# Mass-size scaling M~ r^1.67 of massive star-forming clumps -- evidences of turbulence-regulated gravitational collapse

## TL;DR

This study investigates the mass-size relationship of massive star-forming clumps across multiple scales, providing evidence that turbulence plays a key role in their gravitational collapse.

## Contribution

It presents observational confirmation of a mass-size scaling law consistent with turbulence-regulated collapse theories in massive star-forming regions.

## Key findings

- Mass and size follow M ~ r^{1.68}
- Supports turbulence-supported fragmentation model
- Dense structures are centrally condensed with rho(r) ~ r^{-2}

## Abstract

We study the fragmentation of eight massive clumps using data from ATLASGAL 870 $\mu$m, SCUBA 850 and 450 $\mu$m, PdBI 1.3 and 3.5 mm, and probe the fragmentation from 1 pc to 0.01 pc scale. We find that the masses and the sizes of our objects follow $M \sim r^{1.68\pm0.05}$. The results are in agreements with the predictions of Li (2017) where $M \sim r^{5/3}$. Inside each object, the densest structures seem to be centrally condensed, with $\rho(r)\sim r^{-2}$. Our observational results support a scenario where molecular gas in the Milky Way is supported by a turbulence characterized by a constant energy dissipation rate, and gas fragments like clumps and cores are structures which are massive enough to be dynamically detached from the ambient medium.