  Traditional studies of stellar clusters in external galaxies use surface
photometry and therefore focus on systems that are still bright and compact
enough to be separated from the stellar background. Consequently, the latter
stages of unbound cluster evolution are still poorly understood. This
dramatically constrains our knowledge of the dissolution processes of stellar
clusters in various physical environments.
  We present the first results of a new approach to directly detect and
quantify the characteristics of evolved stellar clusters. Using the exceptional
spatial resolution and sensitivity of HST/ACS images to resolve the stellar
content nearby galaxies, we construct colour-magnitude diagrams for the
observed fields. This enable us to separate the younger population likely
present in young clusters from the older stellar content of the star field
background. We utilize a clustering algorithm to assign each star to a group
based on its local spatial density. This novel approach makes use of algorithms
typically applied in N-body and cosmological studies. We test the method and
show that it successfully detects less compact clusters that would normally be
lost in the star field background. We also detect B-type stars well spread in
the galaxy disk of NGC 1313, probably the result of infant mortality of stellar
clusters.
