Molecular gas in the northern nucleus of Mrk273: Physical and chemical
  properties of the disk and its outflow
  Aiming to characterise the properties of the molecular gas in the
ultraluminous infrared galaxy Mrk273 and its outflow, we used the NOEMA
interferometer to image the dense gas molecular tracers HCN, HCO+, HNC, HOC+
and HC3N at 86GHz and 256GHz with angular resolutions of 4.9x4.5 arcsec
(3.7x3.4 kpc) and 0.61x0.55 arcsec (460x420 pc). We also modelled the flux of
several H2O lines observed with Herschel using a radiative transfer code that
includes excitation by collisions as well as by far-infrared photons. The disk
of the Mrk273 north nucleus has two components with decoupled kinematics. The
gas in the outer parts (1.5 kpc) rotates with a south-east to north-west
direction, while in the inner disk (300 pc) follows a north-east to south-west
rotation. The central 300 pc, which hosts a compact starburst region, is filled
with dense and warm gas, contains a dynamical mass of (4-5)x10^9M_sun, a
luminosity of L'_HCN=(3-4)x10^8 K km/s pc^2, and a dust temperature of 55 K. At
the very centre, a compact core with R~50 pc has a luminosity of
L_IR=4x10^11L_sun (30% of the total infrared luminosity), and a dust
temperature of 95 K. The core is expanding at low velocities ~50-100 km/s,
probably affected by the outflowing gas. We detect the blue-shifted component
of the outflow, while the red-shifted counterpart remains undetected in our
data. Its cold and dense phase reaches fast velocities up to ~1000 km/s, while
the warm outflowing gas has more moderate maximum velocities of ~600 km/s. The
outflow is detected as far as 460 pc from the centre in the northern direction,
and has a mass of dense gas <8x10^8M_sun. The difference between the position
angles of the inner disk (~70 degree) and the outflow (~10 degree) indicates
that the outflow is likely powered by the AGN, and not by the starburst.
Regarding the chemistry, we measure an extremely low HCO+/HOC+ ratio of 10+-5
in the inner disk of Mrk273.
