Abstract Temperate ( T eq C / H = 1 3 − 12 + 78 × solar, although the absence of detectable CO and CO 2 at the current precision disfavors metallicities ≳50 × solar. We also tested several haze prescriptions (Titan-like tholin, soot, and water-rich tholin), but the preference for these models is weak (Bayes factors of ∼2 relative to the clear case). The spectrum also shows an increase in transit depth near 3 μ m, which our self-consistent models attribute to either NH 3 or, less likely, HCN. Follow-up observations could distinguish between these species, helping determine the planet’s vertical mixing regime. The TOI-199 system exhibits strong transit timing variations (TTVs) due to an outer non-transiting giant planet. For planet c, our TTV analysis reduces its mass uncertainty by 50% and prefers a slightly longer orbital period (but still within the conservative habitable zone) and higher eccentricity relative to previous studies. TOI-199 b serves as the first data point for studying clouds and hazes in temperate gas giants, with the detection of spectral features in its transmission spectrum indicating that temperate gas giants are promising targets for detailed atmospheric characterization.
Bello-Arufe et al. (Wed,) studied this question.
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