Planck intermediate results I. Further validation of new Planck clusters with XMM-Newton

被引：52

作者：

Aghanim, N. ^{[54
]}

Arnaud, M. ^{[1
]}

Ashdown, M. ^{[6
,66
]}

Atrio-Barandela, F. ^{[18
]}

Aumont, J. ^{[54
]}

Baccigalupi, C. ^{[76
]}

Balbi, A. ^{[35
]}

Banday, A. J. ^{[9
,84
]}

Barreiro, R. B. ^{[62
]}

Bartlett, J. G. ^{[2
,64
]}

Battaner, E. ^{[86
]}

Benabed, K. ^{[55
,82
]}

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

Bersanelli, M. ^{[32
,48
]}

Boehringer, H. ^{[74
]}

Bonaldi, A. ^{[65
]}

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

Borrill, J. ^{[14
,80
]}

Bouchet, F. R. ^{[55
,82
]}

Bourdin, H. ^{[35
]}

Brown, M. L. ^{[65
]}

Burigana, C. ^{[34
,47
]}

Butler, R. C. ^{[47
]}

Cabella, P. ^{[36
]}

Cardoso, J. -F. ^{[2
,55
,69
,70
]}

Carvalho, P. ^{[6
]}

Catalano, A. ^{[68
,71
]}

Cayon, L. ^{[25
]}

Chamballu, A. ^{[52
]}

Chary, R. -R. ^{[53
]}

Chiang, L. -Y. ^{[58
]}

Chon, G. ^{[74
]}

Christensen, P. R. ^{[37
]}

Clements, D. L. ^{[52
]}

Colafrancesco, S. ^{[44
]}

Colombi, S. ^{[55
]}

Coulais, A. ^{[68
]}

Crill, B. P. ^{[64
]}

Cuttaia, F. ^{[47
]}

da Silva, A. ^{[12
]}

Dahle, H. ^{[11
,60
]}

Davis, R. J. ^{[65
]}

de Bernardis, P. ^{[31
]}

de Gasperis, G. ^{[35
]}

de Zotti, G. ^{[43
,76
]}

Delabrouille, J. ^{[2
]}

Democles, J. ^{[1
]}

Desert, F. -X. ^{[51
]}

Diego, J. M. ^{[62
]}

Dolag, K. ^{[73
,85
]}

机构：

[1] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,IRFU Serv Astrophys,CEA DSM, Bat 709, F-91191 Gif Sur Yvette, France

[2] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris, Paris 13, France

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

[4] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy

[5] Argelander Inst Astron, D-53121 Bonn, Germany

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

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

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

[9] IRAP, CNRS, 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] Natl Space Inst, DTU Space, Copenhagen, Denmark

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

[19] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain

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

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

[22] Univ So Calif, Dept Phys & Astron, Los Angeles, CA USA

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

[24] Univ Helsinki, Dept Phys, Helsinki, Finland

[25] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA

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

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

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

[29] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

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

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

[32] Univ Milan, Dipartimento Fis, Milan, Italy

[33] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[34] Univ Ferrara, Dipartmento Fis, I-44122 Ferrara, Italy

[35] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy

[36] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy

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

[38] ULL, Dpto Astrofis, Tenerife 38206, Spain

[39] ESO Vitacura, European So Observ, Santiago, Chile

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

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

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

[43] INAF Osservatorio Astron Padova, Padua, Italy

[44] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy

[45] INAF Osservatorio Astron Trieste, Trieste, Italy

[46] INAF Ist Radioastron, I-40129 Bologna, Italy

[47] INAF IASF Bologna, Bologna, Italy

[48] INAF IASF Milano, Milan, Italy

[49] Univ Roma La Sapienza, Sez Roma 1, INFN, I-00185 Rome, Italy

[50] Univ Paris 11, INRIA, Lab Rech Informat, F-91405 Orsay, France

来源：

ASTRONOMY & ASTROPHYSICS | 2012年 / 543卷

关键词：

cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters; REPRESENTATIVE SAMPLE; GALAXY CLUSTERS; SCALING RELATIONS; REXCESS; SKY;

D O I：

10.1051/0004-6361/201118731

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N < 5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 < z < 0.94, demonstrating Planck's capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using Y-X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y-SZ-Y-X relation, with a turnover at Y-SZ similar to 4 x 10 (4) arcmin(2). We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the Y-X vs. Y-SZ and X-ray flux F-X vs. Y-SZ relations.

引用

页数：14

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