Abstract HATS-75 b is one of the recently discovered Giant Exoplanets Around M-dwarf Stars (GEMS) with a transmission spectrum shaped by both its atmosphere and the active stellar surface it transits. As part of a JWST program studying seven GEMS, we observed three transits of HATS-75 b with the NIRSpec PRISM instrument (0.6–5.3 μ m). The planet’s spectra exhibit a slightly larger transit depth at shorter wavelengths, indicative of hazes or stellar contamination due to stellar heterogeneities outside the transit chord, i.e., the transit light source (TLS) effect. While both a hazy atmospheric model or TLS model can replicate the transmission spectrum, independent evidence (e.g., stellar rotation, spot-crossing events) favors a model that includes contamination from unocculted starspots and faculae. Within this stellar heterogeneity/TLS-based framework, atmospheric retrievals yield remarkably low atmospheric metallicity ( log M / H = − 1.7 4 − 0.76 + 0.92 ) and supersolar carbon-to-oxygen ( C / O = 1.0 4 − 0.09 + 0.40 ), which paired with a best-fit interior model with bulk metallicity of Z p = 0.20 ± 0.04 implies poor vertical mixing within the planet. Retrievals also detect robust absorption signatures of CH 4 , CO, and CO 2 . We obtain only an upper limit for H 2 O, consistent with its atmospheric spectral features being masked by stellar contamination. These results underscore the importance of accounting for stellar heterogeneity when interpreting exoplanet transmission spectra and highlight HATS-75 b as a significant asset to our understanding of giant exoplanets around M dwarfs with JWST.
Ashtari et al. (2026) studied this question.