Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation

被引：169

作者：

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

Aghanim, N. ^{[62
]}

Armitage-Caplan, C. ^{[96
]}

Arnaud, M. ^{[75
]}

Ashdown, M. ^{[7
,72
]}

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

Aumont, J. ^{[62
]}

Baccigalupi, C. ^{[90
]}

Banday, A. J. ^{[11
,99
]}

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

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

Battaner, E. ^{[101
]}

Benabed, K. ^{[63
,98
]}

Benoit, A. ^{[60
]}

Benoit-Levy, A. ^{[26
,63
,98
]}

Bernard, J. -P. ^{[11
,99
]}

Bersanelli, M. ^{[37
,53
]}

Bethermin, M. ^{[75
]}

Bielewicz, P. ^{[11
,90
,99
]}

Blagrave, K. ^{[10
]}

Bobin, J. ^{[75
]}

Bock, J. J. ^{[12
,70
]}

Bonaldi, A. ^{[71
]}

Bond, J. R. ^{[10
]}

Borrill, J. ^{[15
,93
]}

Bouchet, F. R. ^{[63
,98
]}

Boulanger, F. ^{[62
]}

Bridges, M. ^{[7
,66
,72
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[35
,52
]}

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

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

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

Challinor, A. ^{[13
,66
,72
]}

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

Chen, X. ^{[59
]}

Chiang, H. C. ^{[8
,29
]}

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

Christensen, P. R. ^{[40
,86
]}

Church, S. ^{[95
]}

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

Colombi, S. ^{[63
,98
]}

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

Couchot, F. ^{[73
]}

Coulais, A. ^{[74
]}

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

Curto, A. ^{[7
,69
]}

Cuttaia, F. ^{[52
]}

Danese, L. ^{[90
]}

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

机构：

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

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

[3] African Inst Math Sci, ZA-7945 Cape Town, South Africa

[4] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy

[5] Agenzia Spaziale Italiana, Rome, Italy

[6] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany

[7] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[8] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[9] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile

[10] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

[11] CNRS, IRAP, F-31028 Toulouse 4, France

[12] CALTECH, Pasadena, CA 91125 USA

[13] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England

[14] CEFCA, Teruel 44001, Spain

[15] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[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 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, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, 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, FIN-00014 Helsinki, Finland

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

[30] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

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

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

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

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

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

[36] Univ Roma La Sapienza, Dipartimento Fis, I-00135 Rome, Italy

[37] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[38] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

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

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

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

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

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

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

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

[46] Haverford Coll, Dept Astron, Haverford, PA 19041 USA

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

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

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

[50] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmology: observations; large-scale structure of Universe; galaxies: star formation; infrared: diffuse background; CONDITIONAL LUMINOSITY FUNCTION; FORMATION RATE DENSITY; DARK-MATTER HALOES; 100; MU-M; DUST EMISSION; STELLAR MASS; SUBMILLIMETER GALAXIES; NON-GAUSSIANITY; POWER SPECTRUM; NUMBER COUNTS;

D O I：

10.1051/0004-6361/201322093

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new measurements of cosmic infrared background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto-and cross-frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg(2), respectively. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles l similar to 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from l similar to 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-) halo mass. The two approaches simultaneously fit all auto-and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (M-eff/ M-circle dot) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation.

引用

页数：39

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