Density Exponent Analysis: Gravity-driven steepening of the density profiles of star-forming regions

TL;DR

This paper introduces a new method to map the density exponent in complex star-forming regions, revealing how gravitational collapse causes steepening of density profiles across different structures.

Contribution

The authors develop a Level-Set based formalism to generate detailed maps of the density exponent in complex, non-spherical molecular clouds, advancing the analysis of density structures.

Findings

Density exponent varies widely from -3.5 to -0.5.

Steeper density profiles are associated with later stages of gravitational collapse.

Dense structures near cores have steep profiles due to depletion.

Abstract

The evolution of molecular interstellar clouds is a complex, multi-scale process. The power-law density exponent describes the steepness of density profiles, and it has been used to characterize the density structures of the clouds yet its usage is usually limited to spherically symmetric systems. Importing the Level-Set Method, we develop a new formalism that generates robust maps of a generalized density exponent $k_{\rho}$ at every location for complex density distributions. By applying it to high fidelity, high dynamical range map of the Perseus molecular cloud constructed using data from the Herschel and Planck satellites, we find that the density exponent exhibits a surprisingly wide range of variation ($-3.5 \lesssim k_{\rho} \lesssim -0.5$). Regions at later stages of gravitational collapse are associated with steeper density profiles. Inside a region, gas located in the vicinities of dense structures has very steep density profiles with $k_{\rho} \approx -3$, which forms because of depletion. This density exponent analysis reveals diverse density structures, forming a coherent picture that gravitational collapse leads to a continued steepening of the density profile. We expect our method to be effective in studying other power-law-like density structures, including granular materials and the Large-Scale Structure of the Universe.