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The morphology of a galaxy is a manifestation of the complex interplay ofphysical processes occurring within and around it, and therefore offersindirect clues to its formation and evolution. We use both visualclassification and computer vision to verify the suspected connection betweengalaxy merging activity - as evidenced by a close/merging galaxy pair, or tidalfeatures surrounding an apparently singular system - and AGN activity. Thisstudy makes use of JADES JWST/NIRCam imagery, along with an unprecedentedlycomplete sample of AGN built using JWST/MIRI photometry in the same field. This0.9-25 micron dataset enables constraints on the host galaxy morphologies ofthe broadest possible range of AGN beyond z~1, including heavily obscuredexamples missing from previous studies. We consider two AGN samples, oneconsisting of lightly to highly obscured X-ray-selected AGN (Lyu et al. 2022),and the other, presumed Compton-thick mid-infrared-bright/X-ray-faint AGNrecently revealed by MIRI (Lyu et al. 2023). Both samples contain a significantfraction of host galaxies with disturbed morphologies at all redshifts sampled,and increasingly so towards higher redshift and AGN bolometric luminosity. Themost obscured systems show the highest fraction of strongly disturbed hostgalaxies at $95\pm4$%, followed by the moderately and unobscured/lightlyobscured subsets at $78\pm6$% and $63\pm6.5$%, respectively. From this patternof disturbances, we conclude that mergers are common amongst obscured AGN, andthat the obscured AGN phase may mark a period of significant SMBH growth. Thisfinding presents tension with the leading model on AGN fueling mechanisms(Hopkins et al. 2014) that needs reconciling.

The Relation Between AGN and Host Galaxy Properties: I. Obscured AGN reside in disturbed hosts at 0