X-ray groups and clusters of galaxies in the Subaru-XMM Deep Field

Finoguenov, A.; Watson, M. G.; Tanaka, Masayuki; Simpson, Chris; Cirasuolo, M.; Dunlop, J. S.; Peacock, J. A.; Farrah, D.; Akiyama, Masayuki; Ueda, Yoshihiro; Smolčić, Vernesa; Stewart, G. C.; Rawlings, Steve; Breukelen, C. van; Almaini, O.; Clewley, L.; Bonfield, D. G.; Jarvis, Matt J.; Barr, Jordi; Foucaud, S.; McLure, R. J.; Sekiguchi, K.; Egami, Eiichi

doi:10.1111/j.1365-2966.2010.16256.x

Cited by 123 publications

(166 citation statements)

References 65 publications

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“…Of these three assumptions, the present day mass of Cl 0218.3−0510 most critically depends on whether we know the mass of the main halo at z = 1.62. Independent analyses of X-ray data from both Chandra and XMM-Newton (Tanaka, Finoguenov & Ueda 2010;Finoguenov et al 2010;Pierre et al 2012) and dynamical velocity dispersion estimates (Tran et al 2015) are all consistent with our assumed initial mass, however we caution that estimates for group and cluster masses at this redshift are highly uncertain.…”

Section: The Z = 0 Mass Of CL 02183−0510mentioning

confidence: 85%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a comprehensive picture of the Cl 0218.3−0510 protocluster at z = 1.623 across 10 co-moving Mpc. Using filters that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies we obtain precise photometric redshifts resulting in a protocluster galaxy sample that is 89 ± 5% complete and has a contamination of only 12 ± 5%. Both star forming and quiescent protocluster galaxies are located allowing us to map the structure of the forming cluster for the first time. The protocluster contains 6 galaxy groups, the largest of which is the nascent cluster. Only a small minority of the protocluster galaxies are in the nascent cluster (11%) or in the other galaxy groups (22%), as most protocluster galaxies reside between the groups. Unobscured star forming galaxies predominantly reside between the protocluster's groups, whereas red galaxies make up a large fraction of the groups' galactic content, so observing the protocluster through only one of these types of galaxies results in a biased view of the protocluster's structure. The structure of the protocluster reveals how much mass is available for the future growth of the cluster and we use the Millennium Simulation, scaled to a Planck cosmology, to predict that Cl 0218.3−0510 will evolve into a 2.7 +3.9 −1.7 × 10 14 M ⊙ cluster by the present day.

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Section: The Z = 0 Mass Of CL 02183−0510mentioning

confidence: 85%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We include an additional step in background refinement performed by Finoguenov et al (2010), in which we repeat the background estimate steps for each detector and pointing. This refines the definition of the area used for the background evaluation, which is obtained through the analysis of the final mosaics.…”

Section: Extended X-ray Source Detectionsmentioning

confidence: 99%

“…We use the prescription of Finoguenov et al (2010) for extended source detection, which consists of removing the PSF model for each detected point source from the data before applying the extended source search algorithm. We include an additional step in background refinement performed by Finoguenov et al (2010), in which we repeat the background estimate steps for each detector and pointing.…”

Section: Extended X-ray Source Detectionsmentioning

confidence: 99%

The WIRCAM Deep Infrared Cluster Survey

Bielby

Finoguenov

Tanaka

et al. 2010

A&A

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Aims. We use a combination of CFHTLS deep optical data, WIRcam Deep Survey (WIRDS) near-infrared data and XMM-Newton survey data to identify z > ∼ 1.1 clusters in the CFHTLS D1 and D4 fields. Counterparts to such clusters can not be identified without deep near-infrared data and as such the total of ≈1 deg 2 of J, H and K s band imaging provided by WIRDS is an indispensable tool in such work. Methods. Using public XMM X-ray data, we identify extended X-ray sources in the two fields. The resulting catalogue of extended X-ray sources was then analyzed for optical/near-infrared counterparts, using a red-sequence algorithm applied to the deep optical and near-infrared data. Redshifts of candidate groups and clusters were estimated using the median photometric redshifts of detected counterparts and where available these were combined with spectroscopic data (from VVDS deep and ultra-deep and using AAT AAOmega data). Additionally, we surveyed X-ray point sources for potential group systems at the limit of our detection range in the X-ray data. A catalogue of z > 1.1 cluster candidates in the two fields has been compiled and cluster masses, radii and temperatures have been estimated using the scaling relations. Results. The catalogue of group and cluster candidates consists of 15 z > ∼ 1.1 objects. We find several massive clusters (M > ∼ 10 14 M ) and a number of lower mass clusters/groups. Three of the detections are previously published extended X-ray sources. Of note is JKSC 041 (previously detected via Chandra X-ray data and reported as a z = 1.9 cluster based on UKIDSS infrared imaging) for which we identify a number of structures at redshifts of z = 0.8, z = 0.96, z = 1.13 and z = 1.49 (but see no evidence of a structure at z = 1.9). We also make an independent detection of the massive cluster, XMMXCS J2215.9-1738, for which we estimate a redshift of z = 1.37 (compared to the spectroscopically confirmed redshift of z = 1.45). We use the z > ∼ 1.1 catalogue to compare the cluster number counts in these fields with models based on WMAP 7-year cosmology and find that the models slightly over-predict the observations, whilst at z > 1.5 we do not detect any clusters. We note that cluster number counts at z > ∼ 1.1 are highly sensitive to the cosmological model, however a significant reduction in present statistical (due to available survey area) and systematic (due to cluster scaling relations) uncertainties is required in order to confidently constrain cosmological parameters using cluster number counts at high redshift.

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“…X-ray) permit a complete census of clusters covering a wide range of masses and redshifts, and survey data themselves can provide estimates of the mass of these objects. This is why large surveys in the X-ray wavelengths aimed at constraining cosmology with galaxy clusters have been developed since the early years of X-ray astronomy (Jones & Forman 1984;Henry & Arnaud 1991;Bahcall & Cen 1993), with a notable stepchange brought about by the ROSAT all-sky survey (RASS; Ebeling et al 2000;Ikebe et al 2002;Schuecker et al 2003) and ROSAT serendipitous surveys (Rosati et al 1998;Romer et al 2000;Burke et al 2003;Burenin et al 2007) and the support of Chandra and XMM-Newton (Pacaud et al 2006;Vikhlinin et al 2009;Finoguenov et al 2010;Mantz et al 2010;Clerc et al 2014;Pierre et al 2016). The next major advance in the field will be offered by eROSITA (extended ROentgen Survey with an Imaging Telescope Array; Predehl et al 2014) which will survey the entire sky in the 0.3-10 keV energy range at depths 10-30 times deeper than ROSAT.…”

Section: Introductionmentioning

confidence: 99%

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

Clerc

Merloni

Zhang

et al. 2016

Mon. Not. R. Astron. Soc.

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105

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SPIDERS (The SPectroscopic IDentification of eROSITA Sources) is a programme dedicated to the homogeneous and complete spectroscopic follow-up of X-ray active galactic nuclei and galaxy clusters over a large area (∼7500 deg 2 ) of the extragalactic sky. SPIDERS is part of the Sloan Digital Sky Survey (SDSS)-IV project, together with the Extended Baryon Oscillation Spectroscopic Survey and the Time-Domain Spectroscopic Survey. This paper describes the largest project within SPIDERS before the launch of eROSITA: an optical spectroscopic survey of X-ray-selected, massive (∼10 14 -10 15 M ) galaxy clusters discovered in ROSAT and XMMNewton imaging. The immediate aim is to determine precise ( z ∼ 0.001) redshifts for 4000-5000 of these systems out to z ∼ 0.6. The scientific goal of the program is precision cosmology, using clusters as probes of large-scale structure in the expanding Universe. We present the cluster samples, target selection algorithms and observation strategies. We demonstrate the efficiency of selecting targets using a combination of SDSS imaging data, a robust red-sequence finder and a dedicated prioritization scheme. We describe a set of algorithms and workflow developed to collate spectra and assign cluster membership, and to deliver catalogues of spectroscopically confirmed clusters. We discuss the relevance of line-of-sight velocity dispersion estimators for the richer systems. We illustrate our techniques by constructing a catalogue of 230 spectroscopically validated clusters (0.031 < z < 0.658), found in pilot observations. We discuss two potential science applications of the SPIDERS sample: the study of the X-ray luminosity-velocity dispersion (L X -σ ) relation and the building of stacked phase-space diagrams.

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X-ray groups and clusters of galaxies in the Subaru-XMM Deep Field

Cited by 123 publications

References 65 publications

The structure and evolution of a forming galaxy cluster atz= 1.62

The structure and evolution of a forming galaxy cluster atz= 1.62

The WIRCAM Deep Infrared Cluster Survey

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

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