Revealing the relation between black hole growth and host-galaxy compactness among star-forming galaxies

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dc.contributor.authorNi, Q.
dc.contributor.authorBrandt, W. N.
dc.contributor.authorYang, G.
dc.contributor.authorLeja, J.
dc.contributor.authorChen, C-T J.
dc.contributor.authorLuo, B.
dc.contributor.authorMatharu, J.
dc.contributor.authorSun, M.
dc.contributor.authorVito, F.
dc.contributor.authorXue, Y. Q.
dc.contributor.authorZhang, K.
dc.date.accessioned2025-01-20T23:55:17Z
dc.date.available2025-01-20T23:55:17Z
dc.date.issued2021
dc.description.abstractRecent studies show that a universal relation between black hole (BH) growth and stellar mass (M-*) or star formation rate (SFR) is an oversimplification of BH-galaxy coevolution, and that morphological and structural properties of host galaxies must also be considered. Particularly, a possible connection between BH growth and host-galaxy compactness was identified among star-forming (SF) galaxies. Utilizing approximate to 6300 massive galaxies with I-814W < 24 at z < 1.2 in the Cosmic Evolution Survey (COSMOS) field, we perform systematic partial correlation analyses to investigate how sample-averaged BH accretion rate (BHAR) depends on host-galaxy compactness among SF galaxies, when controlling for morphology and M-* (or SFR). The projected central surface mass density within 1 kpc, Sigma(1), is utilized to represent host-galaxy compactness in our study. We find that the BHAR-Sigma(1) relation is stronger than either the BHAR-M-* or BHAR-SFR relation among SF galaxies, and this BHAR-Sigma(1) relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This BHAR-Sigma(1) relation among SF galaxies suggests a link between BH growth and the central gas density of host galaxies on the kpc scale, which may further imply a common origin of the gas in the vicinity of the BH and in the central similar to kpc of the galaxy. This BHAR-Sigma(1) relation can also be interpreted as the relation between BH growth and the central velocity dispersion of host galaxies at a given gas content (i.e. gas mass fraction), indicating the role of the host-galaxy potential well in regulating accretion on to the BH.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/staa3514
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/staa3514
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/95078
dc.identifier.wosidWOS:000606297700050
dc.issue.numero4
dc.language.isoen
dc.pagina.final5008
dc.pagina.inicio4989
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectgalaxies: evolution
dc.subjectgalaxies: nuclei
dc.subjectX-rays: galaxies
dc.titleRevealing the relation between black hole growth and host-galaxy compactness among star-forming galaxies
dc.typeartículo
dc.volumen500
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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