Origin:
EDP Sciences
Astronomy Keywords:
cosmic background radiation, cosmological parameters, early Universe, inflation, primordial nucleosynthesis
DOI:
10.1051/0004-6361/201321591
Bibliographic Code:
2014A&A...571A..16P

Abstract

This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles (l ≳ 40) are extremely well described by the standard spatially-flat six-parameter LambdaCDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be theta* = (1.04147 ± 0.00062) × 10-2, Omegabh2 = 0.02205 ± 0.00028, Omegach2 = 0.1199 ± 0.0027, and ns = 0.9603 ± 0.0073, respectively(note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H0 = (67.3 ± 1.2) km s-1 Mpc-1, and a high value of the matter density parameter, Omegam = 0.315 ± 0.017. These values are in tension with recent direct measurements of H0 and the magnitude-redshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter LambdaCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter LambdaCDM cosmology. The deviation of the scalar spectral index from unity isinsensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r0.002< 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find Neff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of Neff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = -1.13-0.10+0.13. We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter LambdaCDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. The unusual shape of the spectrum in the multipole range 20 ≲ l ≲ 40 was seen previously in the WMAP data and is a real feature of the primordial CMB anisotropies. The poor fit to the spectrum at low multipoles is not of decisive significance, but is an "anomaly" in an otherwise self-consistent analysis of the Planck temperature data.

Associated Articles

Part  1     Part  2     Part  3     Part  4     Part  5     Part  6     Part  7     Part  8     Part  9     Part 10     Part 11     Part 12     Part 13     Part 14     Part 15     Part 16     Part 17     Part 18     Part 19     Part 20     Part 21     Part 22     Part 23     Part 24     Part 25     Part 26     Part 27     Part 28     Part 29     Part 30     Part 31    


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