The XXL Survey XX. The 365 cluster catalogue

被引：99

作者：

Adami, C. ^{[1
]}

Giles, P. ^{[7
]}

Koulouridis, E. ^{[3
]}

Pacaud, F. ^{[4
]}

Caretta, C. A. ^{[1
,6
]}

Pierre, M. ^{[3
]}

Eckert, D. ^{[9
]}

Ramos-Ceja, M. E. ^{[4
]}

Gastaldello, F. ^{[8
]}

Fotopoulou, S. ^{[47
]}

Guglielmo, V. ^{[1
,2
,32
]}

Lidman, C. ^{[11
]}

Sadibekova, T. ^{[3
]}

Iovino, A. ^{[29
,30
]}

Maughan, B. ^{[7
]}

Chiappetti, L. ^{[8
]}

Alis, S. ^{[42
]}

Altieri, B. ^{[33
]}

Baldry, I. ^{[20
]}

Bottini, D. ^{[8
]}

Birkinshaw, M. ^{[7
]}

Bremer, M. ^{[7
]}

Brown, M. ^{[21
]}

Cucciati, O. ^{[27
,35
]}

Driver, S. ^{[18
,19
]}

Elmer, E. ^{[15
]}

Ettori, S. ^{[27
,43
]}

Evrard, A. E. ^{[25
,26
]}

Faccioli, L. ^{[3
]}

Granett, B. ^{[29
,30
,34
]}

Grootes, M. ^{[24
]}

Guzzo, L. ^{[29
,30
,34
]}

Hopkins, A. ^{[11
]}

Horellou, C. ^{[28
]}

Lefevre, J. P. ^{[3
]}

Liske, J. ^{[22
]}

Malek, K. ^{[37
]}

Marulli, F. ^{[27
,35
,36
]}

Maurogordato, S. ^{[12
]}

Owers, M. ^{[11
,17
]}

Paltani, S. ^{[9
]}

Poggianti, B. ^{[2
]}

Polletta, M. ^{[8
,38
,41
]}

Plionis, M. ^{[10
,46
]}

Pollo, A. ^{[37
,39
]}

Pompei, E. ^{[5
]}

Ponman, T. ^{[16
]}

Rapetti, D. ^{[44
,45
]}

Ricci, M. ^{[12
]}

Robotham, A. ^{[18
,19
]}

机构：

[1] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

[2] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[3] CEA Saclay, CEA, Lab AIM, DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France

[4] Univ Bonn, Argelander Inst Astron, Auf Dem Hugel 71, D-53121 Bonn, Germany

[5] European Southern Observ, Alonso Cordova 3107, Santiago 19001 19, Chile

[6] Univ Guanajuato, Dept Astron, DCNE, CGT, Callejon Jalisco S-N, Guanajuato 36240, Gto, Mexico

[7] HH Wills Phys Lab, Sch Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England

[8] IASF Milano, INAF, Via Bassini 15, I-20133 Milan, Italy

[9] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland

[10] Aristotle Univ Thessaloniki, Phys Dept, Thessaloniki 54124, Greece

[11] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia

[12] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab Lagrange,UMR 7293, F-06304 Nice, France

[13] Univ Oxford, Dept Phys, Oxford OX1 3PU, England

[14] Univ Oxford Merton Coll, Oxford OX1 4JD, England

[15] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England

[16] Univ Birmingham, Sch Phys & Astron, Astrophys & Space Res Grp, Birmingham B15 2TT, W Midlands, England

[17] Macquarie Univ, N Ryde, NSW 2109, Australia

[18] ICRAR, 1 Turner Ave,Technol Pk, Bentley, WA 6102, Australia

[19] Univ St Andrews, Coll Gate, St Andrews KY16 9AJ, Fife, Scotland

[20] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[21] Monash Univ, Clayton, Vic 3800, Australia

[22] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[23] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany

[24] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

[25] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[26] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[27] Osservatorio Astron Bologna, INAF, Via Pietro Gobetti 93-3, I-40129 Bologna, Italy

[28] Chalmers Univ Technol, Onsala Space Observ, Dept Space Environm & Earth, S-43992 Onsala, Sweden

[29] Osservatorio Astron Brere, INAF, Via Brera 28, I-20121 Milan, Italy

[30] Osservatorio Astron Brere, INAF, Via E Bianchi 46, I-20121 Merate, Italy

[31] Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 1A1, Canada

[32] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

[33] European Space Astron Ctr, ESA, ESAC, Operat Dept, Madrid, Spain

[34] Univ Milan, Via G Celoria 16, I-20133 Milan, Italy

[35] Univ Bologna, Dipartimento Fis Astron DIFA, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[36] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[37] Natl Ctr Nucl Res, Ul Hoza 69, PL-00681 Warsaw, Poland

[38] Univ Toulouse, IRAP, CNRS, UPS, Toulouse, France

[39] Jagiellonian Univ, Astron Observ, Orla 171, PL-30001 Krakow, Poland

[40] IASF Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy

[41] Aix Marseille Univ Pharo, 58 Bd Charles Livon Jardin Pharo, F-13007 Marseille, France

[42] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey

[43] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[44] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[45] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[46] Natl Observ Athens, Athens 11851, Greece

[47] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 620卷

基金：

瑞士国家科学基金会;

关键词：

galaxies: clusters: general; large-scale structure of Universe; galaxies: groups: general; galaxies: clusters: intracluster medium; NEWTON DEEP FIELD; FOSSIL GROUP; SCALING RELATIONS; GALAXY; SUPERCLUSTERS; EVOLUTION;

D O I：

10.1051/0004-6361/201731606

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. In the currently debated context of using clusters of galaxies as cosmological probes, the need for well-defined cluster samples is critical. Aims. The XXL Survey has been specifically designed to provide a well characterised sample of some 500 X-ray detected clusters suitable for cosmological studies. The main goal of present article is to make public and describe the properties of the cluster catalogue in its present state, as well as of associated catalogues of more specific objects such as super-clusters and fossil groups. Methods. Following from the publication of the hundred brightest XXL clusters, we now release a sample containing 365 clusters in total, down to a flux of a few 10(-15) erg s(-1) cm(-2) in the [0.5-2] keV band and in a 1' aperture. This release contains the complete subset of clusters for which the selection function is well determined plus all X-ray clusters which are, to date, spectroscopically confirmed. In this paper, we give the details of the follow-up observations and explain the procedure adopted to validate the cluster spectroscopic redshifts. Considering the whole XXL cluster sample, we have provided two types of selection, both complete in a particular sense: one based on flux-morphology criteria, and an alternative based on the [0.5-2] keV flux within 1 arc min of the cluster centre. We have also provided X-ray temperature measurements for 80% of the clusters having a flux larger than 9 x 10(-15) erg s(-1) cm(-2). Results. Our cluster sample extends from z similar to 0 to z similar to 1.2, with one cluster at z similar to 2. Clusters were identified through a mean number of six spectroscopically confirmed cluster members. The largest number of confirmed spectroscopic members in a cluster is 41. Our updated luminosity function and luminosity-temperature relation are compatible with our previous determinations based on the 100 brightest clusters, but show smaller uncertainties. We also present an enlarged list of super-clusters and a sample of 18 possible fossil groups. Conclusions. This intermediate publication is the last before the final release of the complete XXL cluster catalogue when the ongoing C2 cluster spectroscopic follow-up is complete. It provides a unique inventory of medium-mass clusters over a 50 deg(2) area out to z similar to 1.

引用

页数：28

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