Assessing Radiation Pressure as a Feedback Mechanism in Star-Forming Galaxies

TL;DR

This study evaluates the role of radiation pressure on dust as a feedback mechanism in star-forming galaxies, suggesting it influences star formation regulation and correlates with key galactic properties.

Contribution

It provides a comprehensive analysis linking radiation pressure to star formation laws and introduces a new interpretation of the Schmidt Law and related correlations.

Findings

Radiation pressure sets an upper luminosity limit for star-forming regions.

Many normal galaxies are below the Eddington luminosity, indicating other factors at play.

Gas depletion timescale in dense regions aligns with observed starburst durations.

Abstract

Radiation pressure from the absorption and scattering of starlight by dust grains may be an important feedback mechanism in regulating star-forming galaxies. We compile data from the literature on star clusters, star-forming subregions, normal star-forming galaxies, and starbursts to assess the importance of radiation pressure on dust as a feedback mechanism, by comparing the luminosity and flux of these systems to their dust Eddington limit. This exercise motivates a novel interpretation of the Schmidt Law, the LIR-L'CO correlation, and the LIR-L'HCN correlation. In particular, the linear LIR-L'HCN correlation is a natural prediction of radiation pressure regulated star formation. Overall, we find that the Eddington limit sets a hard upper bound to the luminosity of any star-forming region. Importantly, however, many normal star-forming galaxies have luminosities significantly below the Eddington limit. We explore several explanations for this discrepancy, especially the role of "intermittency" in normal spirals - the tendency for only a small number of subregions within a galaxy to be actively forming stars at any moment because of the time-dependence of the feedback process and the luminosity evolution of the stellar population. If radiation pressure regulates star formation in dense gas, then the gas depletion timescale is 6 Myr, in good agreement with observations of the densest starbursts. Finally, we highlight the importance of observational uncertainties - namely, the dust-to-gas ratio and the CO-H2 and HCN-H2 conversion factors - that must be understood before a definitive assessment of radiation pressure as a feedback mechanism in star-forming galaxies.