Planck 2013 results. XVII. Gravitational lensing by large-scale structure

被引:340
作者
Ade, P. A. R.
Aghanim, N. [65 ]
Armitage-Caplan, C. [100 ]
Arnaud, M. [78 ]
Ashdown, M. [6 ,75 ]
Atrio-Barandela, E. [19 ]
Aumont, J. [65 ]
Baccigalupi, C. [93 ]
Banday, A. J. [10 ,103 ]
Barreiro, R. B. [72 ]
Bartlett, J. G. [1 ,73 ]
Basak, S. [93 ]
Battaner, E. [104 ]
Benabed, K. [66 ,102 ]
Benoit, A. [63 ]
Benoit-Levy, A. [26 ,66 ,102 ]
Bernard, J. -P. [10 ,103 ]
Bersanelli, M. [39 ,56 ]
Bielewicz, P. [10 ,93 ,103 ]
Bobin, J. [78 ]
Bock, J. J. [11 ,73 ]
Bonaldi, A. [74 ]
Bonavera, L. [72 ]
Bond, J. R. [9 ]
Borrill, J. [14 ,97 ]
Bouchet, F. R. [66 ,102 ]
Bridges, M. [6 ,69 ,75 ]
Bucher, M. [1 ]
Burigana, C. [37 ,55 ]
Butler, R. C. [55 ]
Cardoso, J. -F. [1 ,66 ,79 ,80 ]
Catalano, A. [77 ,81 ]
Challinor, A. [12 ,69 ,75 ]
Chamballu, A. [16 ,65 ,78 ]
Chiang, H. C. [7 ,31 ]
Chiang, L. -Y [68 ]
Christensen, P. R. [42 ,89 ]
Church, S. [99 ]
Clements, D. L. [61 ]
Colombi, S. [66 ,102 ]
Colombo, L. P. L. [25 ,73 ]
Couchot, F. [76 ]
Coulais, A. [77 ]
Crill, B. P. [73 ,90 ]
Curto, A. [6 ,72 ]
Cuttaia, F. [55 ]
Danese, L. [93 ]
Davies, R. D. [74 ]
Davis, R. J. [74 ]
de Bernardis, P. [38 ]
机构
[1] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS,IN2P3,CEA,lrfu,APC, F-75205 Paris 13, France
[2] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland
[3] African Inst Math Sci, Cape Town, South Africa
[4] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy
[5] Agenzia Spaziale Italiana, 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] Atacama Large Millimeter Submillimeter Array, ALMA Santiago Cent Off, Santiago 7630355, 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, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England
[13] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain
[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
[15] CSIC, Madrid, Spain
[16] CEA Saclay, DMS, SPP, Irfu, 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 4, Switzerland
[19] Univ Salamanca, Dept Fis Fundamental, Fac Ciencias, E-37008 Salamanca, Spain
[20] Univ Oviedo, Dept Fis, E-33007 Oviedo, 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] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA
[29] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA
[30] Univ Helsinki, Dept Phys, Helsinki, Finland
[31] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[32] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[33] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[34] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[35] Univ Illinois, Dept Phys, Urbana, IL USA
[36] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[37] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy
[38] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[39] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy
[40] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy
[41] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy
[42] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[43] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[44] European So Observ, ESO Vitacura, Santiago 19001, Chile
[45] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain
[46] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands
[47] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland
[48] Haverford Coll, Dept Astron, Haverford, PA USA
[49] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland
[50] INAF Osservatorio Astrofis Catania, Catania, Italy
基金
英国科学技术设施理事会;
关键词
gravitational lensing: weak; methods: data analysis; cosmic background radiation; large-scale structure of Universe; MICROWAVE BACKGROUND ANISOTROPIES; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; CROSS-CORRELATION; NON-GAUSSIANITY; DAMPING TAIL; SKY MAPS; GALAXIES; RECONSTRUCTION; MODEL;
D O I
10.1051/0004-6361/201321543
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
On the arcminute angular scales probed by Planck, the cosmic microwave background (CMB) anisotropies are gently perturbed by gravitational lensing. Here we present a detailed study of this effect, detecting lensing independently in the 100, 143, and 217 GHz frequency bands with an overall significance of greater than 25 sigma. We use the temperature-gradient correlations induced by lensing to reconstruct a (noisy) map of the CMB lensing potential, which provides an integrated measure of the mass distribution back to the CMB last-scattering surface. Our lensing potential map is significantly correlated with other tracers of mass, a fact which we demonstrate using several representative tracers of large-scale structure. We estimate the power spectrum of the lensing potential, finding generally good agreement with expectations from the best-fitting ACDM model for the Planck temperature power spectrum, showing that this measurement at z = 1100 correctly predicts the properties of the lower-redshift, later-time structures which source the lensing potential. When combined with the temperature power spectrum, our measurement provides degeneracy-breaking power for parameter constraints; it improves CMB-alone constraints on curvature by a factor of two and also partly breaks the degeneracy between the amplitude of the primordial perturbation power spectrum and the optical depth to reionization, allowing a measurement of the optical depth to reionization which is independent of large-scale polarization data. Discarding scale information, our measurement corresponds to a 4% constraint on the amplitude of the lensing potential power spectrum, or a 2% constraint on the root-mean-squared amplitude of matter fluctuations at z similar to 2.
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页数:39
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