Cluster distribution from Galactic simulations of M51 model

Using a model of M51 we want to compare the cluster distribution of our model with observations. The M51 model consists of an axisymmetric potential with spiral arms and Giant Molecular Clouds (GMCs). Stellar clusters will interact with the galactic tidal field and can as a consequence be destroyed. Accounting for the destruction of clusters we hope to re-create the cluster distribution of M51 and explain the important effects involved.