Planck intermediate results X. Physics of the hot gas in the Coma cluster

被引：92

作者：

Ade, P. A. R. ^{[94
]}

Aghanim, N. ^{[63
]}

Arnaud, M. ^{[78
]}

Ashdown, M. ^{[6
,75
]}

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

Aumont, J. ^{[63
]}

Baccigalupi, C. ^{[93
]}

Balbi, A. ^{[38
,63
]}

Banday, A. J. ^{[9
,103
]}

Barreiro, R. B. ^{[71
]}

Bartlett, J. G. ^{[1
,72
]}

Battaner, E. ^{[105
]}

Benabed, K. ^{[64
,100
]}

Benoit, A. ^{[61
,63
]}

Bernard, J. -P. ^{[9
]}

Bersanelli, M. ^{[35
,53
]}

Bikmaev, I. ^{[3
,21
]}

Boehringer, H. ^{[86
]}

Bonaldi, A. ^{[63
,73
]}

Bond, J. R. ^{[8
]}

Borrill, J. ^{[14
,97
]}

Bouchet, F. R. ^{[64
,100
]}

Bourdin, H. ^{[38
]}

Brown, M. L. ^{[73
]}

Brown, S. D. ^{[25
]}

Burenin, R. ^{[95
]}

Burigana, C. ^{[37
,52
]}

Cabella, P. ^{[39
]}

Cardoso, J. -F. ^{[1
,64
,79
,80
]}

Carvalho, P. ^{[6
]}

Catalano, A. ^{[77
,81
]}

Cayon, L. ^{[32
]}

Chiang, L. -Y ^{[67
]}

Chon, G. ^{[86
]}

Christensen, P. R. ^{[40
,90
]}

Churazov, E. ^{[85
,96
]}

Clements, D. L. ^{[59
]}

Colafrancesco, S. ^{[49
]}

Colombo, L. P. L. ^{[24
,72
]}

Coulais, A. ^{[77
]}

Crill, B. P. ^{[72
,91
]}

Cuttaia, F. ^{[52
]}

Da Silva, A. ^{[12
]}

Dahle, H. ^{[11
,69
]}

Danese, L. ^{[93
]}

Davis, R. J. ^{[73
]}

de Bernardis, P. ^{[34
]}

de Gasperis, G. ^{[38
]}

de Rosa, A. ^{[52
]}

de Zotti, G. ^{[48
,93
]}

机构：

[1] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 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, Atacama Large Millimeter Submillimeter Array, Santiago 7630355, Chile

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

[9] IRAP, CNRS, 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, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark

[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, 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, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

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

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

[25] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA

[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, Dipartimento Fis, Trieste, Italy

[37] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy

[38] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, Rome, Italy

[39] Univ Roma Tor Vergata, Dipartimento Matemat, 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] Planck Sci Off, ESAC, European Space Agcy, Madrid, Spain

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

[45] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France

[46] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland

[47] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy

[48] Osserv Astrofis Catania, INAF, I-35131 Padua, Italy

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

[50] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 554卷

基金：

美国国家科学基金会;

关键词：

galaxies: clusters: individual: Coma cluster; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters; cosmology: observations; galaxies: clusters: general; cosmic background radiation; LARGE-SCALE STRUCTURE; PRE-LAUNCH STATUS; SIMULATED GALAXY CLUSTERS; SUNYAEV-ZELDOVICH; RADIO HALOS; SHOCK-WAVES; MAGNETIC-FIELD; TEMPERATURE STRUCTURE; HADRONIC MODELS; COSMIC-RAYS;

D O I：

10.1051/0004-6361/201220247

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r approximate to 3 x R-500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R-500; by r = 2 x R-500 it underestimates the observed y profile by a factor of similar or equal to 2. This may indicate that at these larger radii either: i) the cluster SZ emission is contaminated by unresolved SZ sources along the line of sight; or ii) the pressure profile of Coma is higher at r > R-500 than the mean pressure profile predicted by the simulations used to constrain the models. The Planck image shows significant local steepening of the y profile in two regions about half a degree to the west and to the south-east of the cluster centre. These features are consistent with the presence of shock fronts at these radii, and indeed the western feature was previously noticed in the ROSAT PSPC mosaic as well as in the radio. Using Planck y profiles extracted from corresponding sectors we find pressure jumps of 4.9(-0.2)(+0.4) and 5.0(-0.1)(+1.3) in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number M-w = 2.03(-0.04)(+0.09) and M-se = 2.05(-0.02)(+0.25) in the west and south-east, respectively. Finally, we find that the y and radio-synchrotron signals are quasi-linearly correlated on Mpc scales, with small intrinsic scatter. This implies either that the energy density of cosmic-ray electrons is relatively constant throughout the cluster, or that the magnetic fields fall off much more slowly with radius than previously thought.

引用

页数：19

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