| Abstract: |
A galaxy’s metal content is a reflection of its growth and enrichment history. The balance of metal-poor inflows, metal-rich outflows, star formation, and enrichment via supernovae and stellar winds all affect the amount of metals within a galaxy. Population-level scaling relations reveal how these baryonic processes depend on properties such as stellar mass and how these dependences change over cosmic time. For example, the dependence of metallicity on stellar mass and star formation rate is much weaker at z>2.3 than it is in local galaxies, perhaps reflecting burstier star formation histories at earlier times. However, to robustly quantify this trend, we need to be able to self-consistently measure metallicity in large samples across different epochs of cosmic history. In this talk, I will discuss metallicity scaling relations at the peak of cosmic star formation (z~2.3, or Cosmic Noon) and prospects for extending this work to lower redshifts with the Prime Focus Spectrograph Galaxy Evolution survey.
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