Planck 2018 results: VI. Cosmological parameters

被引:5548
作者
Aghanim, N. [54 ]
Akrami, Y. [15 ,57 ,59 ]
Ashdown, M. [5 ,65 ]
Aumont, J. [96 ]
Baccigalupi, C. [79 ]
Ballardini, M. [21 ,41 ]
Banday, A. J. [8 ,96 ]
Barreiro, R. B. [61 ]
Bartolo, N. [29 ,62 ]
Basak, S. [86 ]
Battye, R. [64 ]
Benabed, K. [55 ,91 ]
Bernard, J. -P. [8 ,96 ]
Bersanelli, M. [32 ,45 ]
Bielewicz, P. [76 ,79 ]
Bock, J. J. [10 ,63 ]
Bond, J. R. [7 ]
Borrill, J. [12 ,94 ]
Bouchet, F. R. [55 ,91 ]
Boulanger, F. [54 ,55 ,90 ]
Bucher, M. [2 ,6 ]
Burigana, C. [30 ,44 ,47 ]
Butler, R. C. [41 ]
Calabrese, E. [83 ]
Cardoso, J. -F. [55 ,91 ]
Carron, J. [23 ]
Challinor, A. [11 ,58 ,65 ]
Chiang, H. C. [6 ,25 ]
Chluba, J. [64 ]
Colombo, L. P. L. [32 ]
Combet, C. [68 ]
Contreras, D. [20 ]
Crill, B. P. [10 ,63 ]
Cuttaia, F. [41 ]
de Bernardis, P. [31 ]
de Zotti, G. [42 ]
Delabrouille, J. [2 ]
Delouis, J. -M. [67 ]
Di Valentino, E. [64 ]
Diego, J. M. [61 ]
Dore, O. [10 ,63 ]
Douspis, M. [54 ]
Ducout, A. [66 ]
Dupac, X. [35 ]
Dusini, S. [62 ]
Efstathiou, G. [58 ,65 ]
Elsner, F. [73 ]
Ensslin, T. A. [73 ]
Eriksen, H. K. [59 ]
Fantaye, Y. [3 ,19 ]
机构
[1] Univ Paris Diderot, Univ Paris Saclay, CNRS, AIM,CEA,Sorbonne Paris Cite, F-91191 Gif Sur Yvette, France
[2] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,AstroParticule & Cosmol,CNRS,IN2P3,CEA,Irfu, 10 rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France
[3] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa
[4] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
[5] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England
[6] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa
[7] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada
[8] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse, France
[9] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA
[10] CALTECH, Pasadena, CA 91125 USA
[11] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England
[12] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA
[13] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark
[14] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland
[15] PSL Res Univ, CNRS, Dept Phys, Ecole Normale Super, 24 Rue Lhomond, F-75005 Paris, France
[16] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain
[17] Univ Oviedo, Dept Fis, C Federico Garcia Lorca 18, Oviedo, Spain
[18] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands
[19] Univ Stellenbosch, Dept Math, ZA-7602 Stellenbosch, South Africa
[20] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada
[21] Univ Western Cape, Dept Phys & Astron, ZA-7535 Cape Town, South Africa
[22] UCL, Dept Phys & Astron, London WC1E 6BT, England
[23] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England
[24] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki, Finland
[25] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[26] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[27] Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA
[28] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[29] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy
[30] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy
[31] Univ Sapienza, Dipartimento Fis, Ple Moro 2, Rome, Italy
[32] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy
[33] Univ Trieste, Dipartimento Fis, Via Valerio 2, Trieste, Italy
[34] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci, Rome, Italy
[35] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid, Spain
[36] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands
[37] INFN, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy
[38] Argonne Natl Lab, HEP Div, Lemont, IL 60439 USA
[39] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA
[40] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki, Finland
[41] INAF OAS Bologna, Ist Nazl Astrofis, Osservatorio Astrofis & Sci Spazio Bologna, Area Ric,CNR, Via Gobetti 101, I-40129 Bologna, Italy
[42] INAF Osservatorio Astronomico Padova, Vicolo Osservatorio 5, Padua, Italy
[43] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, Trieste, Italy
[44] INAF, Ist Radioastron, Via Piero Gobetti 101, I-40129 Bologna, Italy
[45] INAF IASF Milano, Via E Bassini 15, Milan, Italy
[46] INFN CNAF, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[47] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[48] INFN, Sez Ferrara, Via Saragat 1, I-44122 Ferrara, Italy
[49] INFN, Sez Milano, Via Celoria 16, Milan, Italy
[50] Univ Roma Sapienza, INFN, Sez Roma 1, Piazzale Aldo Moro 2, I-00185 Rome, Italy
基金
欧洲研究理事会; 英国科学技术设施理事会;
关键词
cosmic background radiation; cosmological parameters; OSCILLATION SPECTROSCOPIC SURVEY; BARYON ACOUSTIC-OSCILLATIONS; MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; GALAXY REDSHIFT SURVEY; ACCURATE HALO-MODEL; POWER-SPECTRUM; DARK ENERGY; GROWTH-RATE; INFLATIONARY PARADIGM;
D O I
10.1051/0004-6361/201833910
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5 sigma level. We find good consistency with the standard spatially-flat 6-parameter Lambda CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base Lambda CDM" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density Omega (c)h(2)=0.120 +/- 0.001, baryon density Omega (b)h(2)=0.0224 +/- 0.0001, scalar spectral index n(s)=0.965 +/- 0.004, and optical depth tau =0.054 +/- 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100 theta (*)=1.0411 +/- 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-Lambda CDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H-0=(67.4 +/- 0.5) km s(-1) Mpc(-1); matter density parameter Omega (m)=0.315 +/- 0.007; and matter fluctuation amplitude sigma (8)=0.811 +/- 0.006. We find no compelling evidence for extensions to the base-Lambda CDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be N-eff=2.99 +/- 0.17, in agreement with the Standard Model prediction N-eff=3.046, and find that the neutrino mass is tightly constrained to Sigma m(nu)< 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base <Lambda>CDM at over 2 sigma, which pulls some parameters that affect the lensing amplitude away from the Lambda CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, Omega (K)=0.001 +/- 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w(0)=-1.03 +/- 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r(0.002)< 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-<Lambda>CDM cosmology are in excellent agreement with observations. The Planck base-Lambda CDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey's combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6 sigma, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data.
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