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Article: Black hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations

TitleBlack hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations
Authors
Keywordsgravitational waves
methods: numerical
quasars: supermassive black holes
Issue Date2020
PublisherRoyal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/
Citation
Monthly Notices of the Royal Astronomical Society, 2020, v. 498 n. 2, p. 2219-2238 How to Cite?
AbstractMassive black hole (MBH) coalescences are powerful sources of low-frequency gravitational waves. To study these events in the cosmological context, we need to trace the large-scale structure and cosmic evolution of a statistical population of galaxies, from dim dwarfs to bright galaxies. To cover such a large range of galaxy masses, we analyse two complementary simulations: HORIZON-AGN with a large volume and low resolution that tracks the high-mass (⁠>107M⊙⁠) MBH population, and NEWHORIZON with a smaller volume but higher resolution that traces the low-mass ( <107M⊙⁠) MBH population. While HORIZON-AGN can be used to estimate the rate of inspirals for pulsar timing arrays, NEWHORIZON can investigate MBH mergers in a statistical sample of dwarf galaxies for LISA, which is sensitive to low-mass MBHs. We use the same method to analyse the two simulations, post-processing MBH dynamics to account for time delays mostly determined by dynamical friction and stellar hardening. In both simulations, MBHs typically merge long after galaxies do, so that the galaxy morphology at the time of the MBH merger is no longer determined by the structural disturbances engendered by the galaxy merger from which the MBH coalescence has originated. These time delays cause a loss of high-z MBH coalescences, shifting the peak of the MBH merger rate to z ∼ 1–2. This study shows how tracking MBH mergers in low-mass galaxies is crucial to probing the MBH merger rate for LISA and investigate the properties of the host galaxies.
Persistent Identifierhttp://hdl.handle.net/10722/294626
ISSN
2023 Impact Factor: 4.7
2023 SCImago Journal Rankings: 1.621
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorVolonteri, M-
dc.contributor.authorPfister, H-
dc.contributor.authorBeckmann, RS-
dc.contributor.authorDubois, Y-
dc.contributor.authorColpi, M-
dc.contributor.authorConselice, CJ-
dc.contributor.authorDotti, M-
dc.contributor.authorMartin, G-
dc.contributor.authorJackson, R-
dc.contributor.authorKraljic, K-
dc.contributor.authorPichon, C-
dc.contributor.authorTrebitsch, M-
dc.contributor.authorYi, S-
dc.contributor.authorDevriendt, J-
dc.contributor.authorPeirani, S-
dc.date.accessioned2020-12-08T07:39:38Z-
dc.date.available2020-12-08T07:39:38Z-
dc.date.issued2020-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2020, v. 498 n. 2, p. 2219-2238-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/294626-
dc.description.abstractMassive black hole (MBH) coalescences are powerful sources of low-frequency gravitational waves. To study these events in the cosmological context, we need to trace the large-scale structure and cosmic evolution of a statistical population of galaxies, from dim dwarfs to bright galaxies. To cover such a large range of galaxy masses, we analyse two complementary simulations: HORIZON-AGN with a large volume and low resolution that tracks the high-mass (⁠>107M⊙⁠) MBH population, and NEWHORIZON with a smaller volume but higher resolution that traces the low-mass ( <107M⊙⁠) MBH population. While HORIZON-AGN can be used to estimate the rate of inspirals for pulsar timing arrays, NEWHORIZON can investigate MBH mergers in a statistical sample of dwarf galaxies for LISA, which is sensitive to low-mass MBHs. We use the same method to analyse the two simulations, post-processing MBH dynamics to account for time delays mostly determined by dynamical friction and stellar hardening. In both simulations, MBHs typically merge long after galaxies do, so that the galaxy morphology at the time of the MBH merger is no longer determined by the structural disturbances engendered by the galaxy merger from which the MBH coalescence has originated. These time delays cause a loss of high-z MBH coalescences, shifting the peak of the MBH merger rate to z ∼ 1–2. This study shows how tracking MBH mergers in low-mass galaxies is crucial to probing the MBH merger rate for LISA and investigate the properties of the host galaxies.-
dc.languageeng-
dc.publisherRoyal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectgravitational waves-
dc.subjectmethods: numerical-
dc.subjectquasars: supermassive black holes-
dc.titleBlack hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations-
dc.typeArticle-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1093/mnras/staa2384-
dc.identifier.scopuseid_2-s2.0-85095885190-
dc.identifier.hkuros320427-
dc.identifier.volume498-
dc.identifier.issue2-
dc.identifier.spage2219-
dc.identifier.epage2238-
dc.identifier.isiWOS:000587746400046-
dc.publisher.placeUnited Kingdom-

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