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We present the results of C18O observations by the Nobeyama Millimeter Arraytoward dense clumps with radii of ~ 0.3 pc in six cluster-forming regionsincluding massive (proto)stars. We identified 171 cores, whose radius, linewidth, and molecular mass range from 0.01 to 0.09 pc, 0.43 to 3.33 km/s, and0.5 to 54.1 Mo, respectively. Many cores with various line widths exist in oneclump, and the index of the line width-radius relationship of the cores and theparental clump differs from core to core in the clump. This indicates that thedegree of dissipation of the turbulent motion varies for each core in oneclump. Although the mass of the cores increases with the line width, most coresare gravitationally bound by the external pressure. In addition, the line widthand the external pressure of the cores tend to decrease with the distance fromthe center of the clump, and these dependencies may be caused by the inner H2density structure of the clump that affects the physical properties of thecores. Moreover, the number density of the cores and the number density ofyoung (proto)stars have a similar relationship to the average H2 density of theclumps. Thus, our findings suggest that the cluster is formed in the clumpthrough the formation of such multiple cores, whose physical properties wouldhave been strongly related to the H2 density structure and the turbulent motionof the clump.

High-Resolution Studies of the Multiple-Core Systems toward Cluster-Forming Regions Including Massive Stars