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We report results of observations of the GGD12-15 region, where clusterformation is actively taking place, using various molecular emission lines. TheC18O (J= 1-0) emission line reveals a massive clump in the region with a massof ~2800 Mo distributed over ~2 pc. The distribution of the C18O(J= 3-2)emission is similar to that of a star cluster forming therein, with anelliptical shape of ~1 pc in size. A bipolar molecular outflow driven by IRS9Mc, a constituent star of the cluster, is blowing in a direction perpendicularto the elongated C18O (J= 3-2) distribution, covering the entire clump. Thereis a massive core with a radius of 0.3 pc and a mass of 530 Mo in the center ofthe clump. There are two velocity components around the core, which areprominent in a position-velocity (PV) diagram along the major axis of theclump. In addition, a PV diagram along the minor axis of the clump, which isparallel to the outflow, shows a velocity gradient opposite to that of theoutflow. The velocity structure strongly indicates the infalling motion of theclump. Comparison of the observational data with a simple model of infallingoblate clumps indicates that the clump is undergoing gravitational contractionwith rotation.

Cluster Formation in GGD12-15: Infall Motion with Rotation of the Natal Clump