The Mass-Metallicity Relation at z=8: Direct-Method Metallicity Constraints and Near-Future Prospects

TL;DR

This paper measures the metallicity of galaxies at redshifts 7 to 9 using direct methods, compares results with models, and discusses future prospects with ALMA and JWST for studying early galaxy evolution.

Contribution

It provides the first direct T_e-based metallicity estimates for high-redshift galaxies and evaluates future observational strategies to improve these measurements.

Findings

Average metallicity 12+log(O/H) ≈ 7.9 at z≈8

Observed metallicity evolution of 0.9±0.5 dex from z≈8 to 0

Future observations can achieve 0.1-0.2 dex precision with ALMA and JWST

Abstract

Physical properties of galaxies at z>7 are of interest for understanding both the early phases of star formation and the process of cosmic reionization. Chemical abundance measurements offer valuable information on the integrated star formation history, and hence ionizing photon production, as well as the rapid gas accretion expected at such high redshifts. We use reported measurements of [O III] 88$\mu$m emission and star formation rate to estimate gas-phase oxygen abundances in five galaxies at z=7.1-9.1 using the direct T_e method. We find typical abundances 12+log(O/H) = 7.9 ($\sim$0.2 times the solar value) and an evolution of 0.9$\pm$0.5 dex in oxygen abundance at fixed stellar mass from z$\simeq$8 to 0. These results are compatible with theoretical predictions, albeit with large (conservative) uncertainties in both mass and metallicity. We assess both statistical and systematic uncertainties to identify promising means of improvement with the Atacama Large Millimeter Array (ALMA) and the James Webb Space Telescope (JWST). In particular we highlight [O III] 52$\mu$m as a valuable feature for robust metallicity measurements. Precision of 0.1-0.2 dex in T_e-based O/H abundance can be reasonably achieved for galaxies at z$\approx$5-8 by combining [O III] 52$\mu$m with rest-frame optical strong lines. It will also be possible to probe gas mixing and mergers via resolved T_e-based abundances on kpc scales. With ALMA and JWST, direct metallicity measurements will thus be remarkably accessible in the reionization epoch.