Planck 2013 results. XXII. Constraints on inflation

被引：1525

作者：

Ade, P. A. R. ^{[91
]}

Aghanim, N. ^{[62
]}

Armitage-Caplan, C. ^{[97
]}

Arnaud, M. ^{[75
]}

Ashdown, M. ^{[6
,72
]}

Atrio-Barandela, F. ^{[19
]}

Aumont, J. ^{[62
]}

Baccigalupi, C. ^{[90
]}

Banday, A. J. ^{[10
,100
]}

Barreiro, R. B. ^{[69
]}

Bartlett, J. G. ^{[1
,70
]}

Bartolo, N. ^{[35
]}

Battaner, E. ^{[101
]}

Benabed, K. ^{[63
,99
]}

Benoit, A. ^{[60
]}

Benoit-Levy, A. ^{[26
,63
,99
]}

Bernard, J. -P. ^{[10
,100
]}

Bersanelli, M. ^{[38
,53
]}

Bielewicz, P. ^{[10
,90
,100
]}

Bobin, J. ^{[70
,75
]}

Bock, J. J. ^{[11
,70
]}

Bonaldi, A. ^{[71
]}

Bond, J. R. ^{[9
]}

Borrill, J. ^{[14
,94
]}

Bouchet, F. R. ^{[63
,99
]}

Bridges, M. ^{[6
,66
,72
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[36
,52
]}

Butler, R. C. ^{[52
]}

Calabrese, E. ^{[97
]}

Cardoso, J. -F. ^{[1
,63
,76
,77
]}

Catalano, A. ^{[74
,78
]}

Challinor, A. ^{[12
,66
,72
]}

Chamballu, A. ^{[16
,62
,75
]}

Chiang, H. C. ^{[7
,30
]}

Chiang, L. -Y. ^{[65
]}

Christensen, P. R. ^{[41
,86
]}

Church, S. ^{[96
]}

Clements, D. L. ^{[58
]}

Colombi, S. ^{[63
,99
]}

Colombo, L. P. L. ^{[25
,70
]}

Couchot, F. ^{[73
]}

Coulais, A. ^{[74
]}

Crill, B. P. ^{[70
,87
]}

Curto, A. ^{[6
,69
]}

Cuttaia, F. ^{[52
]}

Danese, L. ^{[90
]}

Davies, R. D. ^{[71
]}

Davis, R. J. ^{[71
]}

de Bernardis, P. ^{[37
]}

机构：

[1] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[3] African Inst Math Sci, ZA-7701 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, Vitacura 7630355, Casilla, 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] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

[14] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[15] CSIC, Madrid 28006, Spain

[16] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[17] Tech Univ Denmark, Natl Space Inst, DTU Space, Lyngby 2800, Denmark

[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[19] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, Salamanca 37008, 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, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, 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 USA

[29] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland

[30] Princeton Univ, Dept Phys, Princeton, NJ 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, I-20133 Milan, Italy

[39] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[40] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy

[41] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[42] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[43] European So Observ, ESO Vitacura, Santiago 19001, Chile

[44] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain

[45] European Space Agcy, ESTEC, NL-2201 AZ Noordwijk, Netherlands

[46] Haverford Coll, Astron Dept, Haverford, PA USA

[47] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[48] INAF Osserv Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[49] Osserv Astrofis Roma, I-00040 Monte Porzio Catone, Italy

[50] INAF Osserv Astron Trieste, I-34131 Trieste, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmic background radiation; inflation; early Universe; PROBE WMAP OBSERVATIONS; BARYON ACOUSTIC-OSCILLATIONS; ISOTHERMAL DENSITY PERTURBATIONS; PARTICLE PHYSICS MODELS; HUBBLE-SPACE-TELESCOPE; LARGE-SCALE STRUCTURE; COSMOLOGICAL PERTURBATIONS; POWER SPECTRUM; BACKGROUND ANISOTROPY; QUANTUM FLUCTUATIONS;

D O I：

10.1051/0004-6361/201321569

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyse the implications of the Planck data for cosmic inflation. The Planck nominal mission temperature anisotropy measurements, combined with the WMAP large-angle polarization, constrain the scalar spectral index to be n(s) = 0.9603 +/- 0:0073, ruling out exact scale invariance at over 5 sigma Planck establishes an upper bound on the tensor-to-scalar ratio of r < 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models preferring potentials with V '' < 0. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n >= 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn(s)/dln k = -0.0134 +/- 0.0090. We verify these conclusions through a numerical analysis, which makes no slowroll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by delta 2 10; however, Bayesian evidence does not prefer these models. We constrain several single-field inflation models with generalized Lagrangians by combining power spectrum data with Planck bounds on fNL. Planck constrains with unprecedented accuracy the amplitude and possible correlation (with the adiabatic mode) of non-decaying isocurvature fluctuations. The fractional primordial contributions of cold dark matter (CDM) isocurvature modes of the types expected in the curvaton and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelated isocurvature component can improve the 2 by approximately 4 as a result of slightly lowering the theoretical prediction for the 40 multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions.

引用

页数：42

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