We infer the intrinsic ionised gas kinematics for 383 star-forming galaxies across a range of integrated star-formation rates ( SFR \in [ 10 ^ { -3 } , 10 ^ { 2 } ] M _ { \odot } yr ^ { -1 } ) at z \lesssim 0.1 using a consistent 3D forward-modelling technique .
The total sample is a combination of galaxies from the SAMI Galaxy Survey and DYNAMO survey .
For typical low- z galaxies taken from the SAMI Galaxy Survey , we find the vertical velocity dispersion ( \sigma _ { v,z } ) to be positively correlated with measures of star-formation rate , stellar mass , H i gas mass , and rotational velocity .
The greatest correlation is with star-formation rate surface density ( \Sigma _ { \text { SFR } } ) .
Using the total sample , we find \sigma _ { v,z } increases slowly as a function of integrated star-formation rate in the range SFR \in [ 10 ^ { -3 } , 1 ] M _ { \odot } yr ^ { -1 } from 17 \pm 3 km s ^ { -1 } to 24 \pm 5 km s ^ { -1 } followed by a steeper increase up to \sigma _ { v,z } \sim 80 km s ^ { -1 } for SFR \gtrsim 1 M _ { \odot } yr ^ { -1 } .
This is consistent with recent theoretical models that suggest a \sigma _ { v,z } floor driven by star-formation feedback processes with an upturn in \sigma _ { v,z } at higher SFR driven by gravitational transport of gas through the disc .