  We present a recent ALMA observation of the CO(1-0) line emission in the
central galaxy of the Zw 3146 galaxy cluster ($z=0.2906$). We also present
updated X-ray cavity measurements from archival Chandra observations. The
$5\times 10^{10}\,M_{\odot}$ supply of molecular gas, which is confined to the
central 4 kpc, is marginally resolved into three extensions that are
reminiscent of the filaments observed in similar systems. No velocity structure
that would be indicative of ordered motion is observed. The three molecular
extensions all trail X-ray cavities, and are potentially formed from the
condensation of intracluster gas lifted in the wakes of the rising bubbles.
Many cycles of feedback would be require to account for the entire molecular
gas reservoir. The molecular gas and continuum source are mutually offset by
2.6 kpc, with no detected line emission coincident with the continuum source.
It is the molecular gas, not the continuum source, that lies at the
gravitational center of the brightest cluster galaxy. As the brightest cluster
galaxy contains possible tidal features, the displaced continuum source may
correspond to the nucleus of a merging galaxy. We also discuss the possibility
that a gravitational wave recoil following a black hole merger may account for
the displacement.
