Formation of Globular Clusters In and Out of Dwarf Galaxies球状星团形成，从矮星系.pptVIP

Formation of Globular Clusters in Hierarchical Cosmology: ART and Science Oleg Gnedin Ohio State University The outcome of models of GC formation depends largely on the initial conditions In hierarchical cosmology, initial conditions are Pushing the limit of current hydrodynamic simulations Clues about star cluster formation from local galaxies Star clusters in spiral arms of high-redshift disks Zero-age mass function of model GCs is in excellent agreement with the mass function of young clusters Half-mass radii of model GCs match those of the Galactic globular clusters Metallicities of model GCs at z 3 Clusters with different metallicity are forming at the same epoch in progenitors of different mass Supergiant molecular clouds form after gas-rich mergers Rate of galaxy mergers declines steadily from high to low z Does reionization matter? The mass function of young clusters deviates from the mass function of globular clusters at low masses Dynamical disruption of star clusters Different types of orbits of globular clusters Not all initial conditions and evolutionary scenarios are consistent with the observed mass function Mergers of progenitor galaxies ensure spheroidal distribution of GC system now Spatial distribution Kinematics Summary Metallicity bimodality: decide what we should explain * Cosmological objects Jeans mass after recombination (Peebles Dicke 1968), DM halos before reionization (Bromm Clarke 2002), triggered by ionization fronts during reionization (Cen 2001) or by galaxy outflows (Scannapiesco et al. 2004) Hierarchical dissipational models [ Searle-Zinn fragments ] supergiant molecular clouds ~ 108 M? (Harris Pudritz 1994), agglomeration of gas clouds at z = 5 ?1 (Weil Pudritz 2001), multi-phase collapse (Forbes, Brodie, Grillmair 1997), semi-analytical galaxy formation (Beasley et al. 2002) Hierarchical dissipationless models accretion of dwarf galaxies (C?té, Marzke West 1998) Thermal instabi