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

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

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.

引用

页数：39

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