Abstract
We use semi-analytical models to analyze galaxy formation in low resolution cosmological N-body simulations and to study star formation rates in time. Our implementation follows the evolution of galaxies in halos through the fusion merger trees of halos in a similar way as presented in Kauffmann et al. (1993, MNRAS, 264, 201) and Kang et al. (2005, ApJ, 631, 21). Our procedure to model the evolution of baryons in halos includes star formation, radiative cooling, supernovae feedback and mergers of galaxies. In our first results we obtain properties of galaxies at redshift z = 0 with which we verify the results of our code, and present some results on the evolution of the star formation rate for the most massive halos in our simulations. Our results are in good agreement with other works and with observations, but star formation rates show deviations compared with some observations.
