Formation and evolution of globular clusters in cosmological simulations
  In a series of three papers, we introduced a novel cluster formation model
that describes the formation, growth, and disruption of star clusters in
high-resolution cosmological simulations. We tested this model on a Milky
Way-sized galaxy and found that various properties of young massive clusters,
such as the mass function and formation efficiency, are consistent with
observations in the local universe. Interestingly, most massive clusters --
globular cluster candidates -- are preferentially formed during major merger
events. We follow the dynamical evolution of clusters in the galactic tidal
field. Due to tidal disruption, the cluster mass function evolves from initial
power law to a peaked shape. The surviving clusters at $z=0$ show a broad range
of metallicity [Fe/H] from -3 to -0.5. A robust prediction of the model is the
age--metallicity relation, in which metal-rich clusters are systematically
younger than metal-poor clusters by up to 3 Gyr.
