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.
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