Synthetic in-transit spectra based on the MUS-a, MUS-b, X-Exo-a, X-Exo-b, MUS-b-RD82, and MUS-b-FA98 models. Thin and thick lines refer to -a and -b models, respectively (see text for details). The spectra were calculated following standard methods (García Muñoz & Schneider 2019), with which we obtain the wavelength-dependent effective radius, R_λ. The excess absorption is defined as EA=((R_λ/R_⋆)²−(R_p/R_⋆)²)×100, with R_p being the planet’s optical radius and R_⋆ the stellar radius. Also shown is the nondetection upper limit reported by Masson et al. (2024). Nortmann et al. (2018) and Guilluy et al. (2024) report upper limits of 0.41 and 0.42%, respectively.