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The growing amount of integral-field spectroscopic data creates an increaseddemand for understanding kinematic peculiarities that carry valuableinformation about the evolution of the host galaxies. For kinematicallydistinct cores (KDCs), a number of formation mechanisms have been proposed, butit is still unclear which of them commonly occur in the Universe. We aim toaddress the KDC formation in the cosmological context. We used the publiclyavailable data of the large-scale hydrodynamic cosmological simulationIllustris. We identify 134 KDCs, study their properties, and follow theirevolution back in time. Examples of four galaxies hosting KDCs are presentedand described in detail. The masses of the KDC hosts follow the generaldistribution of the Illustris galaxies, with a possible slight preferencetowards massive galaxies. KDCs can be long-lived features, with their formationepochs roughly uniformly distributed in look-back times 0-11.4 Gyr, and theycan survive even major or multiple subsequent mergers. There is no singlechannel of KDC formation, but mergers seem to be the formation mechanism forabout 60% of KDCs with a significant preference for major mergers and with thepercentage being higher among massive hosts. Other KDCs formed during apericentric passage or flyby of another galaxy, by precession of a previouslyformed rapidly rotating core, or without an obvious external cause. The meanmass-weighted stellar age inside the KDC radius is either about the same as thelook-back time of the KDC formation or older. Although the radii of our KDCsare on average larger than observed, we find that younger stellar ages aretypically associated with smaller KDCs. A significant fraction of KDC hostspossess stellar shells formed during mergers that led to KDCs within the last 5Gyr, or double peaks in their velocity dispersion maps.

Galaxies with kinematically distinct cores in Illustris