Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM

Abstract We investigate the stellar populations and molecular gas properties of a star-forming region within the dwarf irregular (dIrr) galaxy Wolf–Lundmark–Mellote (WLM). Low-metallicity dIrrs like WLM offer a valuable window into star formation in environments that are unlike those of larger, metal-rich galaxies such as the Milky Way. In these conditions, carbon monoxide (CO), typically used to trace molecular clouds, is more easily photodissociated by ultraviolet (UV) radiation, leading to a larger fraction of CO-dark molecular gas, where H 2 exists without detectable CO emission, or CO-dark gas in the form of cold H i . Understanding the molecular gas content and the stellar populations in these star-forming regions provides important information about the role of CO-bright and CO-dark gas in forming stars. Using Hubble Space Telescope imaging across five Wide Field Camera 3 UVIS bands and CO observations from the Atacama Large Millimeter Array, we examine stellar populations within and outside CO cores and the photodissociation region. Our findings indicate similar physical characteristics such as age and mass across the different environments. Assuming 2% of molecular gas is converted to stars, we estimate the molecular gas content and determine that CO-dark gas constitutes a large fraction of the molecular reservoir in WLM. These results are consistent with molecular gas estimates using a previous dust-derived CO-to-H 2 conversion factor ( α CO ) for WLM. These findings highlight the critical role of CO-dark gas in low-metallicity star formation.