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In order to determine the causes of kinematic asymmetry in the H$\alpha$ gasin the SAMI Galaxy Survey sample, we investigate the comparative influences ofenvironment and intrinsic properties of galaxies on perturbation. We usespatially resolved H$\alpha$ velocity fields from the SAMI Galaxy Survey toquantify kinematic asymmetry ($\overline{v_{asym}}$) in nearby galaxies andenvironmental and stellar mass data from the GAMA survey.  {We find that local environment, measured as distance to nearest neighbour,is inversely correlated with kinematic asymmetry for galaxies with$\mathrm{\log(M_*/M_\odot)}>10.0$, but there is no significant correlation forgalaxies with $\mathrm{\log(M_*/M_\odot)}<10.0$. Moreover, low mass galaxies($\mathrm{\log(M_*/M_\odot)}<9.0$) have greater kinematic asymmetry at allseparations, suggesting a different physical source of asymmetry is importantin low mass galaxies.}  We propose that secular effects derived from gas fraction and gas mass may bethe primary causes of asymmetry in low mass galaxies. High gas fraction islinked to high $\frac{\sigma_{m}}{V}$ (where $\sigma_m$ is H$\alpha$ velocitydispersion and $V$ the rotation velocity), which is strongly correlated with$\overline{v_{asym}}$, and galaxies with $\log(M_*/M_\odot)<9.0$ have offset$\overline{\frac{\sigma_{m}}{V}}$ from the rest of the sample. Further,asymmetry as a fraction of dispersion decreases for galaxies with$\log(M_*/M_\odot)<9.0$. Gas mass and asymmetry are also inversely correlatedin our sample. We propose that low gas masses in dwarf galaxies may lead toasymmetric distribution of gas clouds, leading to increased relativeturbulence.

The SAMI Galaxy Survey: gas content and interaction as the drivers of kinematic asymmetry