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

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 constrai...

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Autores principales: Argüelles, Carlos Raúl, Rueda, Jorge, Ruffini, Remo
Formato: Articulo
Lenguaje:Inglés
Publicado: 2024
Materias:
Ciencias Astronómicas
baryonic matter
dark matter core
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/167247
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-167247
record_format dspace
spelling I19-R120-10915-1672472024-06-13T20:09:04Z http://sedici.unlp.edu.ar/handle/10915/167247 Baryon-induced collapse of dark matter cores into supermassive black holes Argüelles, Carlos Raúl Rueda, Jorge Ruffini, Remo 2024 2024-06-13T18:50:59Z en Ciencias Astronómicas baryonic matter dark matter core 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 Articulo Articulo http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) application/pdf
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
baryonic matter
dark matter core
spellingShingle Ciencias Astronómicas
baryonic matter
dark matter core
Argüelles, Carlos Raúl
Rueda, Jorge
Ruffini, Remo
Baryon-induced collapse of dark matter cores into supermassive black holes
topic_facet Ciencias Astronómicas
baryonic matter
dark matter core
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.
format Articulo
Articulo
author Argüelles, Carlos Raúl
Rueda, Jorge
Ruffini, Remo
author_facet Argüelles, Carlos Raúl
Rueda, Jorge
Ruffini, Remo
author_sort Argüelles, Carlos Raúl
title Baryon-induced collapse of dark matter cores into supermassive black holes
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
publishDate 2024
url http://sedici.unlp.edu.ar/handle/10915/167247
work_keys_str_mv AT arguellescarlosraul baryoninducedcollapseofdarkmattercoresintosupermassiveblackholes
AT ruedajorge baryoninducedcollapseofdarkmattercoresintosupermassiveblackholes
AT ruffiniremo baryoninducedcollapseofdarkmattercoresintosupermassiveblackholes
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