A Serendipitous Galaxy Cluster Survey with<i>XMM</i>: Expected Catalog Properties and Scientific Applications

Romer, A. K.; Viana, P. T. P.; Liddle, Andrew R.; Mann, Robert

doi:10.1086/318382

Cited by 166 publications

(206 citation statements)

References 88 publications

(145 reference statements)

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“…The largest published catalogue of X-ray clusters so far, based on the entire XMM-Newton archive, was compiled by the XMM Cluster Survey team (XCS, Romer et al 2001;Lloyd-Davies et al 2011;Mehrtens et al 2012). The catalogue consists of 503 optically confirmed clusters.…”

Section: Comparison With the Xcs Samplementioning

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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Section: Comparison With the Xcs Samplementioning

confidence: 99%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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“…This will allow one to put strong constraints on cosmological models (e.g. Romer et al 2001) as well as sampling the internal structure evolution of groups (and more massive clusters) up to these redshifts. The time required to treat these future samples with our method is very short.…”

Section: Sample Completeness and 2-point Correlation Functionmentioning

confidence: 99%

“…Oukbir & Blanchard 1992Romer et al 2001). The more distant the structure, the stronger the constraint.…”

Section: Introductionmentioning

confidence: 99%

Group analysis in the SSRS2 catalog

Adami¹,

Mazure²

2002

A&A

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Abstract. We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog. The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms. They have similar mass distribution, similar abundance versus redshift, a similar 2-point correlation function (modeled by a power law: (r/r0) γ with r0 = 7 h −1 Mpc and γ = −1.79) and the same redshift completeness limit, close to 5000 km s −1 . If instead of SSRS2, we use catalogs of the new generation (deep redshift surveys obtained with 10 m class telescopes), it would lead to a completeness limit of z ∼ 0.7. We model the luminosity function for nearby galaxy groups by a Schechter function with parameters M * SSRS2 = (−19.99 ± 0.36) + 5 logh and α = −1.46 ± 0.17 to compute the mass to light ratio. The median value of the mass to light ratio is 360 hM /L (in the SSRS2 band, close to a B band magnitude) and we deduce a relation between mass to light ratio and velocity dispersion σ (M/L = (3.79 ± 0.64)σ − (294 ± 570)). The more massive the group, the higher the mass to light ratio, and therefore, the larger the amount of dark matter inside the group. Another explanation is a significant stripping of the gas of the galaxies in massive groups as opposed to low mass groups. This extends to groups of galaxies the mild tendency already detected for rich clusters of galaxies. Finally, we detect a barely significant fundamental plane for these groups (L ∝ R 2.26±1.39 Vir × σ 2.93±1.64 for groups with more than 8 galaxies) but it is much less narrow than for clusters of galaxies.

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“…see Viana et al, 2003, and references therein). Next generation cluster cosmology surveys, such as the XCS (Romer et al, 2001), will detect sufficiently large numbers of clusters that uncertainties in values of cosmological parameters will be mainly systematic, requiring for example an accurate calibration between cluster X-ray temperature and mass. Such measurements demand an improved understanding of cluster physics, therefore realistic numerical simulations of the cluster population are essential.…”

Section: Introductionmentioning

confidence: 99%

Clusters of galaxies: new results from the CLEF hydrodynamics simulation

Kay

Silva

Aghanim

et al. 2005

Advances in Space Research

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Preliminary results are presented from the CLEF hydrodynamics simulation, a large (N = 2 × 428 3 particles within a 200 h −1 Mpc comoving box) simulation of the ΛCDM cosmology that includes both radiative cooling and a simple model for galactic feedback. Specifically, we focus on the X-ray properties of the simulated clusters at z = 0 and demonstrate a reasonable level of agreement between simulated and observed cluster scaling relations.

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A Serendipitous Galaxy Cluster Survey withXMM: Expected Catalog Properties and Scientific Applications

Cited by 166 publications

References 88 publications

The 2XMMi/SDSS Galaxy Cluster Survey

The 2XMMi/SDSS Galaxy Cluster Survey

Group analysis in the SSRS2 catalog

Clusters of galaxies: new results from the CLEF hydrodynamics simulation

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