Table 2
Results combined.
| Target | c | Significance | Effective radius | 𝑔P | H |  |
|---|---|---|---|---|---|---|
| [%] | [σ] | [Rp] | [m s−2] | [km] | ||
| WASP-69b | 3.91 ± 0.22 | 17.6 | 1.79 ± 0.08 | 5.8 ± 0.6 | 1060 | 56 ± 8 |
| WASP-69 b (without 24 July 2019) | 3.46 ± 0.32 | 10.7 | 1.71 ± 0.08 | 5.8 ± 0.6 | 1060 | 51 ± 8 |
| WASP-107 b (1 night) |  |
10.5 | 2.19 ± 0.11 | 3.37 ± 0.31 | 1450 | 55 ± 7 |
| HAT-P-11 b | 1.36 ± 0.17 | 8.0 | 2.17 ± 0.11 | 10.2 ± 0.6 | 530 | 71 ± 9 |
| GJ 436 b | <0.42(0.52)(+) | <1.27(1.33) | 14.8 ± 1.7 | 294 | <24(29) | |
| GJ 3470 b (1 night) |  |
4.7 | 2.05 ± 0.25 | 8.2 ± 1.6 | 470 | 55 ± 19 |
Notes. From left to right: the investigated target, the contrast from the DE-MCMC analysis, the significance of the detection, the effective He I radius, the planet’s gravity, the atmospheric scale height (computed by assuming a mean molecular weight of 1.3), and the ratio between the equivalent height of the He I atmosphere and the atmospheric scale height. (+)1 σ(2σ) upper limits. For WASP-69 b, we also present results by excluding the first observing night (i.e. 24 July 2019), as it was likely affected by stellar contamination.
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