Dependence of the Lyα escape fraction on EW(Lyα) (top left), M_UV (top right), [O III]/[O II] ratio (O32) (bottom left) and EW(Hβ) (bottom right). The correlations follow the same convention as in Fig. 6. Unsurprisingly, we find that f_esc(Lyα) correlates strongly with EW(Lyα). We also note that UV-faint galaxies show higher f_esc(Lyα), although this could be attributed purely to the flux limited nature of our spectroscopic survey. We do not find strong correlations between f_esc(Lyα) and O32 or Hβ strength, although as previously noted we do find that our faint LAEs on average show high O32 ratios and Hβ line strengths.