LoCuSS: comparison of observed X-ray and lensing galaxy  cluster
scaling relations with simulations

Zhang, Y.-Y.; Finoguenov, A.; Böhringer, H.; Kneib, Jean-Paul; Smith, Graham P.; Kneißl, R.; Okabe, Nobuhiko; Dahle, H.

doi:10.1051/0004-6361:20079103

Cited by 180 publications

(272 citation statements)

References 103 publications

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“…Mahdavi et al (2012) found that the scatter for clusters with low central entropies is particularly low, suggesting that the gas fractions vary very little for such clusters. Zhang et al (2008) found a lower gas mass in low mass systems than expected from a purely gravitational scenario, implying a steepening with respect to the prediction of the self-similar scenario.…”

Section: Thementioning

confidence: 57%

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: Thementioning

confidence: 57%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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“…On the other hand, our masses are mostly calculated with double β-models, taking into account the temperature gradients. This is the same procedure as applied for the LoCuSS clusters (Zhang et al 2008), which we also include in the plots for comparison.…”

Section: Note On Model Choicementioning

confidence: 99%

“…The total gravitational mass of a cluster, consisting of both baryonic matter and dark matter, is tightly correlated with observable quantities such as temperature and luminosity, and relations between these have been studied extensively with both observational and computational techniques (e.g., Allen et al 2001;Finoguenov et al 2001;Reiprich & Böhringer 2002;Borgani et al 2004;Stanek et al 2006;Nagai et al 2007a,b;Rykoff et al 2008;Hartley et al 2008;Zhang et al 2008;Lopes et al 2009;Vikhlinin et al 2009;Ettori et al 2010;Leauthaud et al 2010;Mantz et al 2010;Plagge et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Testing the low-mass end of X-ray scaling relations with a sample ofChandragalaxy groups

Eckmiller

Hudson

Reiprich

2011

A&A

129

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Context. Well-determined scaling relations between X-ray observables and cluster mass are essential for using large cluster samples to constrain fundamental cosmological parameters. Scaling relations between cluster masses and observables, such as the luminositytemperature, mass-temperature, luminosity-mass relations, have been investigated extensively, however the question of whether these relations hold true also for poor clusters and groups remains unsettled. Some evidence supports a "break" at the low end of the group/cluster mass range, possibly caused by the stronger influence of non-gravitational physics on low-mass systems. Aims. The main goal of this work is to test local scaling relations for the low-mass range in order to check whether or not there is a systematic difference between clusters and groups, and to thereby extend this method of reliable and convenient cluster mass determination for future large samples down to the group regime. Methods. We compiled a statistically complete sample of 112 X-ray galaxy groups, 26 of which have usable Chandra data. Temperature, metallicity, and surface brightness profiles were created for these 26 groups, and used to determine the main physical quantities and scaling relations. We then compared the group properties to those of the HIFLUGCS clusters, as well as several other group and cluster samples. Results. We present radial profiles for the individual objects and scaling relations of the whole sample (. Temperature and metallicity profiles behave universally, except for the core regions.and L x − Y x relations of the group sample are generally in good agreement with clusters. The L x − T relation steepens for T < 3 keV, which could point to a larger impact of heating mechanisms on cooler systems. We found a significant drop in the gas mass fraction below < ∼ 1 keV, as well as a correlation with radius, which indicates the ICM is less dominant in groups compared to clusters and the galaxies have a stronger influence on the global properties of the system. In all relations the intrinsic scatter for groups is larger than for clusters, which appears not to be correlated with merger activity but could be due to scatter caused by baryonic physics in the group cores. We also demonstrate the importance of selection effects. Conclusions. We have found some evidence for a similarity break between groups and clusters. However this does not have a strong effect on the scaling relations.

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“…In the low redshift Universe, weak lensing (WL) based mass measurements applied to sizable cluster samples have established massobservable relations with significantly improved accuracy (e.g. Reyes et al 2008;Zhang et al 2008;Marrone et al 2009). First weak lensing constraints on the evolution of scaling relations for X-ray groups are now available (e.g.…”

Section: Introductionmentioning

confidence: 99%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

Self Cite

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Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

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LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations

Cited by 180 publications

References 103 publications

Scaling Relations for Galaxy Clusters: Properties and Evolution

Scaling Relations for Galaxy Clusters: Properties and Evolution

Testing the low-mass end of X-ray scaling relations with a sample ofChandragalaxy groups

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

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