Discovery of new N-emitters over a wide redshift range

TL;DR

This study systematically identifies 45 galaxies with nitrogen UV emission lines across a wide redshift range, revealing their diverse properties, high N/O ratios, and evolution with redshift, thus providing new insights into their nature.

Contribution

It presents the first large, diverse sample of N-emitters from JWST data, expanding the known population and offering new constraints on their chemical abundances and evolution.

Findings

N-emitters found from redshift 3 to 11 with diverse properties.

All N-emitters show supersolar N/O ratios.

The fraction of N-emitters increases with redshift.

Abstract

JWST observations have revealed rare galaxies with UV spectra exhibiting intense lines of nitrogen, indicative of super-solar N/O abundances at low metallicity. To better understand these enigmatic objects and provide new constraints on proposed scenarios, we have undertaken a systematic search for galaxies with UV emission lines of nitrogen. Using public JWST NIRSpec data, we have identified 45 N-emitters with robust NIII] or NIV] detections, including 4 previously known objects. We find N-emitters from redshift $z\sim 3-11$ among a broad diversity of galaxies, in terms of morphology, UV magnitude, stellar mass, SFR, metallicity, and rest-optical line strengths. The UV nitrogen lines show typical equivalent widths between $\sim 5-50$ \AA. Carbon lines are generally fainter than the N lines. Using strong line calibrations established at high-redshift, we find metallicities $12+log(O/H)\sim 7.15-8.5$, including thus also high metallicities. The H$\beta$ equivalent width of N-emitters varies strongly, and sources with low EWs show clear signs of a Balmer break, indicative of composite stellar populations combining both young (< 10 Myr) stars responsible of the UV emission lines and an older population contributing to the rest-optical spectrum. Supersolar N/O ratios are found in all N-emitters. C/O abundances are comparable to those of galaxies at the same metallicity, and all N-emitters show high N/C ratios or lower limits ($\log(N/C) > 0.5$), independently of metallicity. The observed abundance ratios are compatible with ejecta from H-burning and do not show signs of Carbon enhancements, even at higher metallicities. Finally, we find that the fraction of N-emitters increases with redshift, and we quantify this evolution. Our study increases the sample of known N-emitters by a factor $\sim 3$, reveals a diversity of properties among N-emitters, and provides new constraints on their nature.