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Galactic fountains driven by star formation result in a variety of kinematicstructures such as ionised winds and thick gas disks, both of which manifest ascomplex emission line profiles that can be parametrised by multiple Gaussiancomponents. We use integral field spectroscopy (IFS) from the SAMI GalaxySurvey to spectrally resolve these features, traced by broad H$\alpha$components, and distinguish them from the star-forming thin disk, traced bynarrow components, in 3068 galaxies in the local Universe. Using a matchedsample analysis technique, we demonstrate that the presence of complex emissionline profiles in star-forming galaxies is most strongly correlated with theglobal star formation rate (SFR) surface density of the host galaxy measuredwithin $1R_{\rm e}$ ($\Sigma_{{\rm SFR},R_{\rm e}}$), even when controlling forboth observational biases, including inclination, amplitude-to-noise andangular scale, and sample biases in parameters such as stellar mass and SFR.Leveraging the spatially resolved nature of the dataset, we determine that thepresence of complex emission line profiles within individual spaxels is drivennot only by the local $\Sigma_{\rm SFR}$, but by the $\Sigma_{{\rm SFR},R_{\rme}}$ of the host galaxy. We also parametrise the clumpiness of the SFR withinindividual galaxies, and find that $\Sigma_{{\rm SFR},R_{\rm e}}$ is a strongerpredictor of the presence of complex emission line profiles than clumpiness. Weconclude that, with a careful treatment of observational effects, it ispossible to identify structures traced by complex emission line profiles,including winds and thick ionised gas disks, at the spatial and spectralresolution of SAMI using the Gaussian decomposition technique.

The SAMI Galaxy Survey: $\Sigma_{\rm SFR}$ drives the presence of complex emission line profiles in star-forming galaxies