A catalog of intracluster gas temperatures

David, L. P.; Slyz, Adrianne; Jones, C.; Forman, W.; Vrtilek, S. D.; Arnaud, K. A.

doi:10.1086/172936

Cited by 413 publications

(555 citation statements)

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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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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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“…The estimates for about half the detected sources are based on the temperature-luminosity relationship of David et al (1993), which appears to hold out to redshifts ∼ 0.5 or even greater (Mushotzky & Scharf 1997, Donahue et al 1998, comparable with the highest redshifts where we have been able to separate nuclear and extended emission. There is a good deal of scatter in the temperatureluminosity relation and so these results are uncertain by perhaps .…”

Section: Temperature Assumptionsmentioning

confidence: 68%

The environments of FRII radio sources

Hardcastle

Worrall

2000

Monthly Notices of the Royal Astronomical Society

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Using ROSAT observations, we estimate gas pressures in the X-ray-emitting medium surrounding 63 FRII radio galaxies and quasars. We compare these pressures with the internal pressures of the radio-emitting plasma estimated by assuming minimum energy or equipartition. In the majority of cases (including 12/13 sources with modelled, spatially resolved X-ray emission) radio sources appear to be underpressured with respect to the external medium, suggesting that simple minimum-energy arguments underestimate the sources' internal energy density. We discuss possible departures from the minimum energy condition and the consequences of our result for models of the dynamics of radio galaxies, in particular self-similar models (Kaiser & Alexander 1997).

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“…We take the central electron density, temperature and the cool core radius from Churazov et al (2003) and the cluster X-ray luminosity from David et al (1993).…”

Section: A5 Perseus Clustermentioning

confidence: 99%

“…The gas parameters are taken from this reanalysis. The total luminosity used is taken from David et al (1993). Pollack et al (2005) study also the polarisation properties of the central radio source in this cluster.…”

Section: A6 Abell 2597mentioning

confidence: 99%

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Magnetic turbulence in cool cores of galaxy clusters

Vogt¹,

Enßlin²

2006

Astron Nachr

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Abstract. We argue that the recently reported Kolmogorov-like magnetic turbulence spectrum in the cool core of the Hydra A galaxy cluster can be understood by kinetic energy injection by active galaxies that drives a turbulent non-helical magnetic dynamo into its saturated state. Although dramatic differences exist between small-scale dynamo scenarios, their saturated state is expected to be similar, as we show for three scenarios: the ¤ux rope dynamo, the ¤uctuation dynamo, and the explosive dynamo. Based on those scenarios, we develop an analytical model of the hydrodynamic and magnetic turbulence in cool cores. The model implies magnetic £eld strengths that £t well with Faraday rotation measurements and minimum energy estimates for the sample of cool core clusters having such data available. Predictions for magnetic £elds in clusters for which the appropriate observational information is still missing, and for yet unobserved quantities like the hydrodynamical turbulence velocity and characteristic length-scale are provided. The underlying dynamo models suggest magnetic intermittency and possibly a largescale hydrodynamic viscosity. We conclude that the success of the model to explain the £eld strength in cool core clusters indicates that in general cluster magnetic £elds directly re¤ect hydrodynamical turbulence, also in clusters without cool cores.

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A catalog of intracluster gas temperatures

Cited by 413 publications

References 0 publications

Scaling Relations for Galaxy Clusters: Properties and Evolution

Scaling Relations for Galaxy Clusters: Properties and Evolution

The environments of FRII radio sources

Magnetic turbulence in cool cores of galaxy clusters

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