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[Abridged] We present new optical integral field spectroscopy (Gemini South)and submillimeter spectroscopy (Submillimeter Array) of the central galaxy inthe Phoenix cluster (SPT-CLJ2344-4243). This cluster was previously reported tohave a massive starburst (~800 Msun/yr) in the central, brightest clustergalaxy, most likely fueled by the rapidly-cooling intracluster medium. Thesenew data reveal a complex emission-line nebula, extending for >30 kpc from thecentral galaxy. The total Halpha luminosity, assuming Halpha/Hbeta = 2.85, isL_Ha = 7.6 +/- 0.4 x10^43 erg/s, making this the most luminous emission linenebula detected in the center of a cool core cluster. Overall, the relativefluxes of the low-ionization lines (e.g., [O II], Hbeta) to the UV continuumare consistent with photoionization by young stars. In both the center of thegalaxy and in a newly-discovered highly-ionized plume to the north of thegalaxy, the ionization ratios are consistent with both shocks and AGNphotoionization. We speculate that this extended plume may be a galactic wind,driven and partially photoionized by both the starburst and central AGN. Wefind evidence for shocks throughout the ISM of the central galaxy, most likelydriven by a combination of stellar winds from massive young stars,core-collapse supernovae, and the central AGN. In addition to the warm, ionizedgas, we detect a substantial amount of cold, molecular gas via the CO(3-2)transition, coincident in position with the galaxy center. We infer a moleculargas mass of M_H2 = 2.2 +/- 0.6 x10^10 Msun, which implies that the starburstwill consume its fuel in ~30 Myr if it is not replenished. The combination ofthe high level of turbulence in the warm phase and the high L_IR/M_H2 ratiosuggests that this violent starburst may be in the process of quenching itself.

The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (SPT-CLJ2344-4243)