Hierarchical galaxy formation

We describe the GALFORM semi-analytic model for calculating the formation a nd evolution of galaxies in hierarchical clustering cosmologies. It improve s upon, and extends, the earlier scheme developed by Cole et al. The model employs a new Monte Carlo algorithm to follow the merging evolution of dark matter haloes with arbitrary mass resolution. It incorporates realistic de scriptions of the density profiles of dark matter haloes and the gas they c ontain; it follows the chemical evolution of gas and stars, and the associa ted production of dust; and it includes a detailed calculation of the sizes of discs and spheroids. Wherever possible, our prescriptions for modelling individual physical processes are based on results of numerical simulation s. They require a number of adjustable parameters, which we fix by referenc e to a small subset of local galaxy data. This results in a fully specified model of galaxy formation which can be tested against other data. We apply our methods to the Lambda CDM cosmology (Omega (0) = 0.3, Lambda (0) = 0.7 ), and find good agreement with a wide range of properties of the local gal axy population: the B- and K-band luminosity functions, the distribution of colours for the population as a whole, the ratio of ellipticals to spirals , the distribution of disc sizes, and the current cold gas content of discs . Inspire of the overall success of the model, some interesting discrepanci es remain: the colour-magnitude relation for ellipticals in clusters is sig nificantly flatter than observed at bright magnitudes (although the scatter is about right), and the model predicts galaxy circular velocities, at a g iven luminosity, that are about 30 per cent larger than is observed. It is unclear whether these discrepancies represent fundamental shortcomings of t he model, or whether they result from the various approximations and uncert ainties inherent in the technique. Our more detailed methods do not change our earlier conclusion that just over half the stars in the Universe are ex pected to have formed since z less than or similar to 1.5.