Molecular Hydrogen in the Extremely Metal-Poor, Star-Forming Galaxy Leo P

TL;DR

This paper reports the first detection of molecular hydrogen in the extremely metal-poor galaxy Leo P using JWST, providing new insights into star formation processes at very low metallicities in the early universe.

Contribution

It demonstrates JWST's capability to detect molecular gas in galaxies with only 3% solar metallicity, challenging previous assumptions about star formation in such environments.

Findings

Detected molecular hydrogen emission in Leo P at 3% solar metallicity.

Established JWST's sensitivity to low molecular gas masses at low metallicity.

Extended the metallicity range where molecular gas fueling star formation is observed.

Abstract

The James Webb Space Telescope (JWST) has revealed unexpectedly rapid galaxy assembly in the early universe, in tension with models of star and galaxy formation. In the gas conditions typical of early galaxies, particularly their low abundances of heavy elements (metals) and dust, the star-formation process is poorly understood. Some models predict that stars form in atomic gas at low metallicity, in contrast to forming in molecular gas as observed in higher-metallicity galaxies. To understand the very high star-formation rates at early epochs, it is necessary to determine whether molecular gas formation represents a bottleneck to star formation, or if it is plentiful even at extremely low metallicity. Despite repeated searches, star-forming molecular gas has not yet been observed in any galaxy below 7% of the Solar metallicity, leaving the question of how stars form at lower metallicities unresolved. Here, we report the detection of rotationally excited emission from molecular hydrogen in the star-forming region of the nearby, 3% Solar metallicity galaxy Leo P with the MIRI-MRS instrument onboard JWST. These observations place a lower limit on the molecular gas content of Leo P and, combined with our upper limit on carbon monoxide emission from a deep search of this galaxy, demonstrate that MIRI-MRS is sensitive to much smaller molecular gas masses at extremely low metallicity compared to the traditional observational tracer. This discovery pushes the maximum metallicity at which purely atomic gas may fuel star formation a factor of two lower, providing crucial empirical guidance for models of star formation in the early universe.