The Detection of [O iii] λ4363 in a Lensed, Dwarf Galaxy at z = 2.59: Testing Metallicity Indicators and Scaling Relations at High Redshift and Low Mass*

Abstract

We present Keck/MOSFIRE (Multi-Object Spectrometer for InfraRed Exploration) and Keck/LRIS (Low Resolution Imaging Spectrometer) spectroscopy of A1689-217, a lensed (magnification ∼7.9), star-forming (SFR ∼ 16 M ☉ yr −1 ), dwarf (log( M * / M ☉ ) = 8.07–8.59) Ly α emitter (EW 0 ∼ 138 Å) at z  = 2.5918. Dwarf galaxies similar to A1689-217 are common at high redshift and likely responsible for reionization, yet few have been studied with detailed spectroscopy. We report a 4.2 σ detection of the electron-temperature-sensitive [O iii ] λ 4363 emission line and use this line to directly measure an oxygen abundance of 12 + log(O/H) = 8.06 ± 0.12 (∼1/4 Z ☉ ). A1689-217 is the lowest-mass galaxy at z  > 2 with an [O iii ] λ 4363 detection. Using the rest-optical emission lines, we measure A1689-217’s other nebular conditions, including electron temperature ( T e ([O iii ]) ∼ 14,000 K), electron density ( n e  ∼ 220 cm −3 ), and reddening (  ∼ 0.39). We study relations between strong-line ratios and direct metallicities with A1689-217 and other galaxies with [O iii ] λ 4363 detections at z  ∼ 0–3.1, showing that the locally calibrated, oxygen-based, strong-line relations are consistent from z  ∼ 0 to 3.1. We also show additional evidence that the O 32 versus R 23 excitation diagram can be utilized as a redshift-invariant, direct-metallicity-based, oxygen abundance diagnostic out to z  ∼ 3.1. From this excitation diagram and the strong-line ratio–metallicity plots, we observe that the ionization parameter at fixed O/H is consistent with no redshift evolution. Although A1689-217 is metal-rich for its M * and star formation rate, we find it to be consistent within the large scatter of the low-mass end of the fundamental metallicity relation.