Characterizing the average interstellar medium conditions of galaxies at z ∼ 5.6–9 with ultraviolet and optical nebular lines

Abstract

Ultraviolet (UV; rest-frame ∼1200–2000 Å) spectra provide a wealth of diagnostics to characterize fundamental galaxy properties, such as their chemical enrichment, the nature of their stellar populations, and their amount of Lyman-continuum (LyC) radiation. In this work, we leverage publicly released JWST data to construct the rest-frame UV-to-optical composite spectrum of a sample of 63 galaxies at 5.6 < z < 9, spanning a wavelength range from 1500 to 5200 Å. Based on the composite spectrum, we derive an average dust attenuation from Hβ/Hγ, an electron density cm−3 from the [O ii] doublet ratio, an electron temperature K from the [O iii] λ4363/[O iii] λ5007 ratio, and an ionization parameter from the [O iii]/[O ii] ratio. Using a direct Te method, we calculate an oxygen abundance and a carbon-to-oxygen (C/O) abundance ratio . This C/O ratio is smaller than compared to z = 0 and z = 2–4 star-forming galaxies, albeit with moderate significance. This indicates the reionization-era galaxies might be undergoing a rapid buildup of stellar mass with high specific star formation rates. A UV diagnostic based on the ratios of C iii] λλ1907, 1909/He iiλ1640 versus O iii] λ1666/He iiλ1640 suggests that the star formation is the dominant source of ionization, similar to the local extreme dwarf galaxies and z ∼ 2–4 He ii–detected galaxies. The [O iii]/[O ii] and C iv/C iii] ratios of the composite spectrum are marginally larger than the criteria used to select galaxies as LyC leakers, suggesting that some of the galaxies in our sample are strong contributors to the reionizing radiation.