On the origin of nitrogen at low metallicity

Understanding the evolution of the N/O ratio in the interstellar medium (ISM) of galaxies is essential if we are to complete our picture of the chemical evolution of galaxies at high redshift, since most observational calibrations of O/H implicitly depend upon the intrinsic N/O ratio. The observed N/O ratio, however, shows large scatter at low O/H, and is strongly dependent on galactic environment. We show that several heretofore unexplained features of the N/O distribution at low O/H can be explained by the N seen in metal-poor galaxies being mostly primary nitrogen that is returned to the ISM via pre-supernova winds from rapidly rotating massive stars (M greater than or similar to 10M(circle dot), v/v(crit) greater than or similar to 0.4). This mechanism naturally produces the observed N/O plateau at low O/H. We show that the large scatter in N/O at low O/H also arises naturally from variations in star-formation efficiency. By contrast, models in which the N and O come primarily from supernovae provide a very poor fit to the observed abundance distribution. We propose that the peculiar abundance patterns we observe at low O/H are a signature that dwarf galaxies retain little of their SN ejecta, leaving them with abundance patterns typical of winds.

Automated summary

Understanding the evolution of the N/O ratio in the interstellar medium of galaxies is crucial for a complete picture of chemical evolution at high redshift. The primary nitrogen seen in metal-poor galaxies is likely returned to the ISM via pre-supernova winds from rapidly rotating massive stars, explaining the observed N/O plateau at low O/H. Variations in star-formation efficiency also contribute to the large scatter in N/O at low O/H, suggesting that dwarf galaxies retain little of their SN ejecta, leaving them with abundance patterns typical of winds.