On the Pair-Instability Supernova origin of J1010+2358
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2024
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| author | Skúladóttir, Ása Koutsouridou, Ioanna Vanni, Irene Amarsi, Anish M. Lucchesi, Romain Salvadori, Stefania Aguado, David |
| author_facet | Skúladóttir, Ása Koutsouridou, Ioanna Vanni, Irene Amarsi, Anish M. Lucchesi, Romain Salvadori, Stefania Aguado, David |
| contents | The first (Pop III) stars formed only out of H and He and were likely more massive than present-day stars. Massive Pop III stars in the range 140-260 M$_\odot$ 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$_{\odot}$) was discovered by the LAMOST survey, the star J1010+2358. However, the 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 VLT/UVES spectrum, correcting for 3D and/or non-LTE effects. Our measurements of both C and Al give much higher values (~1 dex) than expected from a 260 M$_{\odot}$ PISN. Furthermore, we find significant discrepancies with the previous analysis, and therefore a much less pronounced odd-even pattern. Thus, we show that J1010+2358 cannot be a pure descendant of a 260 M$_{\odot}$ PISN. Instead, we find that the best fit model consists of a 13 M$_{\odot}$ Pop II core-collapse supernova combined with a Pop III supernova. Alternative, less favoured solutions $(χ^2/χ^2_{\rm best}\approx2.3)$ include a 50% contribution from a 260 M$_{\odot}$ PISN, or a 40% contribution from a Pop III type Ia supernova. Ultimately, J1010+2358 is certainly a unique star giving insights into the earliest chemical enrichment, however, this star is not a pure PISN descendant. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2404_19086 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | On the Pair-Instability Supernova origin of J1010+2358 Skúladóttir, Ása Koutsouridou, Ioanna Vanni, Irene Amarsi, Anish M. Lucchesi, Romain Salvadori, Stefania Aguado, David Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena The first (Pop III) stars formed only out of H and He and were likely more massive than present-day stars. Massive Pop III stars in the range 140-260 M$_\odot$ 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$_{\odot}$) was discovered by the LAMOST survey, the star J1010+2358. However, the 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 VLT/UVES spectrum, correcting for 3D and/or non-LTE effects. Our measurements of both C and Al give much higher values (~1 dex) than expected from a 260 M$_{\odot}$ PISN. Furthermore, we find significant discrepancies with the previous analysis, and therefore a much less pronounced odd-even pattern. Thus, we show that J1010+2358 cannot be a pure descendant of a 260 M$_{\odot}$ PISN. Instead, we find that the best fit model consists of a 13 M$_{\odot}$ Pop II core-collapse supernova combined with a Pop III supernova. Alternative, less favoured solutions $(χ^2/χ^2_{\rm best}\approx2.3)$ include a 50% contribution from a 260 M$_{\odot}$ PISN, or a 40% contribution from a Pop III type Ia supernova. Ultimately, J1010+2358 is certainly a unique star giving insights into the earliest chemical enrichment, however, this star is not a pure PISN descendant. |
| title | On the Pair-Instability Supernova origin of J1010+2358 |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2404.19086 |