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We carried out a molecular line study toward the three Spitzer bubbles S116,S117 and S118 which show active formation of high-mass stars. We foundmolecular gas consisting of two components with velocity difference of {$\sim5$ \kms}. One of them, the small cloud, has typical velocity of {$-63$ \kms} \and the other, the large cloud, has that of $-58$ \kms. The large cloud has anearly circular intensity depression whose size is similar to the small cloud.We present an interpretation that the cavity was created by a collision betweenthe two clouds and the collision compressed the gas into a dense layerelongated along the western rim of the small cloud. In this scenario, the Ostars including those in the three Spitzer bubbles were formed in the interfacelayer compressed by the collision. By assuming that the relative motion of theclouds has a tilt of \timeform{45D} to the line of sight, we estimate that thecollision continued over the last 1 Myr at relative velocity of $\sim$10 \kms.In the S116--117--118 system the \HII \ regions are located outside of thecavity. This morphology is ascribed to the density-bound distribution of thelarge cloud which made the \HII \ regions more easily expand toward the outerpart of the large cloud than inside of the cavity. The present case proves thata cloud-cloud collision creates a cavity without an action of O star feedback,and suggests that the collision-compressed layer is highly filamentary.

publications of the astronomical society of japan

Molecular clouds toward three Spitzer bubbles S116, S117 and S118:  Evidence for the cloud-cloud collision which formed the three \HII \ regions  and a 10-pc scale molecular cavity