An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326

[Context] Understanding the most metal-poor objects is key to interpreting the nature of the first stars. HE 1327-2326 (HE 1327), with metallicity [Fe/H] = −5.2, is one of the most metal-poor stars detected and a candidate to be the offspring of the first stars. Numerous efforts have been made to re...

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Detalles Bibliográficos
Autores: Gil Pons, Pilar, Campbell, S. W., Doherty, C. L., Lugaro, Maria
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/411078
Acceso en línea:http://hdl.handle.net/10261/411078
https://api.elsevier.com/content/abstract/scopus_id/105022076915
Access Level:acceso abierto
Palabra clave:Stars: abundances
Stars: AGB and post-AGB
Stars: individual: HE 1327-2326
Stars: peculiar
id ES_4de4910b00103b5cde4e7fecfb77ffaf
oai_identifier_str oai:digital.csic.es:10261/411078
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
title An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
spellingShingle An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
Gil Pons, Pilar
Stars: abundances
Stars: AGB and post-AGB
Stars: individual: HE 1327-2326
Stars: peculiar
title_short An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
title_full An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
title_fullStr An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
title_full_unstemmed An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
title_sort An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326
dc.creator.none.fl_str_mv Gil Pons, Pilar
Campbell, S. W.
Doherty, C. L.
Lugaro, Maria
author Gil Pons, Pilar
author_facet Gil Pons, Pilar
Campbell, S. W.
Doherty, C. L.
Lugaro, Maria
author_role author
author2 Campbell, S. W.
Doherty, C. L.
Lugaro, Maria
author2_role author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Agencia Estatal de Investigación (España)
Generalitat de Catalunya
German Research Foundation
Australian Research Council
Hungarian Academy of Sciences
National Collaborative Research Infrastructure Strategy (Australia)
Campbell, S. W. [0000-0001-5298-0694]
Lugaro, Maria [0000-0002-6972-3958]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Stars: abundances
Stars: AGB and post-AGB
Stars: individual: HE 1327-2326
Stars: peculiar
topic Stars: abundances
Stars: AGB and post-AGB
Stars: individual: HE 1327-2326
Stars: peculiar
description [Context] Understanding the most metal-poor objects is key to interpreting the nature of the first stars. HE 1327-2326 (HE 1327), with metallicity [Fe/H] = −5.2, is one of the most metal-poor stars detected and a candidate to be the offspring of the first stars. Numerous efforts have been made to reproduce its abundance pattern, especially with high-mass stars undergoing supernova (SN) explosions. However, no model satisfactorily explains its entire surface chemical composition. Aims. The characteristic high CNO pattern with [N/Fe] > [C/Fe] > [O/Fe], the light element ‘slide’ (between Na and Si), and the presence of Sr and Ba in HE 1327 is reminiscent of asymptotic giant branch (AGB) stars that undergo third dredge-up, hot-bottom burning, and s-processing – suggesting that these stars were the source of the chemistry of the star. We tested this hypothesis.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/411078
https://api.elsevier.com/content/abstract/scopus_id/105022076915
url http://hdl.handle.net/10261/411078
https://api.elsevier.com/content/abstract/scopus_id/105022076915
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-109363GB-I00
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2023-148661NB-I00
https://doi.org/10.1051/0004-6361/202556363
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
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repository.name.fl_str_mv
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spelling An asymptotic giant branch star as the source of the abundance pattern of hyper-metal-poor star HE 1327-2326Gil Pons, PilarCampbell, S. W.Doherty, C. L.Lugaro, MariaStars: abundancesStars: AGB and post-AGBStars: individual: HE 1327-2326Stars: peculiar[Context] Understanding the most metal-poor objects is key to interpreting the nature of the first stars. HE 1327-2326 (HE 1327), with metallicity [Fe/H] = −5.2, is one of the most metal-poor stars detected and a candidate to be the offspring of the first stars. Numerous efforts have been made to reproduce its abundance pattern, especially with high-mass stars undergoing supernova (SN) explosions. However, no model satisfactorily explains its entire surface chemical composition. Aims. The characteristic high CNO pattern with [N/Fe] > [C/Fe] > [O/Fe], the light element ‘slide’ (between Na and Si), and the presence of Sr and Ba in HE 1327 is reminiscent of asymptotic giant branch (AGB) stars that undergo third dredge-up, hot-bottom burning, and s-processing – suggesting that these stars were the source of the chemistry of the star. We tested this hypothesis.[Methods] We assumed that, where HE 1327 formed, the interstellar medium was well mixed, and adopted an initial stellar composition based on the observed chemical evolution of the early Universe. Zinc, which is enhanced in HE 1327, is well matched by this initial composition, as are the α-elements. We calculated models of hyper-metal-poor AGB stars and compared the predicted chemical yields to the observed chemical pattern of HE 1327.[Resulst] We find our 3 M<inf>⊙</inf> models match 13 of the 14 measured elements in HE1327, more than any model thus far. They are also consistent with the seven elements with known upper limits. The only discrepancy is oxygen, which is underproduced by 0.5 − 1.0 dex. For elements up to Zn, the match is comparable to that of the best-fitting, finely tuned SN models. Unlike the SN models, the AGB models also match Sr and Ba. We stress that the AGB scenario requires only standard stellar evolution, without invoking exotic scenarios. Our model predicts high abundances of P and Pb; thus, observations of these elements would be useful in testing the AGB scenario.[Conclusions] We propose that HE 1327 is the oldest known object that shows nucleosynthetic evidence of the first AGB stars. With lifetimes as short as 200 Myr, these stars may have formed and polluted the Universe very early on. Recent Pop III star formation simulations support this hypothesis, and their strong nitrogen production is qualitatively consistent with recent JWST observations showing high N/O ratios just 440 Myr after the Big Bang. Importantly, our results also suggest that the interstellar medium experienced some degree of homogeneity and mixing at these early epochs.This work was supported by the Spanish projects PID2019-109363GB-100, PID2023-148661NB-I00, by the AGAUR/Generalitat de Catalunya grant SGR-386/2021, and by the Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. SWC acknowledges federal funding from the Australian Research Council through a Future Fellowship (FT160100046) and Discovery Projects (DP190102431 & DP210101299). ML acknowledges funding from the LP2023-10 Lendulet grant of the Hungarian Academy of Sciences. Parts of this research was supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research was supported by use of the Nectar Research Cloud, a collaborative Australian research platform supported by the National Collaborative Research Infrastructure Strategy (NCRIS).Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)Agencia Estatal de Investigación (España)Generalitat de CatalunyaGerman Research FoundationAustralian Research CouncilHungarian Academy of SciencesNational Collaborative Research Infrastructure Strategy (Australia)Campbell, S. W. [0000-0001-5298-0694]Lugaro, Maria [0000-0002-6972-3958]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/411078https://api.elsevier.com/content/abstract/scopus_id/105022076915reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-109363GB-I00info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2023-148661NB-I00https://doi.org/10.1051/0004-6361/202556363Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4110782026-05-22T06:33:51Z
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