Abstract We infer the intrinsic ionised gas kinematics for 383 star-forming galaxies across a range of integrated star-formation rates (SFR ∈ [10−3, 102] M⊙ yr−1) at z ≲ 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 (σv, 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 (ΣSFR). Using the total sample, we find σv, z increases slowly as a function of integrated star-formation rate in the range SFR ∈ [10−3, 1] M⊙ yr−1 from 17 ± 3 km s−1 to 24 ± 5 km s−1 followed by a steeper increase up to σv, z ∼80 km s−1 for SFR ≳ 1 M⊙ yr−1. This is consistent with recent theoretical models that suggest a σv, z floor driven by star-formation feedback processes with an upturn in σv, z at higher SFR driven by gravitational transport of gas through the disc.