The X-ray virial relations for relaxed lensing clusters observed withChandra

Abstract

A B S T R A C TWe 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 D ¼ 2500 with respect to the critical density at the redshifts of the clusters, the observed temperature profiles, scaled in units of T 2500 and r 2500 , exhibit an approximately universal form which rises within r , 0:3r 2500 and then remains approximately constant out to r 2500 . We obtain best-fitting slopes for the mass -temperature and temperature -luminosity relations consistent with the predictions from simple scaling arguments i.e. M 2500 / T 3=2 2500 and L 2500 / T 2 2500 , 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 LCDM cosmologies.

Clusters of galaxies: new results from the CLEF hydrodynamics simulation

“…The thick band is the observed relation derived by (Allen, Schmidt and Fabian, 2001), in good agreement with our results.…”

“…The solid line is the best-fit relation, allowing both the normalisation and slope to vary. The solid band is the best-fit relation to clusters studied by Allen, Schmidt and Fabian (2001).…”

Lensing & Dynamics in the Galaxy Cluster MS2137-23

“…X-rays measurements of Allen et al (2001) confirm our conclusions. Small departs may occur at very small scales r 1 kpc, which are dominated by stars and are well below the actual spatial resolution of numerical simulations.…”

“…The lens properties of the cluster have been extensively studied (Fort et al 1992;Mellier et al 1993;Miralda-Escudé 1995;Bartelmann 1996;Hammer et al 1997;Gavazzi et al 2003). The cluster lies at z l = 0.313 and the sources responsible of the radial and tangential arcs both lie at z s ≈ 1.501, leading to the critical surface density Σ crit = 2.39 × 10 9 h 70 M kpc −2 .…”

Scaling Relations for Galaxy Clusters: Properties and Evolution

“…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.…”