  We present a multiwavelength study of RXC J2014.8-2430, the most extreme
cool-core cluster in the Representative $XMM-Newton$ Cluster Structure Survey
(REXCESS), using $Chandra$ X-ray, Southern Astrophysical Research (SOAR)
Telescope, Atacama Large Millimeter/submillimeter Array (ALMA), Very Large
Array (VLA), and Giant Metrewave Radio Telescope (GMRT) observations. While
feedback from an active galactic nucleus (AGN) is thought to be the dominant
mechanism by which a cooling flow is suppressed, the $Chandra$ imaging
observations surprisingly do not reveal the bi-lateral X-ray cavities expected
in the intracluster medium (ICM) of an extreme cool core hosting a powerful
radio source. We discuss the limits on the presence of any radio bubbles
associated with any undetected X-ray cavities. We place upper limits on any
significant X-ray AGN in the brightest cluster galaxy, and show that the X-ray
peak is offset from the central radio source, which exhibits a steep low
frequency radio spectrum indicative of electron ageing. The SOAR data reveal an
extended, luminous emission line source. From our narrowband H$\alpha$ imaging
of the BCG, the central H$\alpha$ peak is coincident with the radio
observations, yet offset from the X-ray peak, consistent with sloshing found
previously in this cluster. ALMA observations reveal a large reservoir of
molecular gas that traces the extended H$\alpha$ emission. We conclude either
that the radio source and its cavities in the X-ray gas are nearly aligned
along the line of sight, or that ram pressure induced by sloshing has
significantly displaced the cool molecular gas feeding it, perhaps preempting
the AGN feedback cycle. We argue that the sloshing near the core is likely
subsonic, as expected, given the co-location of the H$\alpha$, CO(1-0), radio
continuum, and stellar emission peaks and their proximity to the intact cool
core seen in X-ray.
