Baryon-induced collapse of dark matter cores into supermassive black holes

Autores
Argüelles, Carlos Raúl; Rueda, Jorge; Ruffini, Remo
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Nonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c² fermion, which leads to ∼10⁷M⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρb and velocity vb inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 10⁷M⊙ SMBH, for Qb = pb/vb³= 0.125M⊙ /(100 km s pc)³ , forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 10⁷M⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈10⁷–10⁸M⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 10⁹Me in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
baryonic matter
dark matter core
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/167247

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spelling Baryon-induced collapse of dark matter cores into supermassive black holesArgüelles, Carlos RaúlRueda, JorgeRuffini, RemoCiencias Astronómicasbaryonic matterdark matter coreNonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c² fermion, which leads to ∼10⁷M⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρb and velocity vb inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 10⁷M⊙ SMBH, for Qb = pb/vb³= 0.125M⊙ /(100 km s pc)³ , forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 10⁷M⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈10⁷–10⁸M⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 10⁹Me in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.Instituto de Astrofísica de La Plata2024info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/167247enginfo:eu-repo/semantics/altIdentifier/issn/2041-8213info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/ad1490info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:44:31Zoai:sedici.unlp.edu.ar:10915/167247Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:44:31.843SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Baryon-induced collapse of dark matter cores into supermassive black holes
title Baryon-induced collapse of dark matter cores into supermassive black holes
spellingShingle Baryon-induced collapse of dark matter cores into supermassive black holes
Argüelles, Carlos Raúl
Ciencias Astronómicas
baryonic matter
dark matter core
title_short Baryon-induced collapse of dark matter cores into supermassive black holes
title_full Baryon-induced collapse of dark matter cores into supermassive black holes
title_fullStr Baryon-induced collapse of dark matter cores into supermassive black holes
title_full_unstemmed Baryon-induced collapse of dark matter cores into supermassive black holes
title_sort Baryon-induced collapse of dark matter cores into supermassive black holes
dc.creator.none.fl_str_mv Argüelles, Carlos Raúl
Rueda, Jorge
Ruffini, Remo
author Argüelles, Carlos Raúl
author_facet Argüelles, Carlos Raúl
Rueda, Jorge
Ruffini, Remo
author_role author
author2 Rueda, Jorge
Ruffini, Remo
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
baryonic matter
dark matter core
topic Ciencias Astronómicas
baryonic matter
dark matter core
dc.description.none.fl_txt_mv Nonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c² fermion, which leads to ∼10⁷M⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρb and velocity vb inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 10⁷M⊙ SMBH, for Qb = pb/vb³= 0.125M⊙ /(100 km s pc)³ , forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 10⁷M⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈10⁷–10⁸M⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 10⁹Me in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.
Instituto de Astrofísica de La Plata
description Nonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c² fermion, which leads to ∼10⁷M⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρb and velocity vb inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 10⁷M⊙ SMBH, for Qb = pb/vb³= 0.125M⊙ /(100 km s pc)³ , forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 10⁷M⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈10⁷–10⁸M⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 10⁹Me in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.
publishDate 2024
dc.date.none.fl_str_mv 2024
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/167247
url http://sedici.unlp.edu.ar/handle/10915/167247
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/2041-8213
info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/ad1490
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
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