various observations mentioned above, potentially due to as yet unresolved differences in the metallicity across the galaxy [@obs_paper]. We have removed LGRB 020819B from our combined sample due to the revised host galaxy association of [@Perley020819B] and the poor metallicity constraint on the now correctly associated host galaxy.

### Host Masses

While neither the [@stats_paper] or [@xshooter_survey] provide host galaxy masses or even have the required IR observations required for such mass measurements, the [@Perley_shoals_masses] SHOALS sample does. Unfortunately the [@Perley_shoals_masses] SHOALS sample has a paucity of objects at low redshift (only 3 at z $<$ 0.5) so we supplement it with the [@Svensson] population which is predominately at z $<$ 1 and also has mass values based on deep IR observations. Two objects overlap between the samples (LGRBs 060218 and 080319B) whose log masses differ by 0.24 and -0.43 between the [@Svensson] and [@Perley_shoals_masses] estimates respectively. In our combined sample the duplication has been removed and the [@Perley_shoals_masses] values used.

Metallicity Determination {#Metallicity_Determination}
-------------------------

Here we use metallicities determined via the R$_{23}$ diagnostic in the [@KobulnickyKewley] (KK04) scale. The R$_{23}$ method is the primary metallicity diagnostic for galaxies at $z>0.3$ (especially those where the faint \[O III\] 4363 [Å]{} 