Evolution of Gas-phase Metallicity and Dust Attenuation from z ~ 14 to Cosmic Noon
The chemical enrichment state and dust attenuation of galaxies, their redshift evolution, and their dependence on stellar mass, star-formation rate, and environment are some of the most readily testable predictions of theoretical models of galaxy formation. The complex interplay between the processes that regulate chemical enrichment, including mergers, accretion, star-formation, and feedback-driven outflows is expected to become simpler at early times and easier to model. Hence, high-z constraints on the gas-phase metallicity and dust attenuation of galaxies are crucial for informing the theoretical models. I will present these measurements based on a large compilation of NIRSpec data, containing more than 2000 galaxies at 3 < z < 14. I will highlight established correlations, including the mass-metallicity relation and its redshift evolution, as well as the fundamental metallicity relation. Moreover, I will highlight new findings concerning the cosmic buildup of interstellar dust. The revolutionary combination of depth, wavelength coverage, and spatial resolution afforded by JWST has brought morphological and chemical analysis to the forefront of high-z studies. However, we are already facing the limitations of space telescopes: i) their limited spatial resolution, and ii) the high exposure times required to acquire deep high-spectral-resolution spectra. I will discuss these in light of the upcoming class of ELTs, highlighting the improvements expected in the coming decade.
