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By using a large highly obscured ($N_{\rm H} > 10^{23}\ \rm cm^{-2}$) AGNsample (294 sources at $z \sim 0-5$) selected from detailed X-ray spectralanalyses in the deepest Chandra surveys, we explore distributions of theseX-ray sources in various optical/IR/X-ray color-color diagrams and theirhost-galaxy properties, aiming at characterizing the nuclear obscurationenvironment and the triggering mechanism of highly obscured AGNs. We find thatthe refined IRAC color-color diagram fails to identify the majority of X-rayselected highly obscured AGNs, even for the most luminous sources with ${\rmlog}\,L_{\rm X}\, \rm (erg\ s^{-1}) > 44$. Over 80% of our sources will not beselected as heavily obscured candidates using the flux ratio of $f_{\rm 24 \mum}\, /\,f_R > 1000$ and $R - K > 4.5$ criteria, implying complex origins andconditions for the obscuring materials that are responsible for the heavy X-rayobscuration. The average star formation rate of highly obscured AGNs is similarto that of stellar mass- ($M_*$-) and $z$-controlled normal galaxies, while thelack of quiescent hosts is observed for the former. Partial correlationanalyses imply that highly obscured AGN activity (traced by $L_{\rm X}$)appears to be more fundamentally related to $M_*$, and no dependence of $N_{\rmH}$ on either $M_*$ or SFR is detected. Morphology analyses reveal that 61% ofour sources have a significant disk component, while only 27% of them exhibitirregular morphological signatures. These findings together point toward ascenario where secular processes (e.g., galactic-disk instabilities), insteadof mergers, are most probable to be the leading mechanism that triggersaccretion activities of X-ray-selected highly obscured AGNs.

astrophysical journal/the astrophysical journal

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?