Abstract
The authors present detailed simulations of open clusters including the effects produced by stellar rotation and by the presence of unresolved binaries. They apply for the first time the non parametric statistic D, and follow a Bayesian approach to derive the initial mass function in several open clusters. It is found that even though the slope of the IMF seems rather constant above 1.2 Msun, there is some variability at smaller masses, perhaps linked with mass segregation.
