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Title:
The weak shock in the core of the Perseus cluster
Authors:
Graham, J.; Fabian, A. C.; Sanders, J. S.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA; ), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA; ), AC(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA; )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 386, Issue 1, pp. 278-288. (MNRAS Homepage)
Publication Date:
05/2008
Origin:
MNRAS
MNRAS Keywords:
clusters: individual: Perseus , cooling flows , intergalactic medium , X-rays: galaxies , galaxies
DOI:
10.1111/j.1365-2966.2008.13027.x
Bibliographic Code:
2008MNRAS.386..278G

Abstract

The dissipation of energy from sound waves and weak shocks is one of the most promising mechanisms for coupling active galactic nucleus (AGN) activity to the surrounding intracluster medium, and so offsetting cooling in cluster cores. We present a detailed analysis of the weak shock found in deep Chandra observations of the Perseus cluster core. A comparison of the spectra either side of the shock front shows that they are very similar. By performing a deprojection analysis of a sector containing the shock, we produce temperature and density profiles across the shock front. These show no evidence for a temperature jump coincident with the density jump. To understand this result, we model the shock formation using 1D hydrodynamic simulations including models with thermal conduction and γ < 5/3 gas. These models do not agree well with the data, suggesting that further physics is needed to explain the shock structure. We suggest that an interaction between the shock and the Hα filaments could have a significant effect on cooling the post-shock gas.

We also calculate the thermal energy liberated by the weak shock. The total energy in the shocked region is about 3.5 times the work needed to inflate the bubbles adiabatically, and the power of the shock is around 6 × 1044ergs-1 per bubble, just over 1045ergs-1 in total.

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