Self-similar scaling and evolution in the galaxy cluster X-ray luminosity-temperature relation

Maughan, Ben; Giles, Paul; Randall, Scott W.; Jones, C.; Forman, W.

doi:10.1111/j.1365-2966.2012.20419.x

Cited by 168 publications

(254 citation statements)

References 77 publications

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“…Markevitch 1998;Pratt et al 2009;Mittal et al 2011;Eckmiller et al 2011;Reichert et al 2011;Takey et al 2011;Maughan et al 2012;Hilton et al 2012). These studies showed that the observed L X − T relation is much steeper than that predicted by self-similar evolution.…”

Section: Introductionmentioning

confidence: 73%

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: Introductionmentioning

confidence: 73%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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“…Bolometric luminosities estimated in a region from which the core is excised are supposed to be slightly less sensitive to the baryonic physics. Considering the LX,ce from Maughan et al (2012), we found βY -Z = 1.47 ± 0.18, γz = −1.39 ± 0.57, and σ Y |Z = 0.09 ± 0.05. As expected, the LX,ce-M∆ relation is more tight, with a smaller intrinsic dispersion, and it can be determined with a better statistical accuracy.…”

Section: Self-similaritymentioning

confidence: 88%

“…The sample was later reanalysed using updated softwares and calibration files in Maughan et al (2012). Bolometric luminosities were measured either in the [0-1] r500 aperture, which we took as reference case to ease the comparison with theoretical predictions, or in the core-excised [0.15-1] r500 aperture, LX,ce.…”

Section: X-ray Clustersmentioning

confidence: 99%

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Sereno¹,

Ettori²

2015

Monthly Notices of the Royal Astronomical Society

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The scaling of observable properties of galaxy clusters with mass evolves with time. Assessing the role of the evolution is crucial to study the formation and evolution of massive halos and to avoid biases in the calibration. We present a general method to infer the mass and the redshift dependence, and the time-evolving intrinsic scatter of the mass-observable relations. The procedure self-calibrates the redshift dependent completeness function of the sample. The intrinsic scatter in the mass estimates used to calibrate the relation is considered too. We apply the method to the scaling of mass M ∆ versus line of sight galaxy velocity dispersion σ v , optical richness, X-ray luminosity, L X , and Sunyaev-Zel'dovich signal. Masses were calibrated with weak lensing measurements. The measured relations are in good agreement with time and mass dependencies predicted in the self-similar scenario of structure formation. The lone exception is the L X -M ∆ relation whose time evolution is negative in agreement with formation scenarios with additional radiative cooling and uniform preheating at high redshift. The intrinsic scatter in the σ v -M ∆ relation is notably small, of order of 14 per cent. Robust predictions on the observed properties of the galaxy clusters in the CLASH sample are provided as cases of study. Catalogs and scripts are publicly available at

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“…Mitchell et al 1977Mitchell et al , 1979Mushotzky 1984;Edge & Stewart 1991;David et al 1993;Markevitch 1998;Allen et al 2001;Ikebe et al 2002;Ettori et al 2004a;Pratt et al 2009;Mittal et al 2011;Maughan et al 2012). This is not surprising, since both quantities can be measured easily and almost independently from X-ray data.…”

Section: The L X − T and S − T Scaling Relationmentioning

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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Self-similar scaling and evolution in the galaxy cluster X-ray luminosity-temperature relation

Cited by 168 publications

References 77 publications

The 2XMMi/SDSS Galaxy Cluster Survey

The 2XMMi/SDSS Galaxy Cluster Survey

CoMaLit – IV. Evolution and self-similarity of scaling relations with the galaxy cluster mass

Scaling Relations for Galaxy Clusters: Properties and Evolution

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