Planck intermediate results V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect

被引:257
作者
Ade, P. A. R. [90 ]
Aghanim, N. [60 ]
Arnaud, M. [75 ]
Ashdown, M. [6 ,72 ]
Atrio-Barandela, F. [19 ]
Aumont, J. [60 ]
Baccigalupi, C. [89 ]
Balbi, A. [38 ]
Banday, A. J. [9 ,98 ]
Barreiro, R. B. [69 ]
Bartlett, J. G. [1 ,70 ]
Battaner, E. [101 ]
Benabed, K. [61 ,96 ]
Benoit, A. [58 ]
Bernard, J. -P. [9 ]
Bersanelli, M. [35 ,52 ]
Bhatia, R. [7 ]
Bikmaev, I. [3 ,21 ]
Bobin, J. [75 ]
Boehringer, H. [83 ]
Bonaldi, A. [71 ]
Bond, J. R. [8 ]
Borgani, S. [36 ,49 ]
Borrill, J. [14 ,93 ]
Bouchet, F. R. [61 ,96 ]
Bourdin, H. [38 ]
Brown, M. L. [71 ]
Burenin, R. [91 ]
Burigana, C. [37 ,51 ]
Cabella, P. [39 ]
Cardoso, J. -F. [1 ,61 ,76 ,77 ]
Carvalho, P. [6 ]
Castex, G. [1 ]
Catalano, A. [74 ,78 ]
Cayon, L. [32 ]
Chamballu, A. [56 ]
Chiang, L. -Y [65 ]
Chon, G. [83 ]
Christensen, P. R. [40 ,86 ]
Churazov, E. [82 ,92 ]
Clements, D. L. [56 ]
Colafrancesco, S. [48 ]
Colombi, S. [61 ,96 ]
Colombo, L. P. L. [24 ,70 ]
Comis, B. [78 ]
Coulais, A. [74 ]
Crill, B. P. [70 ,87 ]
Cuttaia, F. [51 ]
Da Silva, A. [12 ]
Dahle, H. [11 ,67 ]
机构
[1] Univ Paris Diderot, CNRS IN2P3, CEA Lrfu, APC AstroParticule & Cosmol,Observ Paris, F-75205 Paris 13, France
[2] Aalto Univ, Metsahovi Radio Observ, Kylamala 02540, Finland
[3] Acad Sci Tatarstan, Kazan 420111, Russia
[4] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy
[5] Agenzia Spaziale Italiana, Rome, Italy
[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[7] ALMA Santiago Cent Offices, Santiago, Chile
[8] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[9] CNRS, IRAP, F-31028 Toulouse 4, France
[10] CALTECH, Pasadena, CA 91125 USA
[11] Univ Oslo, Ctr Math Applicat, Oslo, Norway
[12] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal
[13] CEFCA, 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, 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, E-33007 Oviedo, Spain
[21] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia
[22] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands
[23] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[24] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA
[25] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England
[26] Univ Helsinki, Dept Phys, Helsinki, Finland
[27] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[28] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[29] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[30] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[31] Univ Illinois, Dept Phys, Urbana, IL USA
[32] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA
[33] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[34] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[35] Univ Milan, Dipartimento Fis, Milan, Italy
[36] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy
[37] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy
[38] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy
[39] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy
[40] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[41] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain
[42] ESO Vitacura, European So Observ, Santiago 19001, Chile
[43] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain
[44] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands
[45] Observ Paris, GEPI, F-92195 Meudon, France
[46] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland
[47] INAF Osservatorio Astron Padova, Padua, Italy
[48] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy
[49] INAF Osservatorio Astron Trieste, Trieste, Italy
[50] INAF Ist Radioastron, Bologna, Italy
关键词
cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; submillimeter: general; X-rays: general; INTRACLUSTER GAS TEMPERATURE; X-RAY MEASUREMENTS; REPRESENTATIVE SAMPLE; DARK-MATTER; XMM-NEWTON; COSMOLOGICAL SIMULATIONS; COMPONENT SEPARATION; SCALING PROPERTIES; ASTRONOMICAL DATA; HOT GAS;
D O I
10.1051/0004-6361/201220040
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal indicates that most clusters are individually detected at least out to R-500. By stacking the radial profiles, we have statistically detected the radial SZ signal out to 3 x R-500, i. e., at a density contrast of about 50-100, though the dispersion about the mean profile dominates the statistical errors across the whole radial range. Our measurement is fully consistent with previous Planck results on integrated SZ fluxes, further strengthening the agreement between SZ and X-ray measurements inside R-500. Correcting for the effects of the Planck beam, we have calculated the corresponding pressure profiles. This new constraint from SZ measurements is consistent with the X-ray constraints from XMM-Newton in the region in which the profiles overlap (i. e., [0.1-1] R-500), and is in fairly good agreement with theoretical predictions within the expected dispersion. At larger radii the average pressure profile is slightly flatter than most predictions from numerical simulations. Combining the SZ and X-ray observed profiles into a joint fit to a generalised pressure profile gives best-fit parameters [P-0, c(500), gamma, alpha, beta] = [6.41, 1.81, 0.31, 1.33, 4.13]. Using a reasonable hypothesis for the gas temperature in the cluster outskirts we reconstruct from our stacked pressure profile the gas mass fraction profile out to 3 R-500. Within the temperature driven uncertainties, our Planck constraints are compatible with the cosmic baryon fraction and expected gas fraction in halos.
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