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Understanding the nucleosynthetic origin of nitrogen and the evolution of theN/O ratio in the interstellar medium is crucial for a comprehensive picture ofgalaxy chemical evolution at high-redshift because most observationalmetallicity (O/H) estimates are implicitly dependent on the N/O ratio. Theobserved N/O at high-redshift shows an overall constancy with O/H, albeit witha large scatter. We show that these heretofore unexplained features can beexplained by the pre-supernova wind yields from rotating massive stars(M$\gtrsim 10 \, \mathrm{M}_\odot$, $v/v_{\rm{crit}} \gtrsim 0.4$). Our modelsnaturally produce the observed N/O plateau, as well as the scatter at low O/H.We find the scatter to arise from varying star formation efficiency. However,the models that have supernovae dominated yields produce a poor fit to theobserved N/O at low O/H. This peculiar abundance pattern at low O/H suggeststhat dwarf galaxies are most likely to be devoid of SNe yields and areprimarily enriched by pre-supernova wind abundances.

Can pre-supernova winds from massive stars enrich the interstellar medium with nitrogen at high redshift?