The VMC survey -- XLVII. Turbulence-Controlled Hierarchical Star Formation in the Large Magellanic Cloud

TL;DR

This study analyzes the hierarchical structure of young stars in the Large Magellanic Cloud, revealing fractal, turbulence-driven patterns consistent across scales from 10 to 700 parsecs.

Contribution

It provides the first detailed statistical analysis of young stellar structures in the LMC, linking their fractal properties to turbulence in the gas clouds they form from.

Findings

Young stellar structures follow power-law size and mass distributions.

Fractal dimensions of structures are approximately 1.5.

Star formation in the LMC is scale-free from 10 to 700 parsecs.

Abstract

We perform a statistical clustering analysis of upper main-sequence stars in the Large Magellanic Cloud (LMC) using data from the Visible and Infrared Survey Telescope for Astronomy survey of the Magellanic Clouds. We map over 2500 young stellar structures at 15 significance levels across ~120 square degrees centred on the LMC. The structures have sizes ranging from a few parsecs to over 1 kpc. We find that the young structures follow power-law size and mass distributions. From the perimeter-area relation, we derive a perimeter-area dimension of 1.44+-0.20. From the mass-size relation and the size distribution, we derive two-dimensional fractal dimensions of 1.50+-0.10 and 1.61+-0.20, respectively. We find that the surface density distribution is well-represented by a lognormal distribution. We apply the Larson relation to estimate the velocity dispersions and crossing times of these structures. Our results indicate that the fractal nature of the young stellar structures has been inherited from the gas clouds from which they form and that this architecture is generated by supersonic turbulence. Our results also suggest that star formation in the LMC is scale-free from 10 pc to 700 pc.