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Abstract

We present measurements of [S iii]λλ9069,9531 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]λλ9069,9531/[S ii]λλ6716,6731 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]/Hα at fixed [O iii]/Hβ 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.