Mapping small-scale temperature and abundance structures in the core of the Perseus cluster

J.S. Sanders1, A.C. Fabian1, S.W. Allen1 and R.W. Schmidt2

  1. Institute of Astronomy, Madingley Road, Cambridge. CB3 0HA. UK
  2. Institut für Physik, Universität Potsdam, Am neuen Palais 10, D-14469 Potsdam, Germany.

We report further results from a 191 ks Chandra observation of the core of the Perseus cluster, Abell 426. The emission-weighted temperature and abundance structure is mapped detail. There are temperature variations down to ~1 kpc in the brightest regions. Globally, the strongest X-ray surface brightness features appear to be caused by temperature changes. Density and temperature changes conspire to give approximate azimuthal balance in pressure showing that the gas is in hydrostatic equilibrium. Si, S, Ar, Ca, Fe and Ni abundance profiles rise inward from about 100 kpc, peaking at about 30-40 kpc. Most of these abundances drop inwards of the peak, but Ne shows a central peak, all of which may be explained by resonance scattering. There is no evidence for a widespread additional cooler temperature component in the cluster with a temperature greater than a factor of two from the local temperature. There is however evidence for a widespread hard component which may be nonthermal. The temperature and abundance of gas in the cluster is observed to be correlated in a manner similar to that found between clusters.

Accepted version (MNRAS; astro-ph/0311502)

Includes a more extensive discussion of the hard component, corrections to the references, and a few other minor changes.

Last Modified on 2004-01-07. Comments to jss at