Table 6
Compilation (possibly incomplete) of Hα and He I λ10833 transmission line contrasts, listed in order of ascending effective host star temperature.
| System | Teff (a) (K) | a(a) (10−2 au) | Mp (a) (MJup) | Rp (a) (RJup) | ρp (ρJup) | C(Hα) | C(He Iλ10833) | Refs. (b) |
|---|---|---|---|---|---|---|---|---|
| GJ 3470 | 3600 | 3.6 | 0.04 | 0.37 | 0.84 | 1.5 ± 0.3% | 1 | |
| WASP-107 | 4430 | 5.5 | 0.12 | 0.97 | 0.13 | 7.26 ± 0.24% | 2 | |
| WASP-69 | 4700 | 4.5 | 0.26 | 1.06 | 0.22 | 3.6 ± 0.2% | 3 | |
| HAT-P-11 | 4780 | 5.3 | 0.08 | 0.42 | 1.10 | 1.2% | 4 | |
| HAT-P-18 | 4803 | 5.6 | 0.20 | 0.99 | 0.20 | 0.46 ± 0.12% (c) | 5 | |
| WASP-52 | 5000 | 2.7 | 0.46 | 1.27 | 0.22 | 0.86 ± 0.13% | 6 | |
| HD 189733 | 5040 | 3.1 | 1.14 | 1.14 | 0.78 | 1.9%(d) | 1.04 ± 0.09% | 7 |
| HD 209458 | 6065 | 4.7 | 0.69 | 1.36 | 0.27 | 0.9 ± 0.1% | 8 | |
| HAT-P-32 | 6269 | 3.4 | 0.59 | 1.79 | 0.11 | 3.3% | 5.3% | TW (e) |
| WASP-12 | 6300 | 2.3 | 1.36 | 1.79 | 0.24 | 6%(f) | 9 | |
| WASP-121 | 6460 | 2.5 | 1.18 | 1.81 | 0.20 | 1.87 ± 0.11% | 10 | |
| WASP-33 | 7430 | 2.6 | 2.8 | 1.60 | 0.84 | 0.99 ± 0.05% | 11 | |
| KELT-20 | 8720 | 5.4 | 1.00 | 1.78 | 0.18 | 0.6 ± 0.1% | 12 | |
| KELT-9 | 10170 | 3.4 | 2.88 | 1.94 | 0.40 | 1.15% | 13 |
Notes. (a)Values in columns two through five adopted from exoplanets.org (Han et al. 2014). (b)If more than one reference is given, the listed results refer to the first one. (c)In 6.35 Å band. (d)Estimated from Jensen et al. (2012) (Fig. 3), detection controversial. (e)For this work (TW), the contrast is time variable. We here quote the numbers estimated from the phenomenological model in Sect. 6.3. (f) Estimated from Jensen et al. (2018) (Fig. 9).
References. (1) Palle et al. (2020), Ninan et al. (2020); (2) Kirk et al. (2020), Allart et al. (2019), Kasper et al. (2020); (3) Nortmann et al. (2018), Vissapragada et al. (2020); (4) Allart et al. (2018); (5) Paragas et al. (2021); (6) Chen et al. (2020); (7) Salz et al. (2018), Guilluy et al. (2020), Jensen et al. (2012), Barnes et al. (2016), Cauley et al. (2015), Cauley et al. (2016), Cauley et al. (2017), Kohl et al. (2018); (8) Alonso-Floriano et al. (2019b); (9) Jensen et al. (2018); (10) Cabot et al. (2020), Borsa et al. (2021); (11) Yan et al. (2021b), Cauley et al. (2021), Borsa et al. (2021); (12) Casasayas-Barris et al. (2019), Casasayas-Barris et al. (2018); (13) Yan & Henning (2018), Cauley et al. (2019), Wyttenbach et al. (2020);
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