The x-ray luminous galaxy cluster population at 0.9 &lt;<i>z</i>≲ 1.6 as revealed by the XMM-<i>Newton</i>Distant Cluster Project

Fassbender, R.; Böhringer, H.; Nastasi, A.; Šuhada, R.; Mühlegger, M.; Hoon, A. de; Kohnert, J.; Lamer, G.; Mohr, J. J.; Pierini, D.; Pratt, G. W.; Quintana, H.; Rosati, P.; Santos, J. S.; Schwope, A. D.

doi:10.1088/1367-2630/13/12/125014

Cited by 94 publications

(150 citation statements)

References 106 publications

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“…Among these are the XMM Deep Cluster Project (XDCP2; Fassbender et al 2011) that has so far spectroscopically confirmed 22 clusters at z > 0.8. The study of these high redshift objects is extremely important.…”

Section: Evolutionmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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Well-calibrated scaling relations between the observable properties and the total masses of clusters of galaxies are important for understanding the physical processes that give rise to these relations. They are also a critical ingredient for studies that aim to constrain cosmological parameters using galaxy clusters. For this reason much effort has been spent during the last decade to better understand and interpret relations of the properties of the intra-cluster medium. Improved X-ray data have expanded the mass range down to galaxy groups, whereas SZ surveys have openened a new observational window on the intracluster medium. In addition, continued progress in the performance of cosmological simulations has allowed a better understanding of the physical processes and selection effects affecting the observed scaling relations. Here we review the recent literature on various scaling relations, focussing on the latest observational measurements and the progress in our understanding of the deviations from self similarity.

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Section: Evolutionmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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“…Several other projects are being conducted to detect galaxy clusters from the observations of the XMM-Newton, Chandra, and the X-ray Telescope A&A 558, A75 (2013) on board of the Swift satellite (e.g. Barkhouse et al 2006; Kolokotronis et al 2006;Finoguenov et al 2007Finoguenov et al , 2010Adami et al 2011;Fassbender et al 2011;Takey et al 2011;Mehrtens et al 2012;Clerc et al 2012;Tundo et al 2012;de Hoon et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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Aims. We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). We present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (L X − T ) relation. Methods. The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data we derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. Results. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03−0.70 (median z = 0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. For each cluster, the catalogue also provides the X-ray bolometric luminosity and the cluster mass at R 500 based on scaling relations and the position of the likely brightest cluster galaxy (BCG). The updated L X − T relation of the current sample with X-ray spectroscopic parameters is presented. We found the slope of the L X − T relation to be consistent with published ones. We see no evidence for evolution in the slope and intrinsic scatter of the L X − T relation with redshift when excluding the low-luminosity groups.

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“…Follow-up z, H photometry was originally obtained with the near-IR, wide-field camera OMEGA2000 mounted at the prime focus of the 3.5 m telescope at Calar Alto, Spain. A redshift z ∼ 1.45 ± 0.15 was inferred from comparison between the average z − H colour of the reddest galaxies within 45 from the X-ray position of XMMU J0338.7+0030 and the synthetic z − H colours expected for a large suite of simple stellar population (SSP) models (see Fassbender et al 2011c). The synthetic photometry was computed using the spectro-photometric evolutionary synthesis model PÉGASE v2 (Fioc & Rocca-Volmerange 1997) in analogy with Pierini et al (2005) and Wilman et al (2008).…”

Section: Introductionmentioning

confidence: 99%

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Pierini

Šuhada

Fassbender

et al. 2012

A&A

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Context. The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z ≥ 0.8 based on deep archival XMM-Newton observations. X-ray sources identified as extended are screened against existing optical all-sky surveys for galaxies, in case of candidate high-z clusters followed up with imaging at 4 m-class telescopes and, ultimately, multi-object spectroscopy at 8 m-class telescopes. Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2 m-class telescope. Its unique capability of simultaneous imaging in the g , r , i , z , J, H, Ks bands enables the use of the photometric redshift technique. Aims. Observing strategy, data reduction and analysis, depth and accuracy of the simultaneous multi-wavelength photometry are discussed with the goal of establishing GROND as a useful instrument to confirm X-ray selected (high-z) clusters. Methods. The test case is XMMU J0338.7+0030, suggested to be at z ∼ 1.45 ± 0.15 (1σ) from the analysis of the z − H vs. H colour−magnitude diagram obtained from the follow-up imaging. Later VLT-FORS2 spectroscopy enabled us to identify four members, which set this cluster at z = 1.097 ± 0.002 (1σ). To reach a better knowledge of its galaxy population, we observed XMMU J0338.7+0030 with GROND for about 6 h. The publicly available photo-z code le Phare was used. Results. The Ks-band number counts of the non-stellar sources out of the 832 detected down to z ∼ 26 AB mag (1σ) in the 3.9×4.3 arcmin 2 region of XMMU J0338.7+0030 imaged at all GROND bands clearly exceed those computed in deep fields/survey areas at ∼20.5-22.5 AB mag. The photo-z's of the three imaged spectroscopic members yield z = 1.12 ± 0.09 (1σ). The spatial distribution and the properties of the GROND sources with a photo-z in the range 1.01-1.23 confirm the correspondence of the X-ray source with a galaxy over-density at a significance of at least 4.3σ. Candidate members that are spectro-photometrically classified as elliptical galaxies define a red locus in the i −z vs. z colour−magnitude diagram that is consistent with the red sequence of the cluster RDCS J0910+5422 at z = 1.106. XMMU J0338.7+0030 hosts also a population of bluer late-type spirals and irregulars. The starbursts among the photometric members populate both loci, consistently with previous results. Conclusions. The analysis of the available data set indicates that XMMU J0338.7+0030 is a low-mass cluster (M 200 ∼ 10 14 M ) at z = 1.1. With the photometric accuracy yielded by the present unoptimized multi-band observations with GROND, we not only confirm the spectroscopic redshift of this cluster but also show that it hosts a galaxy population that can still undergo significant bursts of star-formation activity.

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The x-ray luminous galaxy cluster population at 0.9 <z≲ 1.6 as revealed by the XMM-NewtonDistant Cluster Project

Cited by 94 publications

References 106 publications

Scaling Relations for Galaxy Clusters: Properties and Evolution

Scaling Relations for Galaxy Clusters: Properties and Evolution

The 2XMMi/SDSS Galaxy Cluster Survey

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

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