Interpretations of galaxy spectra at high redshift. \ The H_gamma/H_beta excess

TL;DR

This study models high-redshift galaxy spectra, revealing similarities to local metal-poor galaxies and suggesting remnants of pristine galaxies persist at low redshifts.

Contribution

It introduces new spectral models including shock processes and cloud fragments to interpret galaxy spectra across a wide redshift range.

Findings

High-z galaxies have preshock densities much higher than local galaxies.

Metallicities range between 7.9 and 8.55 in log(O/H)+12.

High Hg/Hb ratios indicate very high gas temperatures.

Abstract

Spectra from the cosmic dawn obtained with JWST/NIRSpec (James Webb Space Telescope near-infrared spectroscopy) in the SMACS0723 Early Release Observations are now available. Analyses carried out by different teams indicate poor to extremely low oxygen metallicities (log(O/H)+12<8.0), a characteristic feature of pristine galaxies. In this work, we present new modelling of spectra emitted by objects in the redshift range 2.16<=z<= 8.68, including their recently corrected spectra in the z = 2-9 range. The models account for both photoionisation and shock processes. Our aim is to identify similarities and differences with respect to local galaxies by searching for possible remnants of pristine galaxies among low-z objects. We analyse selected emission-line ratios in relation to elemental abundances and physical parameters. We find that the gaseous clouds within galaxies at cosmic dawn have preshock densities at least a factor of 100 higher than those in local galaxies, but comparable to those calculated for local metal-poor galaxies at 0.005<z<0.05. The metallicities log(O/H)+12 and log(Ne/H)+12 range between 7.9 and 8.55, and between 7.0 and 7.48, respectively. Uncorrected observed Hg/Hb line ratios are mostly >0.5, indicating high temperatures (>10^5K) in the emitting gas. Clear affinities are evident between the high-z galaxy spectra and those of local metal-poor galaxies at 0.005<z<0.05. However, in order to reproduce all the observed line ratios for each spectrum - including Hg/Hb values as high as ~0.8 - emission from cloud fragments was added to that from the main clouds in the pluri-cloud models. We suggest that fragments close to pristine galaxies were destroyed by events that occurred between z>6 and z<0.05, whereas some cloud remnants of pristine galaxies survived and are now found embedded, for example, at 0.005<z<0.05.