  We detect bright [CII]158$\mu$m line emission from the radio galaxy 3C 326N
at z=0.09, which shows weak star formation ($SFR<0.07$M$_{\odot}$~yr$^{-1}$)
despite having strong H$_2$ line emission and $2\times 10^9$M$_{\odot}$ of
molecular gas. The [CII] line is twice as strong as the 0-0S(1) 17$\mu$m H$_2$
line, and both lines are much in excess what is expected from UV heating. We
combine infrared Spitzer and Herschel data with gas and dust modeling to infer
the gas physical conditions. The [CII] line traces 30 to 50% of the molecular
gas mass, which is warm (70<T<100K) and at moderate densities
$700<n_{H}<3000$cm$^{-3}$. The [CII] line is broad with a blue-shifted wing,
and likely to be shaped by a combination of rotation, outflowing gas, and
turbulence. It matches the near-infrared H$_2$ and the Na D optical absorption
lines. If the wing is interpreted as an outflow, the mass loss rate would be
larger than 20M$_{\odot}$/yr, and the depletion timescale shorter than the
orbital timescale ($10^8$yr). These outflow rates may be over-estimated because
the stochastic injection of turbulence on galactic scales can contribute to the
skewness of the line profile and mimic outflowing gas. We argue that the
dissipation of turbulence is the main heating process of this gas. Cosmic rays
can also contribute to the heating but they require an average gas density
larger than the observational constraints. We show that strong turbulent
support maintains a high gas vertical scale height (0.3-4kpc) in the disk and
can inhibit the formation of gravitationally-bound structures at all scales,
offering a natural explanation for the weakness of star formation in 3C 326N.
To conclude, the bright [CII] line indicates that strong AGN jet-driven
turbulence may play a key role in enhancing the amount of molecular gas
(positive feedback) but yet can prevent star formation on galactic scales
(negative feedback).

Astrophysics of Galaxies;Cosmology and Nongalactic Astrophysics