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We present the results of a Chandra study of the Hydra A galaxy cluster,where a powerful AGN outburst created a large-scale cocoon shock. Weinvestigated possible azimuthal variations in shock strength and shape, findingindications for a weak shock with a Mach number in the range ~1.2-1.3. Wemeasured the temperature change across the shock front. However, the detectionof a temperature rise in the regions immediately inside of the front iscomplicated by the underlying temperature profile of the cluster atmosphere. Wemeasured the global temperature profile of the cluster up to 700 kpc, whichrepresents the farthest measurement obtained with Chandra for this cluster. A"plateau" in the temperature profile in the range ~70-150 kpc indicates thepresence of cool gas, which is likely the result of uplift of material by theAGN outburst. After masking the cool filaments visible in the hardness ratiomap, the plateau disappears and the temperature profile recovers a typicalshape with a peak around 190 kpc, just inside the shock front. However, it isunlikely that such a temperature feature is produced by the shock as it isconsistent with the general shape of the temperature profiles observed forrelaxed galaxy clusters. We studied the spectral properties of the coolfilaments finding evidence that ~10^11 M_sun of low-entropy material has beendredged up by the rising lobes from the central 30 kpc to the observed currentposition of 75-150 kpc. The energy required to lift the cool gas is >~2.2 x10^60 erg, which is comparable to the work required to inflate the cavities andis ~25% of the total energy of the large-scale shock. Our results show that theAGN feedback in Hydra A is acting not only by directly heating the gas, butalso by removing a substantial amount of potential fuel for the SMBH.

A Chandra study of the large-scale shock and cool filaments in Hydra A: Evidence for substantial gas dredge-up by the central outburst