Temperature profiles of a representative sample of nearby X-ray galaxy clusters

By G. Pratt, H. Böhringer, Judith Croston, M. Arnaud, Stefano Borgani, A. Finoguenov, R. Temple. 2006

186 citations recorded by the source corpus.

Context. A study of the structural and scaling properties of the temperature distribution of the hot, X-ray emitting intra-cluster medium of galaxy clusters, and its dependence on dynamical state, can give insights into the physical processes governing the formation and evolution of structure. Aims. Accurate temperature measurements are a pre-requisite for a precise knowledge of the thermodynamic properties of the intra-cluster medium. Methods. We analyse the X-ray temperature profiles from XMM-Newton observations of 15 nearby (z < 0.2) clusters, drawn from a statistically representative sample. The clusters cover a temperature range from 2.5 keV to 8.5 keV, and present a variety of X-ray morphologies. We derive accurate projected temperature profiles to ∼0.5 R 200 , and compare structural properties (outer slope, presence of cooling core) with a quantitative measure of the X-ray morphology as expressed by power ratios. We also compare the results to recent cosmological numerical simulations. Results. Once the temperature profiles are scaled by an average cluster temperature (excluding the central region) and the estimated virial radius, the profiles generally decline in the region 0.1 R 200 ≤ R ≤ 0.5 R 200 . The central regions show the largest scatter, attributable mostly to the presence of cool core clusters. There is good agreement with numerical simulations outside the core regions. We find no obvious correlations between power ratio and outer profile slope. There may however be a weak trend with the existence of a cool core, in the sense that clusters with a central temperature decrement appear to be slightly more regular. Conclusions. The present results lend further evidence to indicate that clusters are a regular population, at least outside the core region.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c5be5bb27aea4311d3deb777051a949e85bc9923

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Citations in the corpus

A Catalog of Galaxy Clusters Observed by XMM-Newton (2007, background): “Analysis of samples of cooling flow clusters with XMM-Newton (Piffaretti et al. 2005; Arnaud, Pointecouteau, & Pratt 2005; Pratt et al. 2007) are also mostly consistent with the Markevitch et al. (1998) results.”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, methodology): “For the five groups that were studied in V05 and this work, both works find excess absorption for the same three groups.”
A Measurement of Large-Scale Peculiar Velocities of Clusters of Galaxies: Results and Cosmological Implications (2008, methodology): “This decrease agrees withg 1 0.6T ∝ n ∝ r TX e X simulations of cluster formation within the LCDM model (Borgani et al. 2004) and with the available data on the X-ray temperature profile (Pratt et al. 2007).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, background): “…holds almost independently of the physical processes included in the simulations (e.g., Loken et al. 2002; Borgani et al. 2004; Kay et al. 2007; Pratt et al. 2007; Nagai et al. 2007), should be regarded as a success of cosmological simulations of galaxy clusters, the same simulations have much…”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, background): “Usually, T is overestimated because the observed T (r) decreases at large radii (Markevitch et al. 1998; de Grandi & Molendi 2002; Vikhlinin et al. 2005; Pratt et al. 2007).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, background): “…indicate a similar universal temperature profile with a significant decline beyond cluster cores in observations (e.g. Markevitch et al. 1998; De Grandi & Molendi 2002; Vikhlinin et al. 2005; Zhang et al. 2004, 2005a, 2006, 2007; Pratt et al. 2007) and simulations (e.g. Borgani et al. 2004).”
Radial temperature profiles for a large sample of galaxy clusters observed with XMM-Newton (2008, result): “Recent observations with current experiments (i.e.XMM-Newton and Chandra) have clearly shown that cluster temperature profiles decline beyond the 15-20% of R180 (Piffaretti et al. 2005; Vikhlinin et al. 2005; Pratt et al. 2007; Snowden et al. 2008).”
Total mass biases in X-ray galaxy clusters (2008, background): “…of the ICM has been significantly improved (e.g. Vikhlinin et al. 2006) through observational progress, which showed the existence of temperature profiles declining with radius (De Grandi & Molendi 2002; Vikhlinin et al. 2005; Piffaretti et al. 2005; Sanderson et al. 2006; Pratt et al. 2007).”
Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology (2007, background): “The exact regions sampled depend on the observing conditions, but high-quality data typically extend to r500 (Pratt et al. 2006).”
Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS) (2008, result): “|X) method gives precisely the same results as the modified weighted least squares (WLSS) method describedin Pratt et al. (2006). emission and also appear to scale somewhat more tightly in the outer regions.”
Galaxy-cluster gas-density distributions of the Representative XMM-Newton Cluster Structure Survey (REXCESS) (2008, methodology): “The power ratio method used here is described in more detail in Pratt et al. (2007).”
The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y-SZ-M-500 relation (2009, methodology): “This behaviour was also noticed by Nagai et al. (2007) when comparing their simulations with Chandra relaxed clusters, and it is also observed for the temperature profiles (see Pratt et al. 2007).”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, methodology): “Full details of the depro- 3 Our adoption of FWC data allows the use of a physical model for the X-ray background, in contrast to our previous analysis which used a blank sky background (Pratt et al. 2007).”
Formation of Galaxy Clusters (2012, background): “The presence of cool cores is also reflected in the observed temperature profiles (e.g. Leccardi & Molendi 2008, Pratt et al. 2007, Vikhlinin et al. 2006, see also Figure 4), which exhibit decline of temperature with decreasing radius in the innermost regions of relaxed cool–core clusters.”
A NEW MEASUREMENT OF THE BULK FLOW OF X-RAY LUMINOUS CLUSTERS OF GALAXIES (2009, background): “The temperature TX of hot gas distributed according to these profiles decreases significantly from the cluster cores to the cluster outskirts (Komatsu & Seljak 2001), consistent with current measurements (Pratt et al. 2007) and numerical simulations (e.g., Borgani et al. 2004).”
The representative XMM-Newton cluster structure survey (REXCESS) of an X-ray luminosity selected galaxy cluster sample (2007, methodology): “, and one study on the cluster temperature profiles, showing a high degree of universality of these profiles (outside the central regions) has been published (Pratt et al. 2007).”
A unified model for AGN feedback in cosmological simulations of structure formation (2007, background): “Indeed, a number of observational studies (e.g. De Grandi & Molendi, 2002; Vikhlinin et al., 2005; Dunn & Fabian, 2006; Pratt et al., 2007) have shown that the central temperature profiles of relaxed, cool core clusters decrease with decreasing radius, while at the same time these systems require…”