On the Pair-instability Supernova Origin of J1010+2358
Abstract
The first (Population III) stars formed only out of H and He and were likely more massive than present-day stars. Massive Population III stars in the range 140–260 M ⊙ are predicted to end their lives as pair-instability supernovae (PISNe), enriching the environment with a unique abundance pattern, with high ratios of odd to even elements. Recently, the most promising candidate for a pure descendant of a zero-metallicity massive PISN (260 M ⊙) was discovered by the LAMOST survey, the star J1010+2358. However, key elements to verify the high PISN contribution, C and Al, were missing from the analysis. To rectify this, we obtained and analyzed a high-resolution Very Large Telescope/UVES spectrum, correcting for 3D and/or non-local thermodynamic equilibrium effects. Our measurements of both C and Al give much higher values (∼1 dex) than expected from a 260 M ⊙ PISN. Furthermore, we find significant discrepancies with the previous analysis and therefore a much less pronounced odd–even pattern. Our results show that J1010+2358 cannot be a pure descendant of a 260 M ⊙ PISN. Instead, we find that the best-fit model consists of a 13 M ⊙ Population II core-collapse supernova combined with a Population III supernova. Alternative, less favored solutions (
- Publication:
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The Astrophysical Journal
- Pub Date:
- June 2024
- DOI:
- 10.3847/2041-8213/ad4b1a
- arXiv:
- arXiv:2404.19086
- Bibcode:
- 2024ApJ...968L..23S
- Keywords:
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- Galactic archaeology;
- Population III stars;
- Milky Way stellar halo;
- Early universe;
- Stellar abundances;
- Chemical abundances;
- 2178;
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- 1060;
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- Astrophysics - Solar and Stellar Astrophysics;
- Astrophysics - Astrophysics of Galaxies;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- Accepted to ApJ Letters (3rd of May 2024). 1 table, 4 figures, and Appendix