Kinematics of molecular gas in star-forming galaxies with large-scale
  ionised outflows
  We investigate the kinematics of the molecular gas in a sample of seven
edge-on (i>60 degrees) galaxies identified as hosting large-scale outflows of
ionised gas, using ALMA CO(1-0) observations at ~1 kpc resolution. We build on
Hogarth et al. (2021), where we find that molecular gas is more centrally
concentrated in galaxies which host winds than in control objects. We perform
full 3-dimensional kinematic modelling with multiple combinations of kinematic
components, allowing us to infer whether these objects share any similarities
in their molecular gas structure. We use modelling to pinpoint the kinematic
centre of each galaxy, in order to interpret their minor- and major-axis
position velocity diagrams (PVDs). From the PVDs, we find that the bulk of the
molecular gas in our galaxies is dynamically cold, tracing the rotation of the
stellar disc, but with minor flux asymmetries. Most notably, we find evidence
of radial gas motion in some of our minor-axis PVDs. In our highest S/N object,
we include bi-symmetric radial flow in our kinematic model, and find (via the
Bayesian Information Criterion) that the presence of radial gas motion is
strongly favoured. This may provide a mechanism by which molecular gas and star
formation are centrally concentrated, enabling the launch of massive ionised
gas winds.
