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We investigate the kinematics of the molecular gas in a sample of sevenedge-on (i>60{\deg}) galaxies identified as hosting large-scale outflows ofionised gas, using ALMA CO(1-0) observations at ~ 1kpc resolution. We build onHogarth et al. (2021; H21), where we find that molecular gas is more centrallyconcentrated in galaxies which host winds than in control objects. We performfull 3-dimensional kinematic modelling with multiple combinations of kinematiccomponents, allowing us to infer whether these objects share any similaritiesin their molecular gas structure. We use modelling to pinpoint the kinematiccentre of each galaxy, in order to interpret their minor- and major-axisposition velocity diagrams (PVDs). From the PVDs, we find that the bulk of themolecular gas in our galaxies is dynamically cold, tracing the rotation curvespredicted by our symmetric, rotation-dominated models, but with minor fluxasymmetries. Most notably, we find evidence of radial gas motion in a subset ofour objects, which demonstrate a characteristic "twisting" in their minor-axisPVDs generally associated with gas flow along the plane of a galaxy. In ourhighest S/N object, we include bi-symmetric radial flow in our kinematic model,and find (via the Bayesian Information Criterion) that the presence of radialgas motion is strongly favoured. This may provide one mechanism by whichmolecular gas and star formation are centrally concentrated, enabling thelaunch of massive ionised gas winds. However, in the remainder of our sample,we do not observe evidence that gas is being driven radially, once againemphasising the variety of physical processes that may be powering the outflowsin these objects, as originally noted in H21.

Kinematics of molecular gas in star-forming galaxies with large-scale ionised outflows