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It has long been suspected that powerful radio sources may lower theefficiency with which stars form from the molecular gas in their host galaxy,but so far, alternative mechanisms, in particular related to the stellar massdistribution in the massive bulges of their host galaxies, are not ruled out.We present new ALMA CO(1-0) interferometry of cold molecular gas in the nearby(z=0.0755), massive (M_stellar=4x10^11 M_sun), isolated, late-type spiralgalaxy 2MASSX J23453269-044925, which is outstanding for having two pairs ofpowerful, giant radio jets, and a bright X-ray halo. The molecular gas is in amassive (M_gas=2x10^10 M_sun), 24 kpc wide, rapidly rotating ring, which isassociated with the inner stellar disk. Broad (FWHM=70-180 km s^-1) lines withcomplex profiles associated with the radio source are seen over large regionsin the ring, indicating gas velocities that are high enough to keep theotherwise marginally Toomre-stable gas from fragmenting into gravitationallybound, star-forming clouds. About 1-2% of the jet kinetic energy are requiredto power these motions. Resolved star-formation rate surface densities fallfactors 50-75 short of expectations from the Kennicutt-Schmidt law ofstar-forming galaxies, and near gas-rich early-type galaxies with signatures ofstar formation lowered by jet feedback. We argue that radio AGN feedback is theonly plausible mechanism to explain the low star-formation rates in thisgalaxy. Previous authors have already noted that the X-ray halo of J2345-0449implies a baryon fraction near the cosmic average, which is very high for agalaxy. We contrast this finding with other, equally massive baryon-rich spiralgalaxies without prominent radio sources. Most of the baryons in these galaxiesare in stars, not in the halos. We also discuss the implications of our resultsfor our general understanding of AGN feedback in massive galaxies.

Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with bright X-ray halo