The XMM-NEWTON<i>Ω</i>project

Lumb, D.; Bartlett, J. G.; Romer, A. K.; Blanchard, Alain; Burke, Douglas; Collins, Chris; Nichol, R. C.; Giard, M.; Marty, Philippe; Nevalainen, J.; Sadat, R.; Vauclair, S.

doi:10.1051/0004-6361:20035687

Cited by 61 publications

(81 citation statements)

References 64 publications

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“…The conversion between band and bolometric luminosity is computed using the MEKAL plasma code and measured temperature. Compared with high-redshift measurements (e.g., Ota et al 2006), the slopes match within the uncertainty, while our normalization is smaller, which is in general agreement with the positive redshift evolution of luminosity that has been suggested by previous works (Vikhlinin et al 2002;Lumb et al 2004;Kotov & Vikhlinin 2005). T (keV) Figure 5.…”

Section: The L-t Relationsupporting

confidence: 91%

A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATINGSUZAKUDATA

Shang¹,

Scharf²

2008

ApJ

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We present the first results of a survey of 14 low-redshift galaxy clusters using Suzaku. Although luminous (L x > 1 × 10 43 erg s −1 (0.1-2.4 keV)), these clusters have no prior pointed X-ray data. Together with 47 other systems they form a flux-limited sample (f x > 1.0 × 10 −11 erg s −1 cm −2 (0.1-2.4 keV)) with z 0.1 in the northern celestial hemisphere. Using this total sample, we evaluate the local L-T relationship and the local cluster temperature function. Suzaku temperature measurements appear to be in accord with those of other missions. General agreement is found with other published estimates of the low-redshift cluster temperature function; however, the sample used here exhibits slightly lower space densities at gas temperatures below 4-5 keV. We find a corresponding deficit in the number of clusters with temperatures between approximately 4.5 and 5.5 keV. Although at low significance, a similar feature exists in previous low-redshift cluster data sets. We suggest that low-redshift cluster samples, while crucial for calibrating precision cosmology measurements, must be used with caution due to their limited size and susceptibility to the effects of cosmic variance.

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Section: The L-t Relationsupporting

confidence: 91%

A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATINGSUZAKUDATA

Shang¹,

Scharf²

2008

ApJ

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“…Earlier works find α = 1.5 ± 0.3 in Vikhlinin et al (2002) and Lumb et al (2004), and α = 1.8 ± 0.3 in Kotov & Vikhlinin (2005). Maughan et al (2006) find a value of α = 1.3 ± 0.2 when they combine their WARPS cluster sample with that of Vikhlinin et al (2002) and a value of α = 0.8 ± 0.4 for the WARPS sample alone.…”

Section: Vikhlinin Et Al (2009) Quote a Results For The Evolution Of Thementioning

confidence: 85%

Modelling self-similar appearance of galaxy clusters in X-rays

Böhringer

Dolag

Chon

2012

A&A

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Context. The largest uncertainty for cosmological studies using clusters of galaxies is introduced by our limited knowledge of the statistics of galaxy cluster structure and the related scaling relations between observables and cluster mass. A large effort has therefore been made to compile global galaxy cluster properties, in particular those obtained through X-ray observations, and to study their scaling relations. However, the scaling schemes used in the literature differ. Aims. The present paper aims to clarify this situation by providing a thorough review of the scaling laws within the standard model of large-scale structure growth and to discuss various steps in practical approximations. Methods. We derived the scaling laws for X-ray observables and cluster mass within the pure gravitational structure growth scenario. Using N-body simulations we tested the recent formation approximation used in earlier analytic approaches. It involves a redshiftdependent overdensity parameter. We find this approximation less precise than using a fiducial radius based on a fixed overdensity with respect to critical density. Results. Inspired by the comparison of the predicted scaling relations with observations, we propose a first-order modification of the scaling scheme to include the observed effects of hydrodynamics in structure formation. This modification involves a cluster-mass dependent gas-mass fraction. We also discuss the observational results of the reshift evolution of the most important scaling relations and find that a redshift dependence of the gas mass to total mass relation also has to be invoked within our modification scheme. Conclusions. We find that the current observational data are, within their uncertainties, consistent with the proposed modified scaling laws.

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“…Thanks to the increasing statistics of distant clusters observed in the last years with Chandra and XMM-Newton, a number of authors analysed this evolution out to the highest redshifts, z 1.3, where clusters have been detected so far. These analyses generally indicate that the amplitude of the L X -T relation has a positive evolution out to z 0.5-0.6 (e.g., Arnaud et al 2002;Lumb et al 2004;Kotov and Vikhlinin 2005), with hints for a possible inversion of this trend at higher redshift (e.g., Ettori et al 2004b;Maughan et al 2006;Branchesi et al 2007). In the attempt of interpreting these results, Voit (2005) showed that radiative cooling, combined with a modest amount of pre-heating with extra entropy, predicts an evolution of the L X -T relation slower than that of the self-similar model, also with an inversion of the trend at high redshift.…”

Section: The Luminosity-temperature Relationmentioning

confidence: 97%

Thermodynamical Properties of the ICM from Hydrodynamical Simulations

et al. 2008

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Modern hydrodynamical simulations offer nowadays a powerful means to trace the evolution of the X-ray properties of the intra-cluster medium (ICM) during the cosmological history of the hierarchical build up of galaxy clusters. In this paper we review the current status of these simulations and how their predictions fare in reproducing the most recent X-ray observations of clusters. After briefly discussing the shortcomings of the self-similar model, based on assuming that gravity only drives the evolution of the ICM, we discuss how the processes of gas cooling and non-gravitational heating are expected to bring model predictions into better agreement with observational data. We then present results from the hydrodynamical simulations, performed by different groups, and how they compare with observational data. As terms of comparison, we use X-ray scaling relations between mass, luminosity, temperature and pressure, as well as the profiles of temperature and entropy. The results of this comparison can be summarised as follows: (a) which include gas cooling, star formation and supernova feedback, are generally successful in reproducing the X-ray properties of the ICM outside the core regions; (b) simulations generally fail in reproducing the observed "cool core" structure, in that they have serious difficulties in regulating overcooling, thereby producing steep negative central temperature profiles. This discrepancy calls for the need of introducing other physical processes, such as energy feedback from active galactic nuclei, which should compensate the radiative losses of the gas with high density, low entropy and short cooling time, which is observed to reside in the innermost regions of galaxy clusters.

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The XMM-NEWTONΩproject

Cited by 61 publications

References 64 publications

A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATINGSUZAKUDATA

A LOW-REDSHIFT GALAXY CLUSTER X-RAY TEMPERATURE FUNCTION INCORPORATINGSUZAKUDATA

Modelling self-similar appearance of galaxy clusters in X-rays

Thermodynamical Properties of the ICM from Hydrodynamical Simulations

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