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Table 3

Properties of the systems for which either measurements or non-detections of the He I metastable triplet have been published.

Planet Teff Rs XUV flux Mp Rp a Teq δHe I Upper
[K] [R⊙] [erg cm−2 s−1] [MJ] [RJ] [AU] [K] [Rp] limit
WASP-80b 4150 ± 1001 0.586 ± 0.0182 62813 0.538 ± 0.0362 0.999 ± 0.0312 0.03442 816 ± 20 0.03127 0.113 Y
HD 209458b 6065 ± 501 1.178 ± 0.0094 24075 0.682 ± 0.0151 1.359 ± 0.0191 0.047071 1463 ± 12 0.01345 0.295 N
HD 189733b 5040 ± 501 0.78 ± 0.024 280956 1.123 ± 0.0451 1.138 ± 0.0271 0.0311 1219 ± 13 0.02152 0.167,8 N
WASP-107b 4425 ± 709 0.67 ± 0.029 632310 0.096 ± 0.0059 0.94 ± 0.0211 0.05511 757 ± 12 0.01990 0.9912,13 N
WASP-69b 4700 ± 501 0.818 ± 0.0254 619214,15,16 0.250 ± 0.0231 1.057 ± 0.0471 0.045271 963 ± 11 0.01688 0.7716 N
GJ436b 3479 ± 6017 0.449 ± 0.01917 242818 0.080 ± 0.00719 0.366 ± 0.01419 0.030819 641 ± 11 0.00672 0.2716 Y
KELT9b 9600 ± 40020 2.418 ± 0.05820 317421 2.88 ± 0.3520 1.936 ± 0.04720 0.0336820 3922 ± 165 0.00648 0.2316 Y
GJ3470b 3652 ± 5022 0.48 ± 0.0422 562123 0.040 ± 0.00422 0.346 ± 0.02922 0.034824 654 ± 10 0.00525 0.9625 N
GJ9827b 4340 ± 5026 0.647 ± 0.084 3681027 0.0154 ± 0.001526 0.1407 ± 0.002826 0.018826 1228 ± 26 0.00048 0.7627 Y
GJ9827d 4340 ± 5026 0.647 ± 0.084 416227 0.0127 ± 0.002626 0.1804 ± 0.004126 0.055926 712 ± 11 0.00079 1.9427 Y
HAT-P-11b 4780 ± 5028 0.769 ± 0.0484 323629 0.0736 ± 0.004730 0.389 ± 0.00530 0.0525430 882 ± 11 0.00259 1.2731,32 N
HAT-P-18b 4803 ± 801 0.73 ± 0.044 800033 0.200 ± 0.0191 0.995 ± 0.0521 0.055961 837 ± 14 0.01878 0.1233 N
55 Cnc e 5196 ± 2434 0.95 ± 0.084 741329 0.0251 ± 0.00135 0.1673 ± 0.002635 0.0154435 1965 ± 33 0.00031 0.3436 Y
GJ1214b 3250 ± 10037 0.221 ± 0.00437 85129 0.0197 ± 0.002738 0.254 ± 0.01838 0.0141138 621 ± 19 0.01332 1.1039 Y
HD 63433b 5640 ± 7440 0.912 ± 0.03440 2282641 − 0.192 ± 0.00940 0.071940 969 ± 13 0.00045 2.4941 Y
HD 63433c 5640 ± 7440 0.912 ± 0.03440 555141 − 0.2418 ± 0.012540 0.145840 680 ± 9 0.00071 1.8341 Y
WASP-12b 6250 ± 1001 1.57 ± 0.254 1399415,29 1.39 ± 0.121 1.825 ± 0.0911 0.023121 2484 ± 88 0.01366 0.0142 Y
Trappist-1b 2559 ± 5043 0.117 ± 0.003643 167444 0.0032 ± 0.000545 0.100 ± 0.00345 0.0115545 393 ± 8 0.00739 0.0446 Y
Trappist-1e 2559 ± 5043 0.117 ± 0.003643 26044 0.0024 ± 0.000345 0.0812 ± 0.002545 0.0292845 247 ± 5 0.00487 0.0746 Y
Trappist-1f 2559 ± 5043 0.117 ± 0.003643 15044 0.0029 ± 0.000245 0.0933 ± 0.002745 0.0385345 215 ± 4 0.00643 0.0246 Y
WASP-76b 6316 ± 6447 1.77 ± 0.0747 910515,48 0.92 ± 0.0349 1.83 ± 0.0549 0.03349 2231 ± 27 0.01081 0.3548 Y
HAT-P-32b 6269 ± 6450 1.219 ± 0.01651 42000052 0.585 ± 0.03151 1.789 ± 0.02551 0.034351 1816 ± 19 0.02177 1.0252 N

Notes. The fourth column lists the XUV stellar flux at wavelengths shorter than 912 Å impinging on the planet. Column ten gives the effective absorption of the He I triplet.

References. 1. Bonomo et al. (2017); 2. Triaud et al. (2015); 3. This work; 4. Gaia Collaboration (2018); 5. Alonso-Floriano et al. (2019); 6. Bourrier et al. (2020); 7. Salz et al. (2018); 8. Guilluy et al. (2020); 9. Piaulet et al. (2021); 10. Khodachenko et al. (2021a); 11. Anderson et al. (2017); 12. Allart et al. (2019); 13. Kirk et al. (2020); 14. Figueira et al. (2014); 15. Sreejith et al. (2020); 16. Nortmann et al. (2018); 17. Bourrier et al. (2018c); 18. Bourrier et al. (2016); 19. Lanotte et al. (2014); 20. Borsa et al. (2019); 21. Fossati et al. (2018); 22. Kosiarek et al. (2019); 23. Bourrier et al. (2021); 24. Bonfils et al. (2012); 25. Palle et al. (2020); 26. Rice et al. (2019); 27. Carleo et al. (2021); 28. Bakos et al. (2010); 29. Salz et al. (2016); 30. Yee et al. (2018); 31. Allart et al. (2018); 32. Mansfield et al. (2018); 33. Paragas et al. (2021); 34. von Braun et al. (2011); 35. Bourrier et al. (2018a); 36. Zhang et al. (2021); 37. Gillon et al. (2014); 38. Harpsøe et al. (2013); 39. Crossfield et al. (2019); 40. Mann et al. (2020); 41. Zhang et al. (2022); 42. Kreidberg & Oklopčić (2018); 43. Gillon et al. (2017); 44. Bourrier et al. (2017); 45. Grimm et al. (2018); 46. Krishnamurthy et al. (2021); 47. Tabernero et al. (2021); 48. Casasayas-Barris et al. (2021); 49. Ehrenreich et al. (2020); 50. Zhao et al. (2014); 51. Hartman et al. (2011); 52. Czesla et al. (2022).

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