Chandra Temperature Profiles for a Sample of Nearby Relaxed Galaxy Clusters

By A. Vikhlinin, M. Markevitch, S. Murray, C. Jones, W. Forman, L. V. Speybroeck. 2004

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We present Chandra gas temperature profiles at large radii for a sample of 13 nearby, relaxed galaxy clusters and groups, which includes A133, A262, A383, A478, A907, A1413, A1795, A1991, A2029, A2390, MKW 4, RX J1159+5531, and USGC S152. The sample covers a range of average temperatures from 1 to 10 keV. The clusters are selected from the archive or observed by us to have sufficient exposures and off-center area coverage to enable accurate background subtraction and reach the temperature accuracy of better than 20%-30% at least to r = (0.4-0.5)r180 and for the three best clusters to (0.6-0.7)r180. For all clusters, we find cool gas in the cores, outside of which the temperature reaches a peak at r ~ 0.15r180 and then declines to ~0.5 of its peak value at r ≃ 0.5r180. When the profiles are scaled by the cluster average temperature (excluding cool cores) and the estimated virial radius, they show large scatter at small radii but remarkable similarity at r > (0.1-0.2)r180 for all but one cluster (A2390). Our results are in good agreement with previous measurements from ASCA by Markevitch et al. and from BeppoSAX by De Grandi & Molendi. Four clusters have recent XMM-Newton temperature profiles, two of which agree with our results, and we discuss reasons for disagreement for the other two. The overall shape of the temperature profiles at large radii is reproduced in recent cosmological simulations.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f09348b545bfe88a6e4bf1b743f3c5347e8e5e1e

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Citations in the corpus

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).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, background): “…negative gradients outside core regions, a trend that extends out to the largest radii covered so far by observations(e.g., De Grandi & Molendi 2002; Vikhlinin et al. 2005; Zhang et al. 2006; Baldi et al. 2007; Pratt et al. 2007; Leccardi & Molendi 2008b); gas entropy is higher than expected from…”
Weighing simulated galaxy clusters using lensing and X-ray (2009, methodology): “…consists of measuring the concentration-mass relation of clusters and of comparing Article published by EDP Sciences Page 1 of 23 it with the theoretical predictions (e.g. Pointecouteau et al. 2005; Vikhlinin et al. 2005; Buote et al. 2007; Schmidt & Allen 2007; Comerford & Natarajan 2007).”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, methodology): “This is, effectively, the largest radius at which the ICM temperature can be reliably measured with Chandra and XMM-Newton (e.g., Vikhlinin et al. 2005; Pratt et al. 2007).”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, methodology): “The preliminary comparison with observational data, presented in this paper, shows an encouraging agreement with the profiles of the iron abundance as obtained from Chandra observations of a set of nearby relaxed clusters (Vikhlinin et al. 2005).”
Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, background): “…and its gradient, and unfortunately, even with the two new generation X-ray telescopesXMM-Newton andChandra, it is difficult to achieve such measurements beyond half the virial radius for galaxy clusters (Pointecouteau et al. 2005; Vikhlinin et al. 2005), and even much less for elliptical galaxies.”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, methodology): “…scaled and tied when trying to determin the residual CXB. 7 The edge component is a correction to underestimation of Chandra’sefficiency at∼2 keV (see Vikhlinin et al. 2005). used the radio measured hydrogen absorption columns from the Leiden/Argentine/Bonn HI-Survey (Kalberla et al. 2005) or,…”
The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, background): “…are rendered uncertain by incomplete modeling of ICM physics and by systematic errors associated with determining the spectral temperature derived from the thermally complex intracluster medium of simulated clusters (Mathiesen & Evrard 2001b; Mazzotta et al. 2003; Vikhlinin et al. 2005).”
The case for electron re-acceleration at galaxy cluster shocks (2017, methodology): “The data were reduced with the chav package, following the processing described in [38] and applying the CALDB 4.”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “In the centers of clusters where radiative cooling is important, the gas temperature declines by factors of two to three (Allen et al. 2001; Vikhlinin et al. 2005).”
The observed concentration–mass relation for galaxy clusters (2007, neutral): “8+5531 0.081 X-ray 8.3± 2.1 0.787 ± 0.533 10.6 ± 2.6 0.908 ± 0.686 Gastaldello et al. (2006) X-ray 2.63 ± 0.43 3.51 ± 0.55 Vikhlinin et al. (2005) Abell 1651 0.0825 X-ray 4.9± 0.2 6.4± 0.3 Xu et al. (2001) Abell 2597 0.0852 X-ray 5.86 ± 0.50 3.00 ± 0.33 7.59 ± 0.63 3.54 ± 0.42 Pointecouteau et al.…”
STIRRING UP THE POT: CAN COOLING FLOWS IN GALAXY CLUSTERS BE QUENCHED BY GAS SLOSHING? (2009, background): “In particular, our main cluster closely resembles A2029 (e.g., Vikhlinin et al. 2005), a hot, relatively relaxed cluster with sloshing in the cool core.”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “Luckily, the universal temperature profile in Vikhlinin et al. (2005) is based on the temperature profiles well resolved spatially for 13 low redshift galaxy clusters.”
Searching for cool core clusters at high redshift (2008, methodology): “Therefore, we expect to observe a surface brightness (SB) peak in these regions (with a typical radius of the order of 70 kpc - see for example Vikhlinin et al. 2005) along with some other features such as an enhanced iron abundance.”
Images, Structural Properties, and Metal Abundances of Galaxy Clusters Observed with Chandra ACIS-I at 0.1 < z < 1.3 (2007, methodology): “The gas cooling in cool cores is still significant however; core temperatures of ∼ 30% of the global value are typical, with detectable cooling extending to ∼ 0.15R500 (e.g. Vikhlinin et al. 2005; Sanderson et al. 2006)2.”
Calibration of the galaxy cluster M-500-Υ-x relation with XMM-Newton (2007, methodology): “This derivation is free of any assumption on profile shape, such as power 1 The difference is 3% for A1413 (Arnaud et al. 2005), a cluster for which the temperature profiles measured up toR500 both with XMM-Newton and Chandra are in excellent agreement (Pratt & Arnaud 2002; Vikhlinin et al. 2005).”
INTRACLUSTER MEDIUM ENTROPY PROFILES FOR A CHANDRA ARCHIVAL SAMPLE OF GALAXY CLUSTERS (2009, methodology): “Following the analysis described in Vikhlinin et al. (2005), soft residuals were created and fitted for each observation to account for the spatially varying soft Galactic background (see also Cavagnolo et al. 2008b).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, background): “Therefore, a second correction besides subtracting the scaled blank-sky background is required (e.g., Vikhlinin et al. 2005).”