The X‐ray virial relations for relaxed lensing clusters observed with Chandra

By S. Allen, R. Schmidt, A. C. Fabian. 2001

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We examine the relations linking mass, X-ray temperature and bolometric luminosity for a sample of luminous, relatively relaxed clusters of galaxies observed with the Chandra Observatory, for which independent confirmation of the mass results is available from gravitational lensing studies. Within radii corresponding to a fixed overdensity with respect to the critical density at the redshifts of the clusters, the observed temperature profiles, scaled in units of T2500 and r2500, exhibit an approximately universal form which rises within and then remains approximately constant out to r2500. We obtain best-fitting slopes for the mass–temperature and temperature–luminosity relations consistent with the predictions from simple scaling arguments i.e. and , respectively. We confirm the presence of a systematic offset of ∼40 per cent between the normalizations of the observed and predicted mass–temperature relations for both SCDM and ΛCDM cosmologies.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/eb71126efbc0bf6eb09ee72a33665153d8c6b978

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Citations in the corpus

Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3 (2003, methodology): “We measure Bz = −1.04±0.32 when our data are compared to the determination by Ettori et al. (2002) at median redshift of 0.05, and Bz = −0.16 ± 0.23 when comparing to the results by Allen et al. (2001c) for clusters at median redshift of 0.28 (Fig.”
Hydrodynamical simulations of cluster formation with central AGN heating (2005, background): “…the estimated rate of accretion on to the central galaxy is rather high in many cases (e.g. Fabian, Nulsen & Canizares 1984; White et al. 1994; White, Jones & Forman 1997; Allen 2000; Allen et al. 2001a), implying that a significant amount of gas cooler than 1–2 keV should be present in the centre.”
The structural and scaling properties of nearby galaxy clusters. I. The universal mass profile (2005, methodology): “We used the function given by Allen et al. (2001):T (r) = T0 + T1 [ (r/rc)η 1+(r/rc)η ] to fit the an- 4 The effects of the PSF correction are most noticeable for A2204 and A478.”
THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, methodology): “These new data have shown that Equation 6 with a unique β value cannot always describe the surface brightness profile of clusters (e.g. Allen et al. 2001).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, background): “Most CCCs show simpler morphologies than non-CCCs, though this is not always the case, e.g. Abell 2390 (Allen et al. 2001; Swinbank et al. 2006).”
The Birmingham-CfA cluster scaling Project – I. Gas fraction and the M-Tx relation (2003, methodology): “Allen et al. (2001) find a M − TX logarithmic slope of 1.51 ± 0.27 within a radius of overdensity of 2500, which is approximately equivalent to 0.3R200.”
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 Sunyaev-Zel'dovich angular power spectrum as a probe of cosmological parameters (2002, background): “…the virial radius, roughly corresponding tor2500, which is just in the range ofChandrasatellite for medium redshift clusters (McNamara et al. 2000; Allen, Ettori, & Fabian 2001; Allen et al. 2001) and well withinXMM/Newtonor BeppoSax(Arnaud et al. 2001a; Arnaud et al. 2001b; Kaastra et al. 2001).”
The mass profile of A1413 observed with XMM-Newton: Implications for the M-T relation (2002, methodology): “On the other hand, the c parameters of Allen et al. (2001a) are better in agreement with the theoretical predictions.”
Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster (2002, result): “…are also consistent with their X-ray cluster observations at re0:1rvir (e.g., Ettori et al. 2002b; Pratt & Arnaud 2002; Schmidt et al. 2001; Allen et al. 2001; Arabadjis et al. 2002), while gravitational lensing studies report conflicting results in cluster cores (i.e., Sand et al. 2002;…”
Sample Variance Considerations for Cluster Surveys (2002, result): “…between simulation results for β is at least comparable to this shift and the discrepancy between the theoretical fits to M−TX in simulations and observed relation (Hjorth et al. 1998; Horner et al. 1999; Nevalainen et al. 2000; Finoguenov et al. 2001; Allen et al. 2001) is more substantial still.”
A comparison of weak-lensing masses and X-ray properties of galaxy clusters (2007, result): “For a cluster with a temperature of kT = 5 keV we obtain a mass M2500 = (1.4 ± 0.2) × 1014 h−1 M , in fair agreement with recent Chandra and XMM studies (e.g. Allen et al. 2001; Arnaud et al. 2005; Vikhlinin et al. 2006).”
Spatially resolved X-ray spectroscopy of cooling clusters of galaxies (2003, unknown): “Since the virial radius scales also withT 0.5h , the ratio ofrc to the virial radius is not constant, contrary to the findings of Allen et al. (2001).”