We present new ALMA observations tracing the morphology and velocity structure of the molecular gas in the central galaxy of the cluster Abell 1795 .
The molecular gas lies in two filaments that extend 5 - 7 kpc to the N and S from the nucleus and project exclusively around the outer edges of two inner radio bubbles .
Radio jets launched by the central AGN have inflated bubbles filled with relativistic plasma into the hot atmosphere surrounding the central galaxy .
The N filament has a smoothly increasing velocity gradient along its length from the central galaxy ’ s systemic velocity at the nucleus to -370 \hbox { $ km s ^ { -1 } $ } , the average velocity of the surrounding galaxies , at the furthest extent .
The S filament has a similarly smooth but shallower velocity gradient and appears to have partially collapsed in a burst of star formation .
The close spatial association with the radio lobes , together with the ordered velocity gradients and narrow velocity dispersions , show that the molecular filaments are gas flows entrained by the expanding radio bubbles .
Assuming a Galactic X _ { \mathrm { CO } } factor , the total molecular gas mass is 3.2 \pm 0.2 \times 10 ^ { 9 } \hbox { $ \thinspace M _ { \odot } $ } .
More than half lies above the N radio bubble .
Lifting the molecular clouds appears to require an infeasibly efficient coupling between the molecular gas and the radio bubble .
The energy required also exceeds the mechanical power of the N radio bubble by a factor of two .
Stimulated feedback , where the radio bubbles lift low entropy X-ray gas that becomes thermally unstable and rapidly cools in situ , provides a plausible model .
Multiple generations of radio bubbles are required to lift this substantial gas mass .
The close morphological association then indicates that the cold gas either moulds the newly expanding bubbles or is itself pushed aside and shaped as they inflate .