Piercing through Highly Obscured and Compton-thick AGNs in the Chandra Deep Fields. II. Are Highly Obscured AGNs the Missing Link in the Merger-triggered AGN-Galaxy Coevolution Models?

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dc.contributor.authorLi, Junyao
dc.contributor.authorXue, Yongquan
dc.contributor.authorSun, Mouyuan
dc.contributor.authorBrandt, William N.
dc.contributor.authorYang, Guang
dc.contributor.authorVito, Fabio
dc.contributor.authorTozzi, Paolo
dc.contributor.authorVignali, Cristian
dc.contributor.authorComastri, Andrea
dc.contributor.authorShu, Xinwen
dc.contributor.authorFang, Guanwen
dc.contributor.authorFan, Lulu
dc.contributor.authorLuo, Bin
dc.contributor.authorChen, Chien-Ting
dc.contributor.authorZheng, Xuechen
dc.date.accessioned2025-01-23T19:47:24Z
dc.date.available2025-01-23T19:47:24Z
dc.date.issued2020
dc.description.abstractBy using a large, highly obscured ( N-H > 10(23) cm(-2)) active galactic nucleus (AGN) sample (294 sources at z similar to 0-5) selected from detailed X-ray spectral analyses in the deepest Chandra.surveys, we explore distributions of these X-ray sources in various optical/infrared/X-ray color-color diagrams and their host-galaxy properties, aiming at characterizing the nuclear obscuration environment and the triggering mechanism of highly obscured AGNs. We find that the refined Infrared Array Camera (IRAC) color-color diagram fails to identify the majority of X-ray-selected, highly obscured AGNs, even for the most luminous sources with log L-X(erg s(-1)) > 44. Over 80% of our sources will not be selected as heavily obscured candidates using the flux ratio of f(24 mu m)/f(R) > 1000 and R - K > 4.5 criteria, implying complex origins and conditions for the obscuring materials that are responsible for the heavy X-ray obscuration. The average star formation rate (SFR) of highly obscured AGNs is similar to that of stellar mass-(M*-) and z-controlled normal galaxies, while a lack of quiescent hosts is observed for the former. Partial correlation analyses imply that highly obscured AGN activity (traced by L-X) appears to be more fundamentally related to M*, and no dependence of N-H on either M* or SFR is detected. Morphology analyses reveal that 61% of our sources have a significant disk component, while only similar to 27% of them exhibit irregular morphological signatures. These findings together point toward a scenario where secular processes (e.g., galacticdisk instabilities), instead of mergers, are most probable to be the leading mechanism that triggers accretion activities of X-ray-selected, highly obscured AGNs.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/abb6e7
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/abb6e7
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100378
dc.identifier.wosidWOS:000585797500001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectAGN host galaxies
dc.subjectActive galaxies
dc.subjectX-ray active galactic nuclei
dc.titlePiercing through Highly Obscured and Compton-thick AGNs in the Chandra Deep Fields. II. Are Highly Obscured AGNs the Missing Link in the Merger-triggered AGN-Galaxy Coevolution Models?
dc.typeartículo
dc.volumen903
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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