Insights for Early Massive Black Hole Growth from JWST Detection of the [Ne v] λ3427 Emission Line

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dc.catalogadorvzp
dc.contributor.authorBenny Trakhtenbrot
dc.contributor.authorClaudio Ricci
dc.contributor.authorEzequiel Treister
dc.contributor.authorMichael J. Koss
dc.contributor.authorRichard Mushotzky
dc.contributor.authorKyuseok Oh
dc.contributor.authorAlessandro Peca
dc.contributor.authorFranz E. Bauer
dc.contributor.authorKriti Kamal Gupta
dc.contributor.authorTomer Reiss
dc.date.accessioned2025-10-29T17:42:50Z
dc.date.available2025-10-29T17:42:50Z
dc.date.issued2025
dc.description.abstractWe use the narrow [Ne v] λ3427 emission line detected in the recently published JWST spectra of two galaxies, at z ≃ 6.9 and 5.6, to study the key properties of the active galactic nuclei (AGN) and the supermassive black holes (SMBHs) in their centers. Using a new empirical scaling linking the [Ne V] line emission with AGN accretiondriven (continuum) emission, derived from a highly complete low-redshift AGN sample, we show that the [Ne V] emission in the two z > 5 galaxies implies total (bolometric) AGN luminosities of order Lbol ≈ (4–8) × 1045 erg s −1 . Assuming that the radiation emitted from these systems is Eddington limited, the (minimal) black hole (BH) masses are of order MBH ≳ 107 M⊙. Combined with the published stellar masses of the galaxies, estimated from dedicated fitting of their spectral energy distributions, the implied BH-to-stellar mass ratios are of order MBH/Mhost ≈ 0.1–1. This is considerably higher than what is found in the local Universe, but is consistent with the general trend seen in some other z ≳ 5 AGN. Given the intrinsic weakness of the [Ne V] line and the nature of the [Ne V] –to–Lbol scaling, any (rare) detection of the [Ne v] λ3427 line at z > 5 would translate to similarly high AGN luminosities and SMBH masses, thus providing a unique observational path for studying luminous AGN well into the epoch of reionization, including obscured sources.
dc.format.extent7 páginas
dc.fuente.origenORCID
dc.identifier.doi10.3847/2041-8213/ae0d8c
dc.identifier.eissn2041-8213
dc.identifier.issn2041-8205
dc.identifier.urihttps://doi.org/10.3847/2041-8213/ae0d8c
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/106388
dc.information.autorucInstituto de Astrofísica; Treister , Ezequiel; 0000-0001-7568-6412; 1031846
dc.issue.numero1
dc.language.isoen
dc.nota.accesocontenido completo
dc.pagina.final7
dc.pagina.inicio1
dc.revistaThe Astrophysical Journal Letters
dc.rightsacceso abierto
dc.rights.licenseAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectNúcleos galácticos activos
dc.subjectGalaxias de alto corrimiento al rojo
dc.subjectAgujeros negros supermasivos
dc.subjectGalaxias anfitrionas de AGN
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.subject.ods09 Industry, innovation and infrastructure
dc.subject.odspa09 Industria, innovación e infraestructura
dc.titleInsights for Early Massive Black Hole Growth from JWST Detection of the [Ne v] λ3427 Emission Line
dc.title.alternativePerspectivas para el crecimiento temprano de agujeros negros masivos a partir de la detección de la línea de emisión
dc.typeartículo
dc.volumen993
sipa.trazabilidadORCID;2025-10-20
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