The evolution of galaxy cluster X-ray scaling relations

Short, Chris; Thomas, P.; Young, Owain; Pearce, Frazer R.; Jenkins, Adrian; Muanwong, Orrarujee

doi:10.1111/j.1365-2966.2010.17267.x

Cited by 59 publications

(136 citation statements)

References 126 publications

(224 reference statements)

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“…The only exception is the LX-M∆ relation, which seems to show a negative evolution. A similar level of evolution can be obtained in hydrodynamical simulations of the intracluster medium by including additional radiative cooling and uniform preheating at high redshift as a simple model of non-gravitational heating from astrophysical sources (Ettori et al 2004a;Short et al 2010;Reichert et al 2011).…”

Section: Discussionmentioning

confidence: 56%

“…They found that the energy output from SNe and AGNs as implemented through semi-analytic models of galaxy formation causes a positive evolution. On the other hand, simulations based on a pre-heating model where an entropy floor of 200 keV cm 2 is introduced at z = 4 confirmed the presence of a negative evolution (Short et al 2010).…”

Section: Lx-m∆mentioning

confidence: 93%

“…A exhaustive study of the joint effect of feedback from supernovae (SNe) and active galactic nuclei (AGNs) on the evolution of the X-ray scaling laws presented in Short et al (2010) predicts an opposite behaviour of the evolution of the LX-M∆ relation. They found that the energy output from SNe and AGNs as implemented through semi-analytic models of galaxy formation causes a positive evolution.…”

Section: Lx-m∆mentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 56%

Section: Lx-m∆mentioning

confidence: 93%

Section: Lx-m∆mentioning

confidence: 99%

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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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“…Hence observational constraints have the potential to constrain the non-gravitational physics. However, Short et al (2010) point out that a statistically meaningful comparison with observations is impossible at the moment, because the largest samples of high-redshift clusters currently available are still affected by strong selection biases.…”

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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“…Planelles et al (2013) further showed that AGN feedback in their simulations is capable of reproducing observed cluster baryon, gas and star fractions. Short et al (2010) included AGN feedback into cosmological simulations using a semi-analytic galaxy formation model to infer the heating rates from the full galaxy population and showed that such a model could reproduce a range of X-ray cluster properties, although they neglected the effects of radiative cooling (however, see also Short, Thomas & Young 2013). McCarthy et al (2010McCarthy et al ( , 2011 simulated the effects of AGN feedback in galaxy groups and showed that they could reproduce a number of their observed properties.…”

mentioning

confidence: 99%

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

Pike

Kay

Newton

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present results from a new set of 30 cosmological simulations of galaxy clusters, including the effects of radiative cooling, star formation, supernova feedback, black hole growth and AGN feedback. We first demonstrate that our AGN model is capable of reproducing the observed cluster pressure profile at redshift, z 0, once the AGN heating temperature of the targeted particles is made to scale with the final virial temperature of the halo. This allows the ejected gas to reach larger radii in highermass clusters than would be possible had a fixed heating temperature been used. Such a model also successfully reduces the star formation rate in brightest cluster galaxies and broadly reproduces a number of other observational properties at low redshift, including baryon, gas and star fractions; entropy profiles outside the core; and the Xray luminosity-mass relation. Our results are consistent with the notion that the excess entropy is generated via selective removal of the densest material through radiative cooling; supernova and AGN feedback largely serve as regulation mechanisms, moving heated gas out of galaxies and away from cluster cores. However, our simulations fail to address a number of serious issues; for example, they are incapable of reproducing the shape and diversity of the observed entropy profiles within the core region. We also show that the stellar and black hole masses are sensitive to numerical resolution, particularly the gravitational softening length; a smaller value leads to more efficient black hole growth at early times and a smaller central galaxy.

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The evolution of galaxy cluster X-ray scaling relations

Cited by 59 publications

References 126 publications

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

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

Scaling Relations for Galaxy Clusters: Properties and Evolution

Cosmological simulations of galaxy clusters with feedback from active galactic nuclei: profiles and scaling relations

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