  We perform simulations to test the effects of a moving gas filament on a
young star cluster (i.e. the "Slingshot" Model). We model Orion Nebula
Cluster-like clusters as Plummer spheres and the Integral Shaped Filament gas
as a cylindrical potential. We observe that in a static filament, an initially
spherical cluster evolves naturally into an elongated distribution of stars.
For sinusoidal moving filaments, we observe different remnants, and classify
them into 4 categories.%: 3 different objects and one transition object.
"Healthy" clusters, where almost all the stars stay inside the filament and the
cluster; "destroyed" clusters are the opposite case, with almost no particles
in the filament or near the centre of density of the clusters; "ejected"
clusters, where a large fraction of stars are close to the centre of density of
the stars , but almost none of them in the filament; and "transition" clusters,
where roughly the same number of particles is ejected from the cluster and from
the filament. An {{Orion Nebula Cluster-like}} cluster might stay inside the
filament or be ejected, but it will not be destroyed.
