The efficient star-forming regions of stripped-envelope supernovae

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ID: 327242
2026
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Abstract
Abstract Massive stars ($\ge 8\, \rm {M}_{\odot }$) play a key role in shaping the interstellar medium of galaxies through stellar feedback. However, how these stars form and evolve before exploding as core-collapse supernovae (SNe) remains elusive. We compute for the first time the star-formation efficiencies (SFEs) at the locations of hydrogen-rich (H-rich) SNe and stripped-envelope SNe (SESNe) to constrain their progenitor properties. We used VLT/MUSE and ALMA observations of H α/H β and CO(2–1) emission lines to trace the components of the warm ionised gas and cold molecular gas, respectively. Both observations resolve individual H ii regions and giant molecular clouds at spatial resolutions on cloud-scales (~100 pc). This combined data allows us to compute the SFE from the star formation rate (SFR) and the molecular gas mass (Mmol) as SFE = SFR/Mmol. We find that SESNe explode in environments that are currently forming stars eight times more efficiently than those of H-rich SNe (higher SFR for SESNe with similar Mmol). On one hand, this is consistent with the scenario in which the majority of SESNe are produced from very massive stars ($\ge 20~\rm {M}_{\odot }$) if the initial mass function is top-heavy. On the other hand, most of SESN progenitor channels are formed from interacting binaries ($\le 20~\rm {M}_{\odot }$) if an increased binary system formation rate is connected with turbulences and, in turn, with the boost to SFE. Then, an increased binary fraction could explain the enhanced H α luminosities. In summary, SESNe preferentially occur in regions of intense, efficient star formation rather than simply higher gas content.
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Authors M. Solar, M. J. Michałowski, J. Nadolny, L. Galbany, J. P. Anderson, J. Sollerman, T. Pessi, E. Zapartas, B. Šlaus, J. Alexander, O. Ryzhov, J. Hjorth, C. Jiménez-Palau, P. Nowaczyk, D. Somawanshi, A. Leśniewska
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Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1615
URL
https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stag1615/70852610/stag1615.pdf
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