  We investigate the effects of an oscillating gas filament on the dynamics of
its embedded stellar clusters. Motivated by recent observational constraints,
we model the host gas filament as a cylindrically symmetrical potential, and
the star cluster as a Plummer sphere. In the model, the motion of the filament
will produce star ejections from the cluster, leaving star cluster remnants
that can be classified into four categories: a) Filament Associated clusters,
which retain most of their particles (stars) inside the cluster and inside the
filament; b) destroyed clusters, where almost no stars are left inside the
filament, and there is no surviving bound cluster; c) ejected clusters, that
leave almost no particles in the filament, since the cluster leaves the gas
filament; and d) transition clusters, corresponding to those clusters that
remain in the filament, but that lose a significant fraction of particles due
to ejections induced by filament oscillation. Our numerical investigation
predicts that the Orion Nebula Cluster is in the process of being ejected,
after which it will most likely disperse into the field. This scenario is
consistent with observations which indicate that the Orion Nebula Cluster is
expanding, and somewhat displaced from the Integral Shaped Filament ridgeline.
