Retrieval results of the Cassini/VIMS occultation of Titan, with both the temperature profile and methane retrieved. The reference values in the posteriors are from the same source as in Figure B.1. This setup would be more representative of an exoplanet approach where the priors on the thermal structure and chemistry are unknown. The spectral fit and retrieved chemistry match the results from the main text. However, we obtain inconsistent results for the aerosol solution and the T - p profiles. For the T - p profile, in particular, the retrieved solution does not match the known truth for Titan’s atmosphere. Such degeneracies are expected for exoplanet transit retrievals where obtaining robust T - p structure remains difficult (Rocchetto et al. 2016; Schleich et al. 2024). This is especially true for cases involving secondary and cloudy atmosphere (see e.g., Changeat et al. 2020b; Di Maio et al. 2023).