Stellar-mass black holes in the Hyades star cluster?

Astrophysical models of binary-black hole mergers in the universe require a significant fraction of stellar-mass black holes (BHs) to receive negligible natal kicks to explain the gravitational wave detections. This implies that BHs should be retained even in open clusters with low escape velocities...

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Autores: Torniamenti, Stefano, Gieles, Mark, Penoyre, Zephyr, Jerabkova, T., Wang, Long, Anders, Friedrich
Tipo de documento: artigo
Estado:Versão publicada
Data de publicação:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositório:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/339742
Acesso em linha:http://hdl.handle.net/10261/339742
Access Level:Acceso aberto
Palavra-chave:Black hole physics
Methods: numerical
Binaries: general
Stars: kinematics and dynamics
Star clusters: individual: Hyades cluster
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dc.title.none.fl_str_mv Stellar-mass black holes in the Hyades star cluster?
title Stellar-mass black holes in the Hyades star cluster?
spellingShingle Stellar-mass black holes in the Hyades star cluster?
Torniamenti, Stefano
Black hole physics
Methods: numerical
Binaries: general
Stars: kinematics and dynamics
Star clusters: individual: Hyades cluster
title_short Stellar-mass black holes in the Hyades star cluster?
title_full Stellar-mass black holes in the Hyades star cluster?
title_fullStr Stellar-mass black holes in the Hyades star cluster?
title_full_unstemmed Stellar-mass black holes in the Hyades star cluster?
title_sort Stellar-mass black holes in the Hyades star cluster?
dc.creator.none.fl_str_mv Torniamenti, Stefano
Gieles, Mark
Penoyre, Zephyr
Jerabkova, T.
Wang, Long
Anders, Friedrich
author Torniamenti, Stefano
author_facet Torniamenti, Stefano
Gieles, Mark
Penoyre, Zephyr
Jerabkova, T.
Wang, Long
Anders, Friedrich
author_role author
author2 Gieles, Mark
Penoyre, Zephyr
Jerabkova, T.
Wang, Long
Anders, Friedrich
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
European Research Council
Ministerio de Ciencia, Innovación y Universidades (España)
Agencia Estatal de Investigación (España)
Generalitat de Catalunya
Sun Yat-sen University
National Natural Science Foundation of China
dc.subject.none.fl_str_mv Black hole physics
Methods: numerical
Binaries: general
Stars: kinematics and dynamics
Star clusters: individual: Hyades cluster
topic Black hole physics
Methods: numerical
Binaries: general
Stars: kinematics and dynamics
Star clusters: individual: Hyades cluster
description Astrophysical models of binary-black hole mergers in the universe require a significant fraction of stellar-mass black holes (BHs) to receive negligible natal kicks to explain the gravitational wave detections. This implies that BHs should be retained even in open clusters with low escape velocities (1 km s−1). We search for signatures of the presence of BHs in the nearest open cluster to the Sun – the Hyades – by comparing density profiles of direct N-body models to data from Gaia. The observations are best reproduced by models with 2–3 BHs at present. Models that never possessed BHs have an half-mass radius ∼ 30 per cent smaller than the observed value, while those where the last BHs were ejected recently (150 Myr ago) can still reproduce the density profile. In 50 per cent of the models hosting BHs, we find BHs with stellar companion(s). Their period distribution peaks at ∼103 yr, making them unlikely to be found through velocity variations. We look for potential BH companions through large Gaia astrometric and spectroscopic errors, identifying 56 binary candidates – none of which is consistent with a massive compact companion. Models with 2–3 BHs have an elevated central velocity dispersion, but observations cannot yet discriminate. We conclude that the present-day structure of the Hyades requires a significant fraction of BHs to receive natal kicks smaller than the escape velocity of ∼ 3 km s−1 at the time of BH formation and that the nearest BHs to the Sun are in, or near, Hyades.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/339742
url http://hdl.handle.net/10261/339742
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The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stad1925
https://doi.org/10.1093/mnras/stad1925
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dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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spelling Stellar-mass black holes in the Hyades star cluster?Torniamenti, StefanoGieles, MarkPenoyre, ZephyrJerabkova, T.Wang, LongAnders, FriedrichBlack hole physicsMethods: numericalBinaries: generalStars: kinematics and dynamicsStar clusters: individual: Hyades clusterAstrophysical models of binary-black hole mergers in the universe require a significant fraction of stellar-mass black holes (BHs) to receive negligible natal kicks to explain the gravitational wave detections. This implies that BHs should be retained even in open clusters with low escape velocities (1 km s−1). We search for signatures of the presence of BHs in the nearest open cluster to the Sun – the Hyades – by comparing density profiles of direct N-body models to data from Gaia. The observations are best reproduced by models with 2–3 BHs at present. Models that never possessed BHs have an half-mass radius ∼ 30 per cent smaller than the observed value, while those where the last BHs were ejected recently (150 Myr ago) can still reproduce the density profile. In 50 per cent of the models hosting BHs, we find BHs with stellar companion(s). Their period distribution peaks at ∼103 yr, making them unlikely to be found through velocity variations. We look for potential BH companions through large Gaia astrometric and spectroscopic errors, identifying 56 binary candidates – none of which is consistent with a massive compact companion. Models with 2–3 BHs have an elevated central velocity dispersion, but observations cannot yet discriminate. We conclude that the present-day structure of the Hyades requires a significant fraction of BHs to receive natal kicks smaller than the escape velocity of ∼ 3 km s−1 at the time of BH formation and that the nearest BHs to the Sun are in, or near, Hyades.ST acknowledges financial support from the European Research Council for the ERC Consolidator grant DEMOBLACK, under contract no. 770017. MG acknowledges support from the Ministry of Science and Innovation (EUR2020-112157, PID2021-125485NB-C22, CEX2019-000918-M funded by MCIN/AEI/10.13039/501100011033) and from AGAUR (SGR-2021-01069). ZP acknowledges that this project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101002511 - VEGA P). LW thanks the support from the one-hundred-talent project of Sun Yat-sen University, the Fundamental Research Funds for the Central Universities, Sun Yat-sen University (22hytd09), and the National Natural Science Foundation of China through grant 12073090 and 12233013. FA acknowledges financial support from MCIN/AEI/10.13039/501100011033 through grants IJC2019-04862-I and RYC2021-031638-I (the latter co-funded by European Union NextGenerationEU/PRTR).Peer reviewedOxford University PressEuropean CommissionEuropean Research CouncilMinisterio de Ciencia, Innovación y Universidades (España)Agencia Estatal de Investigación (España)Generalitat de CatalunyaSun Yat-sen UniversityNational Natural Science Foundation of China202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/339742reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/770017info:eu-repo/grantAgreement/AEI//EUR2020-112157info:eu-repo/grantAgreement/AEI//PID2021-125485NB-C22info:eu-repo/grantAgreement/AEI//CEX2019-000918-Minfo:eu-repo/grantAgreement/EC/H2020/101002511info:eu-repo/grantAgreement/AEI//IJC2019-04862-Iinfo:eu-repo/grantAgreement/AEI//RYC2021-031638-IThe underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/stad1925https://doi.org/10.1093/mnras/stad1925Noinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3397422026-05-22T06:33:51Z
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