Cloud mass function in a disk galaxy

Abstract

In order to study formation and evolution of interstellar clouds, we simulate the multi-phase interstellar matter in a disk galaxy using an SPH code, considering radiative cooling, cloud formation, star formation and heating by supernovae. By calculating various cases of total interstellar mass and strength of UV background radiation, we study how cloud mass function depends on theses parameters. We show that the power index, α, of the cloud mass function is small when there is a large amount of interstellar medium or strong UV radiation. Our results suggest that cloud mass function is a good indicator of these interstellar processes.