Physical properties of 221 clumps

For {sigma}-R, its tight relation indicates a kinematic connection between hierarchical density structures, supporting theoretical models of multiscale high-mass star formation. From the L-{Sigma} relation, cloud structures can be found to transition from overvirial state ({alpha}vir>2) to subvirial state ({alpha}vir<2) as they become smaller and denser, indicating a possible shift in the governing force from turbulence to gravity.

This implies that the multiscale physical process of high-mass star formation hinges on the self-gravity of subvirial molecular clouds. However, the influence of turbulence may not be dismissed until large-scale clouds attain a subvirial state. This is pending confirmation from future multiscale kinematic observations of molecular clouds with uniform observing settings.