The maximum stellar mass, star-cluster formation and composite stellar   populations
  We demonstrate that the mass of the most massive star in a cluster correlates non-trivially with the cluster mass. A simple algorithm according to which a cluster is filled up with stars that are chosen randomly from the standard IMF but sorted with increasing mass yields an excellent description of the observational data. Algorithms based on random sampling from the IMF without sorted adding are ruled out with a confidence larger than 0.9999. A physical explanation of this would be that a cluster forms by more-massive stars being consecutively added until the resulting feedback energy suffices to revert cloud contraction and stops further star formation. This has important implications for composite populations. For example, 10^4 clusters of mass 10^2 Msol will not produce the same IMF as one cluster with a mass of 10^6 Msol. It also supports the notion that the integrated galaxial IMF (IGIMF) should be steeper than the stellar IMF and that it should vary with the star-formation rate of a galaxy. 
Carsten Weidner, Pavel Kroupa (Sternwarte Bonn)