Very massive stars in not so massive clusters
  Very young star clusters in the Milky Way exhibit a well-defined relation
between their maximum stellar mass, m_max, and their mass in stars, M_ecl. A
recent study shows that the young intermediate-mass star cluster VVV CL041
possibly hosts a >80 Msun star, WR62-2, which appears to violate the existence
of the m_max-M_ecl relation since the mass of the star is almost two times
higher than that expected from the relation. By performing direct N-body
calculations with the same mass as the cluster VVV CL041 (3000 Msun), we study
whether such a very massive star can be formed via dynamically induced stellar
collisions in a binary-rich star cluster that initially follows the m_max-M_ecl
relation. Eight out of 100 clusters form a star more massive than 80 Msun
through multiple stellar collisions. This suggests that the VVV CL041 cluster
may have become an outlier of the relation because of its early-dynamical
evolution, even if the cluster followed the relation at birth. We find that
more than half of our model clusters host a merger product as its most massive
member within the first 5 Myr of cluster evolution. Thus, the existence of
stars more massive than the m_max-M_ecl relation in some young clusters is
expected due to dynamical processes despite the validity of the m_max-M_ecl
relation. We briefly discuss evolution of binary populations in our model.
