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

Published online by Cambridge University Press:  30 November 2022

Arpita Roy Open the ORCID record for Arpita Roy [Opens in a new window] ,
Mark R. Krumholz ,
Michael A. Dopita ,
Ralph S. Sutherland ,
Lisa J. Kewley  and
Alexander Heger
Arpita Roy
Affiliation:
Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy email: [email protected]
Mark R. Krumholz
Affiliation:
RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia. ASTRO 3D, Canberra, ACT 2611, Australia
Michael A. Dopita
Affiliation:
RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia.
Ralph S. Sutherland
Affiliation:
RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia. ASTRO 3D, Canberra, ACT 2611, Australia
Lisa J. Kewley
Affiliation:
RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia. ASTRO 3D, Canberra, ACT 2611, Australia
Alexander Heger
Affiliation:
ASTRO 3D, Canberra, ACT 2611, Australia School of Physics and Astronomy, Monash Centre for Astrophysics, 19 Rainforest walk, Monash University, VIC 3800, Australia.
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Abstract

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Understanding the nucleosynthetic origin of nitrogen and the evolution of the N/O ratio in the interstellar medium is crucial for a comprehensive picture of galaxy chemical evolution at high-redshift because most observational metallicity (O/H) estimates are implicitly dependent on the N/O ratio. The observed N/O at high-redshift shows an overall constancy with O/H, albeit with a large scatter. We show that these heretofore unexplained features can be explained by the pre-supernova wind yields from rotating massive stars (M≳10M⊙,ν/νcrit≳0.4). Our models naturally 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 the observed N/O at low O/H. This peculiar abundance pattern at low O/H suggests that dwarf galaxies are most likely to be devoid of SNe yields and are primarily enriched by pre-supernova wind abundances.

Keywords

stars: abundances(stars:) supernovae: generalstars: windsISM: abundancesISM: evolutiongalaxies: dwarfgalaxies: high-redshiftGalaxy: evolution
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 33 - 38
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

Footnotes

†

deceased

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