Speaker
Description
In the last years, we have seen immense progress in the success of cosmological galaxy formation simulations in reproducing a range of observables. We are now at a point in which we have converged to approximately predict the correct evolution of the stellar mass growth of galaxies. However, the main challenge we currently face is that the latter is achieved for sometimes very different physical reasons, mostly associated to the different treatment of feedback. A crucial measurement to disentangle between different, plausible models, is to study the gas content of galaxies, which provide independent validation tests to the simulations. During this talk I will discuss recent relevant comparisons between simulations and HI observations, what different simulations tell us about the evolution of HI in and around galaxies, and how we expect to use the coming HI observations to improve galaxy formation modelling.