Molecular gas properties in young stellar clusters with a suppressed star cluster wind

TL;DR

This paper develops a self-consistent model for molecular gas in young stellar clusters where feedback is suppressed, explaining residual gas distribution and star formation efficiency, aligning well with observations.

Contribution

It introduces a novel model for residual gas distribution in clusters with suppressed winds, linking turbulence, gravity, and star formation.

Findings

Model matches observed properties of cloud D1 in NGC 5253.

Predicts residual gas density and star formation efficiency.

Provides insights into star formation in dense clusters.

Abstract

In compact and dense star-forming clouds a global star cluster wind could be suppressed. In this case the stellar feedback is unable to expel the leftover gas from the cluster. Young massive stars remain embedded into a dense residual gas and stir it moving in the gravitational well of the system. Here we present a self-consistent model for the molecular gas distribution in such young, enshrouded stellar clusters. It is assumed that the cloud collapse terminates and the star formation ceases when a balance between the turbulent pressure and gravity and between the turbulent energy dissipation and regeneration rates is established. These conditions result in an equation that determines the residual gas density distribution that, in turn, allows one to determine the other characteristics of the leftover gas and the star formation efficiency. It is shown that model predictions are in good agreement with several observationally determined properties of cloud D1 in nearby dwarf spheroidal galaxy NGC 5253 and its embedded cluster.