The IMF and its Evolution

Abstract

Observations of the stellar initial mass function are reviewed. The flattening at low mass is evidence for a characteristic mass in star formation, which could be the minimum stellar mass for the onset of deuterium burning or the thermal Jeans mass. Variations in the mass of the flattened part are important for understanding star formation; e.g., starburst galaxies may be an example where the characteristic mass is larger than it is locally. A steeper high-mass slope in the extreme field studied by Massey et al. may be the result of cloud destruction and the termination of star formation by ionization, with a normal IMF in each separate cluster. The lack of a density dependence in cluster IMFs suggests that star and protostar interactions play little role in star formation or the IMF. These considerations, along with indirect observations of the IMF in the early Universe, suggest that the IMF does not vary much in its basic form over position and time, but that shifts in the characteristic mass might occur in regions with extremely high or low star formation activity.