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There have been many studies aiming to reveal the origins of the star-gasmisalignment found in galaxies, but there still is a lack of understanding ofthe contribution from each formation channel candidate. We aim to answer thequestion by investigating the misaligned galaxies in Horizon-AGN, acosmological large-volume simulation of galaxy formation. There are 27,903galaxies of stellar mass $M_* > 10^{10} M_\odot$ in our sample, of which 5,984are in a group of the halo mass of $M_{200} > 10^{12} M_\odot$. We haveidentified four main formation channels of misalignment and quantified theirlevel of contribution: mergers (35%), interaction with nearby galaxies (23%),interaction with dense environments or their central galaxies (21%), andsecular evolution including smooth accretion from neighboring filaments (21%).We found in the simulation that the gas, rather than stars, is typically morevulnerable to dynamical disturbances; hence, misalignment formation is mainlydue to the change in the rotational axis of the gas rather than stars,regardless of the origin. We have also inspected the lifetime (duration) of themisalignment. The decay timescale of the misalignment shows a stronganti-correlation with the kinematic morphology ($V/{\sigma}$) and the cold gasfraction of the galaxy. The misalignment has a longer lifetime in denserregions, which is linked with the environmental impact on the host galaxy.There is a substantial difference in the length of the misalignment lifetimedepending on the origin, and it can be explained by the magnitude of theinitial position angle offset and the physical properties of the galaxies.

Star-Gas Misalignment in Galaxies: II. Origins Found from the Horizon-AGN Simulation