The Integral Shaped Filament ( ISF ) is the nearest molecular cloud with rapid star formation , including massive stars , and it is therefore a star-formation laboratory . We use Gaia parallaxes , to show that the distances to young Class II stars ( ‘ ‘ disks ’ ’ ) projected along the spine of this filament are related to the gas radial velocity by v = - { D \over \tau } + K; \tau = 4 { Myr } , where K is a constant . This implies that the ISF is a standing wave , which is consistent with the Stutz & Gould ( 2016 ) ‘ ‘ Slingshot ’ ’ prediction . The \tau = 4 { Myr } timescale is consistent with the ‘ ‘ Slingshot ’ ’ picture that the Orion Nebula Cluster ( ONC ) is the third cluster to be violently split off from the Orion A cloud ( following NGC 1981 and NGC 1987 ) at few-Myr intervals due to gravito-magnetic oscillations . We also present preliminary evidence that the truncation of the ISF is now taking place 16 ^ { \prime } south of the ONC and is mediated by a torsional wave that is propagating south with a characteristic timescale \tau _ { torsion } = 0.5 { Myr } , i.e . eight times shorter . The relation between these two wave phenomena is not presently understood .