Planck 2013 results. XVIII. The gravitational lensing-infrared background correlation

被引：130

作者：

Ade, P. A. R. ^{[1
,88
]}

Aghanim, N. ^{[2
,60
]}

Armitage-Caplan, C. ^{[3
,4
,93
]}

Arnaud, M. ^{[5
,9
,73
]}

Ashdown, M. ^{[6
,12
,70
]}

Atrio-Barandela, F. ^{[6
,19
,32
]}

Aumont, J. ^{[7
,34
,60
]}

Baccigalupi, C. ^{[8
,40
,87
]}

Banday, A. J. ^{[9
,50
,96
]}

Barreiro, R. B. ^{[10
,60
,67
]}

Bartlett, J. G. ^{[1
,10
,61
]}

Basak, S. ^{[10
,64
,87
]}

Battaner, E. ^{[10
,65
,97
]}

Benabed, K. ^{[10
,61
,68
]}

Benoit, A. ^{[10
,58
,87
]}

Benoit-Levy, A. ^{[10
,26
,91
]}

Bernard, J. -P. ^{[10
,95
,96
]}

Bersanelli, M. ^{[10
,36
]}

Bethermin, M. ^{[11
,73
]}

Bielewicz, P. ^{[11
,96
]}

Bobin, J. ^{[11
,73
]}

Bock, J. J. ^{[11
,68
]}

Bonaldi, A. ^{[14
,69
]}

Bond, J. R. ^{[9
,15
]}

Borrill, J. ^{[14
,16
]}

Bouchet, F. R. ^{[28
,61
]}

Boulanger, F. ^{[28
,60
]}

Bridges, M. ^{[34
,70
]}

Bucher, M. ^{[1
,37
]}

Burigana, C. ^{[39
,50
]}

Butler, R. C. ^{[39
,50
]}

Cardoso, J. -F. ^{[45
,74
,75
]}

Catalano, A. ^{[45
,76
]}

Challinor, A. ^{[45
,64
]}

Chamballu, A. ^{[47
,73
]}

Chiang, H. C. ^{[29
,48
]}

Chiang, L. -Y ^{[51
,63
]}

Christensen, P. R. ^{[51
,83
]}

Church, S. ^{[51
,92
]}

Clements, D. L. ^{[52
,56
]}

Colombi, S. ^{[52
,61
]}

Colombo, L. P. L. ^{[25
,53
]}

Couchot, F. ^{[53
,71
]}

Coulais, A. ^{[54
,72
]}

Crill, B. P. ^{[59
,68
]}

Curto, A. ^{[6
,60
]}

Cuttaia, F. ^{[50
,60
]}

Danese, L. ^{[61
,87
]}

Davies, R. D. ^{[64
,69
]}

de Bernardis, P. ^{[35
,67
]}

机构：

[1] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, CNRS,IN2P3,CEA,lrfu,APC, F-75205 Paris 13, France

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

[3] African Inst Math Sci, ZA-7701 Muizenberg, Rondebosch Cape, 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] 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 OWA, 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, 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 4, Switzerland

[19] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain

[20] Univ Oviedo, Dept Fis, Oviedo 93007, 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] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[28] Univ Helsinki, Dept Phys, Helsinki, Finland

[29] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[30] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[31] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[32] Univ Illinois, Dept Phys, Urbana, IL USA

[33] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[34] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[35] Univ Roma La Sapienza, Dept Fis, I-00185 Rome, Italy

[36] Univ Milan, Dept Phys, I-20133 Milan, Italy

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

[38] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

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

[40] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

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

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

[43] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[44] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland

[45] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[46] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[47] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[48] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy

[49] INAF Ist Radioastron, I-40129 Bologna, Italy

[50] INAF IASF Bologna, I-40129 Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

gravitational lensing: weak; cosmic background radiation; large-scale structure of Universe; dark matter; galaxies: star formation; PRE-LAUNCH STATUS; STAR-FORMING GALAXIES; SENSITIVITY HI SURVEY; DUST EMISSION; COSMOLOGICAL PARAMETERS; ANISOTROPIES; MODEL; CMB; FLUCTUATIONS; EVOLUTION;

D O I：

10.1051/0004-6361/201321540

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The multi-frequency capability of the Planck satellite provides information both on the integrated history of star formation (via the cosmic infrared background, or CIB) and on the distribution of dark matter (via the lensing effect on the cosmic microwave background, or CMB). The conjunction of these two unique probes allows us to measure directly the connection between dark and luminous matter in the high redshift (1 <= z <= 3) Universe. We use a three-point statistic optimized to detect the correlation between these two tracers, using lens reconstructions at 100, 143, and 217 GHz, together with CIB measurements at 100-857 GHz. Following a thorough discussion of possible contaminants and a suite of consistency tests, we report the first detection of the correlation between the CIB and CMB lensing. The well matched redshift distribution of these two signals leads to a detection significance with a peak value of 42/19 sigma (statistical/statistical + systematics) at 545 GHz and a correlation as high as 80% across these two tracers. Our full set of multi-frequency measurements (both CIB auto-and CIB-lensing cross-spectra) are consistent with a simple halo-based model, with a characteristic mass scale for the halos hosting CIB sources of log(10)(M/M-circle dot) = 10.5 +/- 0.6. Leveraging the frequency dependence of our signal, we isolate the high redshift contribution to the CIB, and constrain the star formation rate (SFR) density at z >= 1. We measure directly the SFR density with around 2 sigma significance for three redshift bins between z = 1 and 7, thus opening a new window into the study of the formation of stars at early times.

引用

页数：24

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