Galaxy-cluster gas-density distributions of the Representative XMM-Newton Cluster Structure Survey (REXCESS)

By Judith Croston, G. Pratt, H. Böhringer, M. Arnaud, E. Pointecouteau, Trevor J. Ponman, A. Sanderson, R. Temple, Richard G. Bower, M. Donahue. 2008

149 citations recorded by the source corpus.

We present a study of the structural and scaling properties of the gas distributions in the intracluster medium (ICM) of 31 nearby (z 3 keV scale self-similarly, with no temperature dependence of gas-density normalisation. The REXCESS sample allows us to investigate the correlations between cluster properties and dynamical state. We find no evidence of correlations between cluster dynamical state and either the gas density slope in the inner regions or temperature, but do find some evidence of a correlation between dynamical state and outer gas density slope. We also find a weak correlation between dynamical state and both central gas normalisation and inner cooling times, but this is only significant at the 10% level. We conclude that, for the X-ray cluster population as a whole, both the central gas properties and the angle-averaged, large-scale gas properties are linked to the cluster dynamical state. We also investigate the central cooling times of the clusters. While the cooling times span a wide range, we find no evidence of a significant bimodality in the distributions of central density, density gradient, or cooling time. Finally, we present the gas mass-temperature relation for the REXCESS sample, finding that h(z)Mgas ∝ T 1.99±0.11 , which is consistent with the expectation of self-similar scaling modified by the presence of an entropy excess in the inner regions of the cluster and consistent with earlier work on relaxed cluster samples. We measure a logarithmic intrinsic scatter in this relation of ∼10%, which should be a good measure of the intrinsic scatter in the Mgas−T relation for the cluster population as a whole.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cfc15db74f9eb5cb126ed602ceb98665c0cab2df

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Towards a realistic population of simulated galaxy groups and clusters (2013, background): “8 and observational estimates of Croston et al. (2008) for the representative REXCESS cluster sample.”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, background): “…distances ∼ > 0.1R500 (e.g., Loken et al. 2002; Borgani et al. 2004; Kay et al. 2004; Roncarelli et al. 2006; Pratt et al. 2007; Nagai et al. 2007; Croston et al. 2008); the observed entropy level atR500 is well reproduced by simulations including radiative cooling and star formation (e.g.,…”
Relativistic jet feedback in high-redshift galaxies – I. Dynamics (2016, background): “The density consists of an isothermal hot (T ∼ 107 K; typical of galaxy clusters and elliptical galaxies, Allen et al. 2006; Croston et al. 2008; Diehl & Statler 2008; Maughan et al. 2012; Goulding et al. 2016) halo in hydrostatic equilibrium and a dense warm (T 3.4 × 104 K) turbulent and…”
Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS) (2008, background): “TheREXCESS gas density profiles from which Mgas is derived are discussed in Croston et al. (2008).”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, methodology): “1) yields a more accurate description than the traditionalβ-model (see Croston et al. 2008, and references therein), most of the analyses listed in Sect.”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “…in cluster radial quantities has long been shown in X-ray observations (e.g., Arnaud et al. 2001; Pointecouteau et al. 2005; Vikhlinin et al. 2006; Croston et al. 2008; Arnaud et al. 2010), in the optical (e.g., Rines & Diaferio 2006; Wojtak & Lokas 2010), and with weak-lensing (e.g., Postman et…”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, methodology): “The procedure used to calculate the gas density profiles, plu extensive analysis of their properties, is described in full in Croston et al. (2008).”
The cool-core bias in X-ray galaxy cluster samples - I. Method and application to HIFLUGCS (2010, background): “At variance with the cores, it has been found that in cluster outskirts the surface-brightness profiles are essentially self-similar (Neumann 2005; Croston et al. 2008; Leccardi et al. 2010), so the selection based on the fluxes in the outer regions should be unbiased.”
The Karl G. Jansky Very Large Array Sky Survey (VLASS). Science Case and Survey Design (2019, background): “…such as whether the most powerful sources are expanding supersonically throughout their lifetimes (e.g., Begelman & Cioffi 1989; Hardcastle & Worrall 2000), or what provides the pressure supporting the lobes of low-power objects (e.g., Bı̂rzan et al. 2008; Croston et al. 2008) remain unanswered.”
Dark light, dark matter, and the misalignment mechanism (2011, methodology): “We take a free electron density curve from [29], replotted in 1, to determine the portion of (χ,M) parameter space in which this infall turns out to be adiabatic, taking the velocity of infall to be the escape velocity v(r) = √ GMc/r.”
Formation of Galaxy Clusters (2012, background): “A number of observational evidences, based on X–ray measurements of gas density (e.g. Croston et al. 2008) and temperature profiles (Leccardi & Molendi 2008, Pratt et al. 2007, Vikhlinin et al. 2006), and the combination of the two in the form of entropy profile (Cavagnolo et al. 2009), demonstrate…”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, methodology): “Specifically, for comparison to the Croston et al. (2008) REXCESS cluster sample we select all simulated clusters with a hydrostatic X-ray mass of M500,X−ray > 2× 10 14 M⊙ (of which there are 166 from the four independent volumes), yielding a median X-ray mass of ≈ 2.6 × 1014 M⊙.”
The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y-SZ-M-500 relation (2009, methodology): “2 The normalisation of the density profiles, scaled accordingto the standard self-similar model, varies with mass as shown by Croston et al. (2008).”