Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts

被引：416

作者：

Ade, P. A. R. ^{[96
]}

Aghanim, N. ^{[66
]}

Armitage-Caplan, C. ^{[102
]}

Arnaud, M. ^{[79
]}

Ashdown, M. ^{[7
,76
]}

Atrio-Barandela, F. ^{[21
]}

Aumont, J. ^{[66
]}

Baccigalupi, C. ^{[94
]}

Banday, A. J. ^{[11
,106
]}

Barreiro, R. B. ^{[73
]}

Barrena, R. ^{[72
]}

Bartlett, J. G. ^{[1
,74
]}

Battaner, E. ^{[108
]}

Battye, R. ^{[75
]}

Benabed, K. ^{[67
,105
]}

Benoit, A. ^{[64
]}

Benoit-Levy, A. ^{[29
,67
,105
]}

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

Bersanelli, M. ^{[40
,56
]}

Bielewicz, P. ^{[11
,94
,106
]}

Bikmaev, I. ^{[3
,24
]}

Blanchard, A. ^{[106
]}

Bobin, J. ^{[79
]}

Bock, J. J. ^{[12
,74
]}

Boehringer, H. ^{[86
]}

Bonaldi, A. ^{[75
]}

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

Borrill, J. ^{[16
,99
]}

Bouchet, F. R. ^{[67
,105
]}

Bourdin, H. ^{[42
]}

Bridges, M. ^{[7
,70
,76
]}

Brown, M. L. ^{[75
]}

Bucher, M. ^{[1
]}

Burenin, R. ^{[89
,98
]}

Burigana, C. ^{[38
,55
]}

Butler, R. C. ^{[55
]}

Cardoso, J. -F. ^{[1
,67
,80
]}

Carvalho, P. ^{[7
]}

Catalano, A. ^{[78
,81
]}

Challinor, A. ^{[13
,70
,76
]}

Chamballu, A. ^{[18
,66
,79
]}

Chary, R. -R. ^{[63
]}

Chiang, L. -Y ^{[69
]}

Chiang, H. C. ^{[8
,32
]}

Chon, G. ^{[86
]}

Christensen, P. R. ^{[43
,90
]}

Church, S. ^{[101
]}

Clements, D. L. ^{[62
]}

Colombi, S. ^{[67
,105
]}

Colombo, L. P. L. ^{[28
,74
]}

机构：

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

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

[3] Acad Sci Tatarstan, Kazan 420111, Russia

[4] African Inst Math Sci, ZA-7701 Rondebosch, South Africa

[5] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Frascati, Italy

[6] Agenzia Spaziale Italiana, I-00198 Rome, Italy

[7] Univ Cambridge, Astrophys Grp, Cavendish Lab, 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 7630355, Chile

[10] Univ Toronto, CITA, Toronto, ON M55 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] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal

[15] CEFCA, Teruel 44001, Spain

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

[17] CSIC, E-28006 Madrid, Spain

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

[19] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

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

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

[22] Univ Oviedo, Dept Fis, Oviedo 33007, Spain

[23] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada

[24] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia

[25] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands

[26] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA

[27] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[28] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA

[29] UCL, Dept Phys & Astron, London WC1E 6BT, England

[30] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England

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

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

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

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

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

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

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

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

[39] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

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

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

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

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

[44] ULL, Dpt Astrofis, Tenerife 38206, Spain

[45] European So Observ, Santiago 19001, Chile

[46] European Space Agcy, Planck Sci Off, Madrid 28691, Spain

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmological parameters; large-scale structure of Universe; galaxies: clusters: general; BARYON ACOUSTIC-OSCILLATIONS; MASSIVE GALAXY CLUSTERS; LARGE-SCALE STRUCTURE; X-RAY-CLUSTERS; HYDRODYNAMIC SIMULATIONS; NONTHERMAL PRESSURE; RICH CLUSTERS; XMM-NEWTON; HOT-MODEL; CONSTRAINTS;

D O I：

10.1051/0004-6361/201321521

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude sigma(8) and matter density parameter Omega(m) in a flat Lambda CDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that sigma(8) = 0.75 +/- 0.03, Omega(m) = 0.29 +/- 0.02, and sigma(8)(Omega(m)/0.27)(0.3) = 0.764 +/- 0.025. The value of sigma(8) is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find sigma(8)(Omega(m)/0.27)(0.3) = 0.78 +/- 0.01 and a tighter one-dimensional range sigma(8) = 0.77 +/- 0.02. We find that the larger values of sigma(8) and Omega(m) preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the Lambda CDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field.

引用

页数：20

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