The MOSDEF Survey: [S iii] as a New Probe of Evolving Interstellar Medium Conditions*

Abstract

We present measurements of [S  iii ] λλ 9069,9531 for a sample of z  ∼ 1.5 star-forming galaxies, the first representative sample with measurements of these lines at z  ≳ 0.1. We employ the line ratio S 32  ≡ [S  iii ] λλ 9069,9531/[S  ii ] λλ 6716,6731 as a novel probe of evolving interstellar medium (ISM) conditions. Since this ratio includes the low-ionization line [S  ii ], it is crucial that the effects of diffuse ionized gas (DIG) on emission-line ratios be accounted for in z  ∼ 0 galaxy spectra, or else that comparisons be made to samples of local H  ii   regions in which DIG emission is not present. We find that S 32 decreases with increasing stellar mass at both z  ∼ 1.5 and z  ∼ 0, but with a shallow slope suggesting S 32 has a weak dependence on metallicity, in contrast with [O  iii ]/[O  ii ] that displays a strong metallicity dependence. As a result, S 32 only mildly evolves with redshift at fixed stellar mass. The z  ∼ 1.5 sample is systematically offset toward lower S 32 and higher [S  ii ]/H α at fixed [O  iii ]/H β relative to z  = 0 H  ii   regions. We find that such trends can be explained by a scenario in which the ionizing spectrum is harder at fixed O/H with increasing redshift, but are inconsistent with an increase in ionization parameter at fixed O/H. This analysis demonstrates the advantages of expanding beyond the strongest rest-optical lines for evolutionary studies, and the particular utility of [S  iii ] for characterizing evolving ISM conditions and stellar compositions. These measurements provide a basis for estimating [S  iii ] line strengths for high-redshift galaxies, a line that the James Webb Space Telescope will measure out to z  ∼ 5.5.