Suppression of Star Formation in NGC 1266
  NGC1266 is a nearby lenticular galaxy that harbors a massive outflow of
molecular gas powered by the mechanical energy of an active galactic nucleus
(AGN). It has been speculated that such outflows hinder star formation (SF) in
their host galaxies, providing a form of feedback to the process of galaxy
formation. Previous studies, however, indicated that only jets from extremely
rare, high power quasars or radio galaxies could impart significant feedback on
their hosts. Here we present detailed observations of the gas and dust
continuum of NGC1266 at millimeter wavelengths. Our observations show that
molecular gas is being driven out of the nuclear region at $\dot{M}_{\rm out}
\approx 110 M_\odot$ yr$^{-1}$, of which the vast majority cannot escape the
nucleus. Only 2 $M_\odot$ yr$^{-1}$ is actually capable of escaping the galaxy.
Most of the molecular gas that remains is very inefficient at forming stars.
The far-infrared emission is dominated by an ultra-compact ($\lesssim50$pc)
source that could either be powered by an AGN or by an ultra-compact starburst.
The ratio of the SF surface density ($\Sigma_{\rm SFR}$) to the gas surface
density ($\Sigma_{\rm H_2}$) indicates that SF is suppressed by a factor of
$\approx 50$ compared to normal star-forming galaxies if all gas is forming
stars, and $\approx$150 for the outskirt (98%) dense molecular gas if the
central region is is powered by an ultra-compact starburst. The AGN-driven bulk
outflow could account for this extreme suppression by hindering the
fragmentation and gravitational collapse necessary to form stars through a
process of turbulent injection. This result suggests that even relatively
common, low-power AGNs are able to alter the evolution of their host galaxies
as their black holes grow onto the M-$\sigma$ relation.
