Planck early results. IX. XMM-Newton follow-up for validation of Planck cluster candidates

被引:116
作者
Aghanim, N. [47 ]
Arnaud, M. [58 ]
Ashdown, M. [5 ,56 ]
Aumont, J. [47 ]
Baccigalupi, C. [68 ]
Balbi, A. [30 ]
Banday, A. J. [1 ,8 ,64 ]
Barreiro, R. B. [53 ]
Bartelmann, M. [64 ,76 ]
Bartlett, J. G. [4 ,54 ]
Battaner, E. [77 ]
Benabed, K. [48 ]
Benoit, A. [46 ]
Bernard, J-P [1 ,8 ]
Bersanelli, M. [27 ,41 ]
Bhatia, R. [6 ]
Bock, J. J. [54 ]
Bonaldi, A. [37 ]
Bond, J. R. [7 ]
Borrill, J. [63 ,72 ]
Bouchet, F. R. [48 ]
Brown, M. L. [5 ,56 ]
Bucher, M. [4 ]
Burigana, C. [40 ]
Cabella, P. [30 ]
Cantalupo, C. M. [63 ]
Cardoso, J-F [4 ,48 ,59 ,60 ]
Carvalho, P. [5 ]
Catalano, A. [4 ,57 ]
Cayon, L. [20 ]
Challinor, A. [11 ,50 ,56 ]
Chamballu, A. [44 ]
Chiang, L-Y [49 ]
Chon, G. [5 ,65 ]
Christensen, P. R. [31 ]
Churazov, E. [64 ,71 ]
Clements, D. L. [44 ]
Colafrancesco, S. [38 ]
Colombi, S. [48 ]
Couchot, F. [62 ]
Coulais, A. [57 ]
Crill, B. P. [54 ]
Cuttaia, F. [40 ]
Da Silva, A. [10 ]
Dahle, H. [9 ,51 ]
Danese, L. [68 ]
de Bernardis, P. [26 ]
de Gasperis, G. [30 ]
de Rosa, A. [40 ]
de Zotti, G. [37 ,68 ]
机构
[1] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France
[2] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland
[3] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy
[4] Univ Paris 07, CNRS, UMR7164, Paris, France
[5] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[6] ALMA Santiago Cent Off, Santiago, Chile
[7] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[8] IRAP, CNRS, F-31028 Toulouse 4, France
[9] Univ Oslo, Ctr Math Applicat, Oslo, Norway
[10] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal
[11] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England
[12] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[13] Natl Space Inst, DTU Space, Copenhagen, Denmark
[14] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain
[15] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada
[16] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[17] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA
[18] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England
[19] Univ Helsinki, Dept Phys, Helsinki, Finland
[20] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[21] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[22] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[23] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[24] Univ Illinois, Dept Phys, Urbana, IL USA
[25] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy
[26] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[27] Univ Milan, Dipartimento Fis, Milan, Italy
[28] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy
[29] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy
[30] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy
[31] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[32] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain
[33] European So Observ, ESO Vitacura, Santiago 19, Chile
[34] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain
[35] European Space Agcy, ESTEC, NL-2201 AZ Noordwijk, Netherlands
[36] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland
[37] Osserv Astron Padova, INAF, Padua, Italy
[38] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy
[39] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy
[40] IASF Bologna, INAF, Bologna, Italy
[41] IASF Milano, INAF, Milan, Italy
[42] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France
[43] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France
[44] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England
[45] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA
[46] Univ Grenoble 1, CNRS, Inst Neel, F-38041 Grenoble, France
[47] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France
[48] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France
[49] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan
[50] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
关键词
cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters; PRE-LAUNCH STATUS; MASSIVE GALAXY CLUSTERS; PHOTON IMAGING CAMERA; X-RAY-PROPERTIES; REPRESENTATIVE SAMPLE; SCALING RELATIONS; PROFILES; REXCESS; CHANDRA; GAS;
D O I
10.1051/0004-6361/201116460
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (similar to 10 ks) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (4 < S/N < 6), and a further 15 in a programme to observe a sample of S/N > 5 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N <= 4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about similar to 70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z = 0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09 less than or similar to z less than or similar to 0.54, with a median redshift of z similar to 0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y-500. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y-500-Y-X relation established for X-ray selected objects, where Y-X is the product of the gas mass and temperature.
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