$M_{\star}$–$Z$–${\rm SFR}$ relation evolves with redshift.'
author:
- |
    Jonathan S. Brown,$^{1}$[^1] Paul Martini,$^{1,2}$ and Brett H. Andrews$^{3}$\
    $^{1}$Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA\
    $^{2}$Center for Cosmology and Astro-Particle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA\
    $^{3}$PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA
bibliography:
- 'calib.bib'
date: 'Accepted XXX. Received YYY; in original form ZZZ'
title: A Recalibration of Strong Line Oxygen Abundance Diagnostics via the Direct Method and Implications for the High Redshift Universe
---

\[firstpage\]

galaxies: active – galaxies: abundances – galaxies: evolution – galaxies: ISM – ISM: abundances

Introduction {#sec:intro}
============

Galaxies are continually undergoing chemical enrichment. Gas is condensed into stars, processed into heavier elements, and returned to the interstellar medium. This gas, enriched by the products of stellar nucleosynthesis and/or supernova ejecta, is reincorporated into new generations of stars, where it is enriched once again. A galaxy may also accrete low metallicity gas from the intergalactic medium, which both dilutes the ISM and provides fuel for a new generation of stars to form. This interplay between star formation, chemical enrichment, 