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Massive stars within young star clusters underpin galaxy evolution physics. Massive stars shape their environments through mechanical feedback, ionisation, and heavy element enrichment of the interstellar medium (ISM). Yet, our understanding of these stars’ chemical composition, especially at low metallicity, remains uncertain. This limits our ability to quantify how they interact with the ISM and the resulting emission line observables. By quantifying chemical abundance ratios over cosmic time and integrating them into stellar and photoionisation models self-consistently, we are starting to accurately predict galaxy properties across epochs. In this presentation, we will merge stellar models with observations of star forming regions, linking the formation of stars to the global galactic environment. We will explore significant knowledge gaps, paving the way to quantify energy, metal, and matter flows on 10 parsec scales. Additionally, we highlight how JWST observations are addressing the disparity between local and high-redshift realms. We’ll end by demonstrating how this work establishes a foundational framework for future investigations with MAVIS, which will enable detailed characterisations of resolved stellar populations beyond our cosmic neighbourhood. |
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