Comparison of the outflow properties to their host galaxy properties. The red symbols correspond to confirmed LyC leakers, and the blue points correspond to the control sample. The upper left plot gives the scaling of Si ii velocity at 90% of the continuum (v₉₀) with the galaxy’s stellar mass (M_∗). The upper middle panel shows the variation of the Si iiv₉₀ with the star formation rate of the galaxy (SFR). The upper right panel shows the variation of the v₉₀/v_cen ratio with log(O/H) + 12. The lower left panel shows the variation of v_cen with M_∗. The bottom middle panel shows the variation of the Si ii equivalent width with SFR. The lower right panel gives the variation of the Si ii equivalent width with log(O/H) + 12. The scatter of the velocity and equivalent width depends on which host property is studied. Notably the v₉₀ is more scattered with SFR than with M_∗; and the equivalent width and SFR are uncorrelated, but the metallicity correlates with the equivalent width. This casually indicates that some host properties more strongly determine outflow properties than others. Note that we only measure LyC upper-limits for the Leitherer et al. (2016) sample (red diamonds; see the Appendix).