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The archetype FR-II galaxy Cygnus A lies in a moderately rich cluster aboutto undergo a major merger. We study the pre-merger Cygnus cluster environmentusing smoothed particle hydrodynamics simulations constrained by 2Ms of Chandraobservations of the hot intracluster medium. The observations constrain thetotal gravitating mass and concentration parameter, and the simulations providethe quiescent and merger-enhanced temperature profiles of the pre- and postmerger of the cluster excluding the central active galactic nucleus. We presentthe first detailed model of the sub cluster north west of Cygnus A, namedCygNW. We find a lower baryon fraction and higher concentration parameter forCygA than expected from known scaling relations in the literature. The modelsuggests the Cygnus cluster hosts a pre-merger with a progenitor mass ratio ofabout 1.5:1 at the virial radius. We notice that the intra cluster medium isheated as a result of the merger, but we find no evidence for a (pre-)mergershock in the interstitial region between both cluster haloes. We attribute themerger-induced heating to compression of the cluster outskirts. The smoothmodel obtained from our simulations is subtracted from the observed clusterstate and shows residual temperature structure that is neither hydrostatic normerger-heated cluster gas. We speculate that this residual heating may resultfrom previous AGN activity over the last ~100 Myr.

Simulations of the merging cluster of galaxies Cygnus A