CO kinematics unveil outflows plausibly driven by a young jet in the
  Gigahertz Peaked Radio Core of NGC6328
  We report the detection of outflowing molecular gas in the center of the
nearby (z=0.014) massive radio galaxy NGC6328. The radio core of the galaxy,
PKS B1718-649, is identified as a Gigahertz Peaked Spectrum source with a
compact (2 pc) double radio lobe morphology. We used ALMA CO(2-1) and CO(3-2)
observations at 100 pc resolution to study the gas kinematics up to ~5 kpc from
the galaxy center. While the bulk of the molecular gas is settled in a highly
warped disk, in the inner 300 pc of the disk and along with the orientation of
the radio jet, we identified high-excitation and high-velocity gas that cannot
be attributed to any regular kinematic component based on our detailed 3D
modeling of the ALMA data. The high-velocity dispersion in the gas also
suggests that it is not part of an inflowing, shredding structure. These
results suggest the presence of a molecular outflow of 3 to 8 solar masses per
year. The outflow possibly originated from the interaction of the jet with the
dense interstellar medium, even though the radio emission is detected closer to
the center than the outflow. In this sense, this source resembles NGC1377,
4C31.04 and ESO420-G13, in which the outflows are linked to faint or past jet
activity.
