Multiphase gas flows in the nearby Seyfert galaxy ESO428-G14
  We present ALMA rest-frame 230 GHz continuum and CO(2-1) line observations of
the nearby Compton-thick Seyfert galaxy ESO428-G14, with angular resolution 0.7
arcsec (78 pc). We detect CO(2-1) emission from spiral arms and a
circum-nuclear ring with 200 pc radius, and from a transverse gas lane with
size of $\sim100$ pc, which crosses the nucleus and connects the two portions
the circumnuclear ring. The molecular gas in the host galaxy is distributed in
a rotating disk with intrinsic circular velocity $v_{rot}=135$ km/s,
inclination $i=57$ deg, and dynamical mass $M_{dyn }=5\times 10^9~\rm
M_{\odot}$ within a radius of $\sim 1$ kpc. In the inner 100 pc region CO is
distributed in a equatorial bar, whose kinematics is highly perturbed and
consistent with an inflow of gas towards the AGN. This inner CO bar overlaps
with the most obscured, Compton-thick region seen in X-rays. We derive a column
density of $\rm N(H_2) \approx 2\times10^{23}~ cm^{-2}$ in this region,
suggesting that molecular gas may contribute significantly to the AGN
obscuration. We detect a molecular outflow with a total outflow rate $\rm \dot
M_{of}\approx 0.8~M_{\odot}/yr$, distributed along a bi-conical structure with
size of $700$ pc on both sides of the AGN. The bi-conical outflow is also
detected in the $\rm H_2$ emission line at 2.12 $\mu$m, which traces a warmer
nuclear outflow located within 170 pc from the AGN. This suggests that the
outflow cools with increasing distance from the AGN. We find that the hard
X-ray emitting nuclear region mapped with Chandra is CO-deprived, but filled
with warm molecular gas traced by $\rm H_2$ - thus confirming that the hard
(3-6 keV) continuum and Fe K$\alpha$ emission are due to scattering from dense
neutral clouds in the ISM.
