Morphology, structure and kinematics of galaxies in hydrodynamical simulations
The light or matter distribution and the dynamical state of a single galaxy can be empirically characterized through the morphology, structure, and kinematic parameters. Observations have identified many relations among galaxy properties, some of which are reproduced by the current hydrodynamical simulations. With simulations, we may also gain insights into how the observed trends are formed, using some information that is difficult to obtain from observations. I will mainly talk about two examples regarding the morphologies and sizes of galaxies, including their relations with star formation, dark matter halo properties, etc. I will compare the results of simulations with those of observations, and show some examples of studies on their origins, scatters, etc. that make use of simulations.