  The rapidly improving quality and resolution of both low surface brightness
observations and cosmological simulations of galaxies enables one to address
the important question how the formation history is imprinted in the outer,
unrelaxed regions of galaxies, and to inspect the correlations of such imprints
with the internal kinematics. Using the hydrodynamical cosmological simulation
Magneticum Pathfinder, we identify tidal tails, shells, streams, and satellite
planes, and connect their existence to the amount of rotational support and the
formation histories of the host galaxies. This presents the first combined
statistical census considering all those four types of features in
hydrodynamical cosmological simulations. Tidal features are visually classified
from a 3D rendering of the simulated galaxies by several scientists. The
results are compared to observations, especially from the MATLAS survey.
Prominent features are more common around elliptical than around disk galaxies.
Shells are preferentially found around kinematically slowly rotating galaxies
in both simulations and observations, while streams only have a slight
preference to be present around slowly rotating galaxies. Tails and satellite
planes appear independently of the internal kinematics of the central galaxy,
indicating that they are formed through processes that have not (yet) affected
the internal kinematics. As shells are formed through radial merger events
while streams are remnants of circular merger infall, this suggests that the
orbital angular momentum of the merger event plays a more crucial role in
transforming the host galaxy than previously anticipated. The existence of
shells around slow rotators is further a sign of a radial merger formation for
the particular slow rotators, as a third of the galaxies with a shell were
transformed into slow rotators by the merger event that also caused the shells.
