Evident black hole-bulge coevolution in the distant universe

Simple item page
dc.contributor.authorYang, G.
dc.contributor.authorBrandt, W. N.
dc.contributor.authorAlexander, D. M.
dc.contributor.authorChen, C. -T. J.
dc.contributor.authorNi, Q.
dc.contributor.authorVito, F.
dc.contributor.authorZhu, F. -F.
dc.date.accessioned2025-01-23T21:11:57Z
dc.date.available2025-01-23T21:11:57Z
dc.date.issued2019
dc.description.abstractObservations in the local universe show a tight correlation between the masses of supermassive black holes (SMBHs; M-BH) and host-galaxy bulges (M-bulge), suggesting a strong connection between SMBH and bulge growth. However, direct evidence for such a connection in the distant universe remains elusive. We have studied sample-averaged SMBH accretion rate ((BHAR) over bar) for bulge-dominated galaxies at z = 0.5-3. While previous observations found (BHAR) over bar is strongly related to host-galaxy stellar mass (M-star) for the overall galaxy population, our analyses show that, for the bulge-dominated population, (BHAR) over bar is mainly related to SFR rather than M-star. This (BHAR) over bar -SFR relation is highly significant, e.g. 9.0 sigma (Pearson statistic) at z = 0.5-1.5. Such a (BHAR) over bar -SFR connection does not exist among our comparison sample of galaxies that are not bulge dominated, for which M-star appears to be the main determinant of SMBH accretion. This difference between the bulge-dominated and comparison samples indicates that SMBHs only coevolve with bulges rather than the entire galaxies, explaining the tightness of the local M-BH - M-bulge correlation. Our best-fitting (BHAR) over bar -SFR relation for the bulge-dominated sample is log (BHAR) over bar = log SFR - (2.48 +/- 0.05) (solar units). The best-fitting (BHAR) over bar /SFR ratio (10(-2.48)) for bulge-dominated galaxies is similar to the observed M-BH/M-bulge values in the local universe. Our results reveal that SMBH and bulge growth are in lockstep, and thus non-causal scenarios of merger averaging are unlikely the origin of the M-BH-M-bulge correlation. This lockstep growth also predicts that the M-BH-M-bulge relation should not have strong redshift dependence.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stz611
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stz611
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100932
dc.identifier.wosidWOS:000474902000057
dc.issue.numero3
dc.language.isoen
dc.pagina.final3737
dc.pagina.inicio3721
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectgalaxies: bulges
dc.subjectgalaxies: evolution
dc.subjectgalaxies: nuclei
dc.subjectX-rays: galaxies
dc.titleEvident black hole-bulge coevolution in the distant universe
dc.typeartículo
dc.volumen485
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas