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

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

2003-11-21

arxiv.org/abs/astro-ph/0311502v2

Mon.Not.Roy.Astron.Soc.349:952,2004

Astronomy and Astrophysics

Astrophysics

~20 pages, colour, accepted by MNRAS. Updates include a more extensive discussion of the hard component, reference corrections

Scientific paper

10.1111/j.1365-2966.2004.07576.x

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.

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