Table 1.
Transmission depths, past measurements, and our calculations.
| Source | HAT-P-11 b | GJ 3470 b | GJ 436 b |
|---|---|---|---|
| NO18† | < 0.41% ; < 1.22 | ||
| NI20‡ | 1.5% ; 1.98 | ||
| PA20† | 1.50 ± 0.3% ; 1.98 ± 0.15 | ||
| AL23†, △ | 0.76 ± 0.07% ; 1.75 ± 0.05 | < 0.64% ; < 1.50 | |
| GU24† | 1.36 ± 0.17% ; 2.17 ± 0.11 | 1.75 ± 0.36% ; 2.10 ± 0.17 | < 0.42% ; < 1.22 |
| MA24† | 1.2 ± 0.2% ; 2.1 ± 0.1 | < 0.9% ; < 1.7 | < 0.3% ; < 1.2 |
| kR2, v = 0 | 1.03% ; 1.95 | 1.55% ; 2.01 | 0.39% ; 1.20 |
| kR2, LTEthe | 0.97% ; 1.91 | 1.27% ; 1.87 | 0.32% ; 1.17 |
| kR2, LTEexp, min | 0.92% ; 1.87 | 1.08% ; 1.77 | 0.28% ; 1.15 |
| kR2, LTEexp, max | 0.90% ; 1.85 | 0.93% ; 1.68 | 0.25% ; 1.14 |
| ṁ [g s−1] and kR2, LTEexp, min | 2.0 × 1011 | 5.9 × 1010 | 6.4 × 109 |
Notes. NO18: Nortmann et al. (2018); NI20: Ninan et al. (2020); PA20: Pallé et al. (2020); AL23: Allart et al. (2023); GU24: Guilluy et al. (2024); MA24: Masson et al. (2024). For each bibliographic source/planet, left and right-hand side entries refer to the excess absorption (EA) and the planet’s opaque radius at the line core (Guilluy et al. 2024), respectively. Last row, mass loss rate calculated here for the given setting. †: Opaque radius inferred by us from the EA quoted in the reference, using the planet and star sizes adopted here; ‡: Estimated from their Fig. 5; △: Measured on a 0.75-Å passband.
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