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We present gas-phase metallicity measurements for 583 emission line galaxiesat $0.3<z<0.85$, including 388 dwarf galaxies with $log(M_{\star}/M_{\odot}) <9.5$, and explore the dependence of the metallicity on the stellar mass andstar formation properties of the galaxies. Metallicities are determined throughthe measurement of emission lines in very deep ($\sim$7 hr exposure)Keck/DEIMOS spectra taken primarily from the HALO7D survey. We measuremetallicity with three strong-line calibrations (O3H$\beta$, R23, and O3O2) forthe overall sample, as well as with the faint [Ne III]$\lambda$3869 and [OIII]$\lambda$4363 emission lines for 112 and 17 galaxies where robustdetections were possible. We construct mass-metallicity relations (MZR) foreach calibration method, finding MZRs consistent with other strong-line resultsat comparable redshift, as well as with $z\sim0$ galaxies. We quantify theintrinsic scatter in the MZR as a function of mass, finding it increases withlower stellar mass. We also measure a weak but significant correlation betweenincreased MZR scatter and higher specific star formation rate. We find a weakinfluence of SFR in the fundamental metallicity relation as well, with an SFRcoefficient of $\alpha=0.21$. Finally, we use the flux ratios of the [OII]$\lambda\lambda$3727,3729 doublet to calculate gas electron density in$\sim$1000 galaxies with $log(M_{\star}/M_{\odot}) < 10.5$ as a function ofredshift. We measure low electron densities ($n_e\sim25$ cm$^{-3}$) for $z<1$galaxies, again consistent with $z\approx0$ conditions, but measure higherdensities ($n_e\sim100$ cm$^{-3}$) at $z>1$. These results all suggest thatthere is little evolution in star-forming interstellar medium conditions from$z\sim1$ to $z=0$, confirmed with a more complete sample of low-mass galaxiesthan has previously been available in this redshift range.

Dwarf galaxies show little ISM evolution from $z\sim1$ to $z\sim0$: a spectroscopic study of metallicity, star formation, and electron density