Observational Constraints on the Theory of the IMF
  Observational constraints on the theory of the IMF are reviewed. These observations include the new result that star formation is very rapid, usually going from start to finish in only 1 or 2 dynamical times on a wide range of scales. This result, combined with the observation that the IMF is independent of cluster density over a factor of several hundred, implies that protostar coagulation during orbital motions in a cloud are not important for the IMF: there is not enough time. The observation that the IMF in individual clusters is about the same as the IMF in whole galaxies implies that stars of all masses form randomly in self-gravitating clouds of all masses. There cannot be a sequence of stellar masses in a cluster, based on stirring or heating for example, where the largest star that forms keeps increasing until the cloud is destroyed. The uniformity of the IMF over time and space argues for a process that is independent of specific properties of molecular clouds. This uniformity, along with the common observation of young stars in hierarchical clusters that resemble the structures of interstellar gas, suggests that the IMF, at least in the power law range, is a by-product of turbulence. Detailed physical processes may affect the turnover at low mass, but even this may have a universal character arising from a combination of turbulence-induced variations in the local cloud properties, and fragmentation in unstable cloud pieces. 
B. G. Elmegreen (IBM Watson Research Center)