Metallicities for emission line galaxies from HALO7D

We quantify the intrinsic scatter in the MZR as a function of mass, finding it increases with lower stellar mass. We also measure a weak but significant correlation between increased MZR scatter and higher specific star formation rate (SFR). We find a weak influence of SFR in the fundamental metallicity relation as well, with an SFR coefficient of {alpha}=0.21.

Finally, we use the flux ratios of the [OII]{lambda}{lambda}3727,3729 doublet to calculate gas electron density in ~1000 galaxies with log(M_*_/M_{sun}_)<10.5 as a function of redshift. We measure low electron densities (n_e_~25cm^-3^) for z<1 galaxies, again consistent with z~0 conditions, but measure higher densities (n_e_~100cm^-3^) at z>1. These results all suggest that there is little evolution in star-forming interstellar medium conditions from z~1 to z=0, confirmed with a more complete sample of low-mass galaxies than has previously been available in this redshift range.