# Redshift Evolution of Electron Density in the Interstellar Medium at z ∼ 0–9 Uncovered with JWST/NIRSpec Spectra and Line-spread Function Determinations

Article · Yuki Isobe, Masami Ouchi, Kimihiko Nakajima, Yuichi Harikane, Yoshiaki Ono, Yi Xu, Yechi Zhang, Hiroya Umeda

- Archive id: doi:10.3847/1538-4357/acf376
- Published: 2023-10-01
- Venue: The Astrophysical Journal
- DOI: https://doi.org/10.3847/1538-4357/acf376
- Citations: 126
- Source URL: https://doi.org/10.3847/1538-4357/acf376
- Provenance: openalex

## Abstract

Abstract We present electron densities n e in the interstellar medium (ISM) of star-forming galaxies at z = 4–9 observed by the JWST/NIRSpec GLASS, Early Release Observations, and CEERS programs. We carefully evaluate the line-spread functions of the NIRSpec instrument as a function of wavelength with the calibration data of a planetary nebula taken on board, and obtain secure \[O ii \] λ λ 3726, 3729 doublet fluxes for 14 galaxies at z = 4.02–8.68 falling on the star formation main sequence with the NIRSpec high- and medium-resolution spectra. We thus derive the electron densities of singly ionized oxygen nebulae with the standard n e indicator of the \[O ii \] doublet, and find that the electron densities of the z = 4–9 galaxies are n e ≳ 300 cm −3 significantly higher than those of low- z galaxies at a given stellar mass, star formation rate (SFR), and specific SFR. Interestingly, the typical electron densities of the singly ionized nebulae increase from z = 0 to z = 1−3 and z = 4–9, which is approximated by the evolutionary relation of n e ∝ (1 + z ) p with p ∼ 1–2. Although it is not obvious that the ISM property of n e is influenced by global galaxy properties, these results may suggest that the nebula densities of high- z galaxies are generally high due to the compact morphologies of high- z galaxies evolving by r e ∝ ∼ ( 1 + z ) − 1 ( r vir ∝ (1 + z ) −1 ) for a given stellar (halo) mass whose inverse square corresponds to the p ∼ 2 evolutionary relation. The p ∼ 1−2 evolutionary relation can be explained by a combination of the compact morphology and the reduction of n e due to the high electron temperature of high- z metal-poor nebulae.

_Abstract reproduced under CC-BY (publisher license, via OpenAlex)._

Topics: [JWST & the Early Universe](https://space-kitty.com/topics/early-universe-jwst)

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