Cold gas in the models of galaxy formation and evolution
Abstract
Cold gas in interstellar medium is a very important component in galaxies, which mainly includes molecular gas $\h2$ and atomic gas HI. They play significant roles in galaxy formation and evolution, and offer reservoirs for star formation. To study molecular gas and atomic gas based on the galaxy formation models, two kinds of methods are usually used. They are the semi-analytic model and the hydrodynamic simulation. Both of them have advantages and disadvantages compared to each other. In this paper, we review the progress on the model work in recent years and introduce some new results and predictions based on these models. These results cannot only give explanations for current observations, but also give predictions for future HI and CO surveys using large radio facilities, e.g. ALMA, ASKAP, SKA, FAST, etc.
