Same as Figure 6, except we plot strong line metallicities calculated using R ₂₃ McGaugh (1991). The strong line metallicities are systematically +0.2 dex larger than the T _e metallicities, but the overall distribution remains the same: our sample of metal-poor galaxies and the GRB hosts are systematically offset from the Richer & McCall (1995) luminosity–metallicity relation (dashed line), which we shift by +0.2 dex for consistency.