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We present new, deep observations of the Phoenix cluster from the ChandraX-ray Observatory, the Hubble Space Telescope, and the Karl Jansky Very LargeArray. These data provide an order of magnitude improvement in depth and/orangular resolution at X-ray, optical, and radio wavelengths, yielding anunprecedented view of the core of the Phoenix cluster. We find that theone-dimensional temperature and entropy profiles are consistent withexpectations for pure-cooling hydrodynamic simulations and analyticdescriptions of homogeneous, steady-state cooling flow models. In the inner ~10kpc, the cooling time is shorter by an order of magnitude than any other knowncluster, while the ratio of the cooling time to freefall time approaches unity,signaling that the ICM is unable to resist multiphase condensation on kpcscales. When we consider the thermodynamic profiles in two dimensions, we findthat the cooling is highly asymmetric. The bulk of the cooling in the inner ~20kpc is confined to a low-entropy filament extending northward from the centralgalaxy. We detect a substantial reservoir of cool (10^4 K) gas (as traced bythe [OII] doublet), which is coincident with the low-entropy filament. The bulkof this cool gas is draped around and behind a pair of X-ray cavities,presumably bubbles that have been inflated by radio jets, which are detectedfor the first time on kpc scales. These data support a picture in which AGNfeedback is promoting the formation of a multiphase medium via a combination ofordered buoyant uplift and locally enhanced turbulence. These processes oughtto counteract the tendency for buoyancy to suppress condensation, leading torapid cooling along the jet axis. The recent mechanical outburst has sufficientenergy to offset cooling, and appears to be coupling to the ICM via a cocoonshock, raising the entropy in the direction orthogonal to the radio jets.

Anatomy of a Cooling Flow: The Feedback Response to Pure Cooling in the Core of the Phoenix Cluster