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We investigate the connection between the morphology and internal kinematicsof the stellar component of central galaxies with mass $M_\star > {10}^{9.5}{\rm M}_\odot$ in the EAGLE simulations. We compare several kinematicdiagnostics commonly used to describe simulated galaxies, and find goodconsistency between them. We model the structure of galaxies as ellipsoids andquantify their morphology via the ratios of their principal axes. We show thatthe differentiation of blue star-forming and red quiescent galaxies usingmorphological diagnostics can be achieved with similar efficacy to the use ofkinematical diagnostics, but only if one is able to measure both the flatteningand the triaxiality of the galaxy. Flattened oblate galaxies exhibit greaterrotational support than their spheroidal counterparts, but there is significantscatter in the relationship between morphological and kinematical diagnostics,such that kinematically-similar galaxies can exhibit a broad range ofmorphologies. The scatter in the relationship between the flattening and theratio of the rotation and dispersion velocities ($v/\sigma$) correlatesstrongly with the anisotropy of the stellar velocity dispersion: at fixed$v/\sigma$, flatter galaxies exhibit greater dispersion in the plane defined bythe intermediate and major axes than along the minor axis, indicating that themorphology of simulated galaxies is influenced significantly by the structureof their velocity dispersion. The simulations reveal that this anisotropycorrelates with the intrinsic morphology of the galaxy's inner dark matterhalo, i.e. the halo's morphology that emerges in the absence of dissipativebaryonic physics. This implies the existence of a causal relationship betweenthe morphologies of galaxies and that of their host dark matter haloes.

The relationship between the morphology and kinematics of galaxies and its dependence on dark matter halo structure in EAGLE