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Table C.4

He I 10 830 Å triplet equivalent width and XUV (5–504 Å) flux at planet distance.

Planet name SpT R* EWa FXUV,He Modelb Mp Rp ρp References (planet data and He observation)
(R⊙) (mÅ) (W m−2) (MJ) (RJ) (g cm−3)
GJ 436 b M2.5V 0.464±0.011 <1.4 0.14±0.02 1 0.067±0.001 0.374±0.010 1.595±0.125 Trifonov et al. (2018); Nortmann et al. (2018)
GJ 1214 b M4.5V 0.216±0.012 33.2±2 8 0.29−0.06+0.08${0.29_{ - 0.06}^{ + 0.08}}$ 1 0.026±0.001 0.245±0.005 2.179±0.170 Cloutier et al. (2021); Orell-Miquel et al. (2022)
GJ 3470 b M1.5V 0.48±0.04 20.7±1.3 2.24−0.17+0.25${2.24_{ - 0.17}^{ + 0.25}}$ 1 0.040±0.004 0.374±0.053 0.940±0.408 Kosiarek et al. (2019); Palle et al. (2020)
HAT-P-11 b K4V 0.683±0.009 12.4±2.4 3.23±0.02 2 0.074±0.005 0.389±0.005 1.551±0.118 Yee et al. (2018); Allart et al. (2018)
HAT-P-18 b K2V 0.717±0.026 29.2±7.6 5.2: 4 0.183±0.034 0.947±0.044 0.267±0.062 Knutson et al. (2014); Paragas et al. (2021)
HAT-P-26 b K1V 0.788±0.043 19.7±6.4 <2.3 2 0.059±0.007 0.570±0.010 0.392±0.052 Hartman et al. (2011); Vissapragada et al. (2022)
HAT-P-32 b F8V 1.387±0.067 114.0±4.0 258.22−133.02+383.18$258.22_{ - 133.02}^{ + 383.18}$ 2 0.750±0.130 1.789±0.025 0.162±0.029 Bonomo et al. (2017); Czesla et al. (2022)
HAT-P-67 b F5IV 2.65±0.12 147±25 361.0: 4 0.320±0.180 2.164±0.010 0.039±0.022 Gully-Santiago et al. (2024)
HD 73583 b K4V 0.71±0.02 7.4±0.6 0.98−0.10+0.11${0.98_{ - 0.10}^{ + 0.11}}$ 1 0.032±0.011 0.249±0.009 2.579±0.904 Barragán et al. (2022); Zhang et al. (2022a)
HD 189733 b K2V 0.805±0.016 12.8±0.4 20.86−1.98+1.20${20.86_{ - 1.98}^{ + 1.20}}$ 1 1.154±0.025 1.138±0.077 0.971±0.198 Paredes et al. (2021); Salz et al. (2018)
HD 209458 b G0V 1.203±0.061 5.3±0.5 1.41−0.16+0.11${1.41_{ - 0.16}^{ + 0.11}}$ 1 0.685±0.017 1.390±0.018 0.316±0.015 Wang & Ford (2011); Alonso-Floriano et al. (2019)
HD 235088 b K2V 0.789±0.022 11.1±1.7 1.88−0.13+0.26${1.88_{ - 0.13}^{ + 0.26}}$ 2 0.022±0.006 0.187±0.018 4.172±1.657 Zhang et al. (2023b); Orell-Miquel et al. (2023)
HD 283636 b K0V 0.636±0.024 8.5±1.6 6.41−2.89+8.09${6.41_{ - 2.89}^{ + 8.09}}$ 2 0.025±0.006 0.205±0.027 3.599±1.664 Zhang et al. (2023b)
KELT-9 b A0V 2.362±0.07 <1.2 0.2: 5 2.880±0.350 1.840±0.040 0.573±0.079 Borsa et al. (2019); Nortmann et al. (2018)
TOI-1268 b K2V 0.92±0.06 17.7±1.9 6.8: 4 0.303±0.026 0.810±0.050 0.707±0.144 Šubjak et al. (2022); Orell-Miquel et al. (2024)
TOI-1420 b G6V 0.923±0.024 42.9±5.1 < 1.4 4 0.079±0.012 1.062±0.027 0.082±0.014 Yoshida et al. (2023); Vissapragada et al. (2024)
TOI-2018 b K4V 0.62±0.01 6.8±1.5 1.4: 4 0.029±0.007 0.203±0.006 4.316±1.062 Dai et al. (2023); Orell-Miquel et al. (2024)
TOI-2076 b K0 0.761±0.016 10.0±0.7 9.91−3.07+2.17${9.91_{ - 3.07}^{ + 2.17}}$ 3 0.028:c 0.293±0.004 1.383: Hedges et al. (2021); Zhang et al. (2023b)
TOI-2134b K5V 0.744±0.027 3.3±0.3 0.19−0.04+0.10${0.19_{ - 0.04}^{ + 0.10}}$ 2 0.029±0.002 0.240±0.014 2.575±0.499 Rescigno et al. (2024); Zhang et al. (2023a)
WASP-12 b G0V 1.657±0.045 <4.0 <236.8 2 1.460±0.270 1.884±0.057 0.271±0.056 Turner et al. (2021); Czesla et al. (2024)
WASP-52 b K2V 0.79±0.02 39.6±1.4 50.67−7.29+8.63${50.67_{ - 7.29}^{ + 8.63}}$ 1 0.460±0.020 1.270±0.030 0.278±0.023 Hébrard et al. (2013); Kirk et al. (2022)
WASP-69 b K4V 0.813±0.028 28.3±0.9 3.33−0.48+1.17${3.33_{ - 0.48}^{ + 1.17}}$ 2 0.260±0.017 1.057±0.047 0.273±0.041 Anderson et al. (2014); Nortmann et al. (2018)
WASP-76b F7IV-V 1.73±0.04 <21.3 <103.4 2 0.920±0.030 1.830±0.060 0.186±0.019 West et al. (2016); Casasayas-Barris et al. (2021)
WASP-107 b K7V 0.66±0.02 87.2±7.6 2.46−1.09+3.12$\matrix{ \hfill {2.46_{ - 1.09}^{ + 3.12}} \cr } $ 2 0.120±0.001 0.940±0.020 0.179±0.012 Anderson et al. (2017); Allart et al. (2019)
WASP-177b K2V 0.885±0.046 6.8±1.6 10.9: 4 0.508±0.038 1.580±0.660 0.160±0.201 Turner et al. (2019); Kirk et al. (2022)
V1298 Tau b K1IV 1.305±0.07 <19.0 34.42−5.28+9.84${34.42_{ - 5.28}^{ + 9.84}}$ 1 0.64±0.19 0.888±0.032 0.886±0.096 Suárez Mascareño et al. (2021); Orell-Miquel et al. (2024)
V1298 Tau c K1IV 1.305±0.07 <95.8 144.08−22.09+41.20${144.08_{ - 22.09}^{ + 41.20}}$ 1 0.062±0.029 0.467±0.021 0.755±0.368 Sikora et al. (2023); Orell-Miquel et al. (2024)
55 Cnc e G8V 0.98±0.016 <0.7 4.53−0.73+1.15${4.53_{ - 0.73}^{ + 1.15}}$ 0.027±0.001 0.174±0.003 6.396±0.492 Crida et al. (2018); Zhang et al. (2021)
GJ 486 b M3.5V 0.328±0.011 <1.9 0.10−0.02+0.05${0.10_{ - 0.02}^{ + 0.05}}$ 1 (944±41)e-5 0.120±0.006 6.809±1.000 Caballero et al. (2022); Masson et al. (2024)
GJ 9827 b K6V 0.651±0.065 <1.9 0.72−0.13+0.22${0.72_{ - 0.13}^{ + 0.22}}$ 1 0.015±0.001 0.136±0.005 7.485±1.022 Kosiarek et al. (2021); Carleo et al. (2021)
GJ 9827 d K6V 0.651±0.065 <1.2 0.08−0.01+0.02${0.08_{ - 0.01}^{ + 0.02}}$ 1 0.011±0.002 0.174±0.007 2.515±0.540 Kosiarek et al. (2021); Carleo et al. (2021)
HD 63433 b G5V 0.912±0.034 <2.0 6.46−0.59+0.65${6.46_{ - 0.59}^{ + 0.65}}$ 1 <0.068:c 0.191±0.007 <12.174 Mallorquín et al. (2023); Zhang et al. (2022b)
HD 63433 c G5V 0.912±0.034 <4.2 1.57−0.14+0.16${1.57_{ - 0.14}^{ + 0.16}}$ 1 0.048±0.013 0.243±0.009 4.181±1.220 Mallorquín et al. (2023); Zhang et al. (2022b)
HD 97658 b K1V 0.73±0.02 <0.9 0.13−0.01+0.02${0.13_{ - 0.01}^{ + 0.02}}$ 1 0.025±0.002 0.200±0.009 3.782±0.558 Van Grootel et al. (2014); Kasper et al. (2020)
K2-100b G0V 1.22±0.02 <5.7 127.72−4.44+8.54${127.72_{ - 4.44}^{ + 8.54}}$ 2 0.069±0.019 0.346±0.014 2.054±0.635 Barragán et al. (2019); Gaidos et al. (2020)
K2-105b G8V 0.91±0.01 <23.3 1.2: 4 0.094±0.060 0.301±0.011 4.275±2.768 Narita et al. (2017); Zhang et al. (2023b)
K2-136c K5V 0.66±0.02 <25.0 0.58−0.21+0.59$0.58_{ - 0.21}^{ + 0.59}$ 2 0.022:c 0.260±0.010 1.552: Mann et al. (2018); Gaidos et al. (2021)
Kepler-25 c F6V 1.31 ±0.02 <18.6 1.5: 4 0.048±0.004 0.465±0.006 0.591±0.060 Mills et al. (2019); Zhang etal. (2023b)
Kepler-68 b G1V 1.24±0.02 <7.2 < 0.8 4 0.024±0.004 0.206±0.065 3.415±3.287 Mills et al. (2019); Zhang etal. (2023b)
TOI-1807b K3V 0.68±0.015 <2.8 207.30±59.90 3 0.008±0.002 0.122±0.009 5.498±1.630 Nardiello et al. (2022); Masson et al. (2024)
TOI-3757 b M0V 0.62±0.01 <73.0 < 12.7 4 0.268±0.028 1.071±0.040 0.271±0.041 Kanodia et al. (2022)
TRAPPIST-1 b M8V 0.119±0.001 <3.5 0.72−0.04+0.03$0.72_{ - 0.04}^{ + 0.03}$ 2 (43.2±2.2)e-4 0.100±0.001 5.429±0.336 Agol et al. (2021); Krishnamurthy et al. (2021)
TRAPPIST-1 e M8V 0.119±0.001 <10.5 0.11±0.01 2 (218±7)e-5 0.082±0.001 4.889±0.264 Agol et al. (2021); Krishnamurthy et al. (2021)
TRAPPIST-1 f M8V 0.119±0.001 <4.1 0.07±0.00 2 (327±10)e-5 0.093±0.001 5.004±0.244 Agol et al. (2021); Krishnamurthy et al. (2021)
WASP-47 d G9V 1.14±0.01 <32.9 1.1: 4 0.041±0.005 0.319±0.004 1.575±0.190 Vanderburg et al. (2017); Zhang et al. (2023b)
WASP-48 b F8IV 1.75±0.09 <25 207.9: 4 0.984±0.085 1.670±0.100 0.262±0.052 Enoch et al. (2011); Bennett et al. (2023)
WASP-80 b K7V 0.63±0.15 <21 1.64−0.14+0.27$1.64_{ - 0.14}^{ + 0.27}$ 2 0.554±0.040 0.952±0.027 0.796±0.089 Triaud et al. (2013); Fossati et al. (2022)
WASP-127b G5V 1.39±0.03 <6.8 < 16.8 2 0.180±0.020 1.370±0.040 0.087±0.012 Lam et al. (2017); dos Santos et al. (2020)

Notes. (a) Equivalent width of the net transmission planetary signal.(b) Model employed to calculate XUV flux (see text): coronal model with (1) and without (2) UV data; X vs. EUV relation (3); X-rays vs Prot relation (4); and blackbody emission (5).(c) No error bars associated with the mass are used in the plot of these objects.

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