Planck 2013 results. XVI. Cosmological parameters

被引:7928
作者
Ade, P. A. R. [95 ]
Aghanim, N. [65 ]
Armitage-Caplan, C. [101 ]
Arnaud, M. [79 ]
Ashdown, M. [6 ,76 ]
Atrio-Barandela, F. [19 ]
Aumont, J. [65 ]
Baccigalupi, C. [94 ]
Banday, A. J. [10 ,104 ]
Barreiro, R. B. [72 ]
Bartlett, J. G. [1 ,74 ]
Battaner, E. [107 ]
Benabed, K. [66 ,103 ]
Benoit, A. [63 ,66 ]
Benoit-Levy, A. [26 ,66 ,103 ]
Bernard, J. -P. [10 ,104 ]
Bersanelli, M. [38 ,55 ]
Bielewicz, P. [10 ,94 ,104 ]
Bobin, J. [79 ]
Bock, J. J. [11 ,74 ]
Bonaldi, A. [75 ]
Bond, J. R. [9 ]
Borrill, J. [14 ,98 ]
Bouchet, F. R. [66 ,103 ]
Bridges, M. [6 ,69 ,76 ]
Bucher, M. [1 ]
Burigana, C. [36 ,54 ]
Butler, R. C. [54 ]
Calabrese, E. [101 ]
Cappellini, B. [55 ]
Cardoso, J. -F. [1 ,66 ,80 ,81 ]
Catalano, A. [78 ,82 ]
Challinor, A. [12 ,69 ,76 ]
Chamballu, A. [16 ,65 ,76 ]
Chary, R. -R. [62 ]
Chen, X. [62 ]
Chiang, H. C. [7 ,30 ]
Chiang, L. -Y [68 ]
Christensen, P. R. [41 ,90 ]
Church, S. [100 ]
Clements, D. L. [61 ]
Colombi, S. [66 ,103 ]
Colombo, L. P. L. [25 ,74 ]
Couchot, F. [77 ]
Coulais, A. [78 ]
Crill, B. P. [74 ,91 ]
Curto, A. [6 ,72 ]
Cuttaia, F. [54 ]
Danese, L. [94 ]
Davies, R. D. [75 ]
机构
[1] Univ Paris Diderot, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Lrfu,Observ Paris, F-75205 Paris 13, France
[2] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland
[3] African Inst Math Sci, ZA-7950 Cape Town, South Africa
[4] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy
[5] Agenzia Spaziale Italiana, I-00198 Rome, Italy
[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[7] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa
[8] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile
[9] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[10] CNRS, IRAP, F-31028 Toulouse 4, France
[11] CALTECH, Pasadena, CA 91125 USA
[12] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England
[13] CEFCA, Teruel 44001, Spain
[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
[15] CSIC, E-28006 Madrid, Spain
[16] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[17] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark
[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland
[19] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain
[20] Univ Oviedo, Dept Fis, Oviedo 33007, Spain
[21] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada
[22] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands
[23] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA
[24] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[25] Univ So Calif, Dana & David Dornsife Coll Letter, Dept Phys & Astron, Los Angeles, CA 90089 USA
[26] UCL, Dept Phys & Astron, London WC1E 6BT, England
[27] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England
[28] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA
[29] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland
[30] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[31] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[32] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[33] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[34] Univ Illinois, Dept Phys, Urbana, IL USA
[35] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[36] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy
[37] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[38] Univ Milan, Dipartimento Fis, U-20133 Milan, Italy
[39] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy
[40] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy
[41] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[42] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[43] European So Observ, ESO Vitacura, Santiago 19001, Chile
[44] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain
[45] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands
[46] Univ Turku, Finnish Ctr Astron, ESO FINCA, Piikkio 21500, Finland
[47] Haverford Coll, Dept Astron, Haverford, PA 19041 USA
[48] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland
[49] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy
[50] Osserv Astron Padova, INAF, I-35122 Padua, Italy
关键词
cosmic background radiation; cosmological parameters; early Universe; inflation; primordial nucleosynthesis; PROBE WMAP OBSERVATIONS; BARYON ACOUSTIC-OSCILLATIONS; HUBBLE-SPACE-TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; INFLATIONARY UNIVERSE SCENARIO; PRIMORDIAL MAGNETIC-FIELDS; FINE-STRUCTURE CONSTANT; SUNYAEV-ZELDOVICH; POWER-SPECTRUM; DARK-MATTER;
D O I
10.1051/0004-6361/201321591
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 greater than or similar to 40) are extremely well described by the standard spatially-flat six-parameter ACDM 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) x 10(-2), Omega(b)h(2) = 0.02205 +/- 0.00028, Omega(c)h(2) = 0.1199 +/- 0.0027, and n(s) = 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, H-0 = (67.3 +/- 1.2) km s(-1) Mpc(-1), and a high value of the matter density parameter, Omega(m) = 0.315 +/- 0.017. These values are in tension with recent direct measurements of H-0 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 ACDM 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 ACDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r(0.002) < 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 N-eff = 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 N-eff = 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 ACDM 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 less than or similar to l less than or similar to 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.
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