Formation of Globular Clusters in Hierarchical Cosmology

We study the formation of globular clusters (GCs) in a Milky Way-size galaxy using a high-resolution cosmological simulation. The clusters in our model form in the strongly baryon-dominated cores of supergiant molecular clouds in the gaseous disks of high-redshift galaxies. The properties of clusters are estimated using a physically-motivated subgrid model of the isothermal cloud collapse. The first clusters in the simulation form at z~12, while the best conditions for GC formation appear to be at z~3-5. Most clusters form in the progenitor galaxies of the virial mass >10⁹ Msun and the total mass of the cluster population is strongly correlated with the mass of its host galaxy with a fraction ~2x10^-4 of the galactic baryons being in the form of GCs. In addition, the mass of the GC population and the maximum cluster mass in a given region strongly correlate with the local average star formation rate. We find that the mass, size, and metallicity distributions of the cluster population identified in the simulation are remarkably similar to the corresponding distributions of the Milky Way globulars. We find no clear mass-metallicity or age-metallicity correlations for the old clusters. The zero-age cluster mass function can be approximated by a power-law, dN/dM~M^-alpha, with alpha~2, in agreement with the mass function of young stellar clusters in starbursting galaxies. However, the shape of the zero-age mass function may be better described by the high-mass tail of a lognormal distribution which peaks at \\~10³ Msun. We discuss in detail the origin, universality, and dynamical evolution of the globular cluster mass function. Our results indicate that globular clusters with properties similar to those of observed clusters can form naturally within young dense gaseous disks at z>~3 in the LCDM cosmology.