Aspects of Galaxy Formation

Abstract

The universe at large scales is homogeneous and isotropic (∼ 100M pc). But, at smaller scales galaxies can be observed. If density perturbations exist at small scales the formation of such objects can be reasoned using Newtonian gravity. The evolution of such perturbations can be studied considering their distribution of matter in the universe to be continuous and fluid. The objects undergoing grav- itational infall virialise. For various masses of objects the temperature and radii can be calculated as a function of time. Further, upper and lower limit on such objects and their abundances an be obtained as a function of time. These aspects of galaxy formation can then be applied to specific problems of reionization and metal enrichment in galaxies.