JWST Observations of Starbursts: Molecular Hydrogen Excitation and Disequilibrium in M82

TL;DR

This study uses JWST MIRI/MRS observations of M82 to analyze molecular hydrogen excitation, revealing non-equilibrium conditions, shock-heating effects, and the thermal history of molecular gas in a starburst environment.

Contribution

It extends H$_2$ temperature models to include dust extinction and OPR disequilibrium, providing spatially resolved insights into heating processes in M82.

Findings

H$_2$ temperature distribution slope anti-correlates with shock indicators.

OPR is about half of equilibrium, indicating rapid heating and mixing.

Models reveal non-equilibrium conditions and recent heating events.

Abstract

Emission from the pure rotational transitions of H$_2$ traces warm molecular gas, providing insight into its temperature distribution and local heating conditions. We have extended previous power-law H$_2$ temperature models to account for differential extinction by dust as well as non-equilibrium ortho-to-para-H$_2$ ratios (OPR). The turbulent environment of the M82 starburst offers a unique opportunity to study H$_2$ out of equilibrium conditions, using ~15 pc spatially resolved measurements from MIRI/MRS on JWST. With extensive detections of H$_2$ S(1)-S(7), we use our model to assess spatial variations in local heating conditions of molecular gas across a ~500 pc region of the M82 central starburst. The average slope of the recovered H$_2$ power law temperature distribution is consistent with prior studies, and the slope strongly anti-correlates with relative [Fe II]/H$_2$ S(1)-S(2) strength, pointing to the importance of shock-heating. Our models indicate that the OPR is, on average, about half of its equilibrium value. This suppression is attributed to cloud mixing timescales which are short compared to timescales for spin conversion, with molecular gas remembering its ''cooler past''. By accounting for OPR disequilibrium, we can identify instances of recent and rapid heating to better understand the flow of energy through the interstellar medium and track its thermal history.