The MOPYS project: A survey of 70 planets in search of extended He I and H atmospheres - No evidence of enhanced evaporation in young planets

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Volume 689 (September 2024)

A&A, 689 (2024) A179

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Table 2

Compilation of Hα and He I observations from high-resolution spectroscopy facilities of young (≲1 Gyr) transiting exoplanets, from the literature and this work (Sect. 3).

Planet	Hα(%)	He I(%)	Planet	Hα (%)	He I (%)
MASCARA-2b	0.85 ± 0.03⁽¹⁾	<0.5	TOI-2046 b	<5	<2.4

K2-100 b	<1.4	<1.3	TOI-1807 b	<0.95	<0.80
		≲1.2⁽²⁾			≲0.4⁽⁸⁾

TOI-1431 b	<0.33⁽³⁾	<0.4	TOI-2048 b	<1.5	<1.0

HD 63433 b	<0.4	<0.4	HD 63433 c	<0.4	<0.4
		≲0.5⁽⁴⁾		–	≲0.5⁽⁴⁾

HD 73583 b	≲0.5	0.72±0.08 ^(5,6)	HD 73583 c	≲0.5	<0.5

HD 235088 b	×⁽⁷⁾	0.91±0.11⁽⁷⁾	TOI-2076 b	<0.7	≲1
		0.64±0.06⁽⁶⁾			1.01 ±0.05⁽⁶⁾

V1298 Taub	–	≲1.7⁽²⁰⁾	V1298 Tau c	<1.1	<3.7

TOI-1268 b	–	${2.00}_{- 0.16}^{+ 0.15}$ $2.00_{ - 0.16}^{ + 0.15}$	TOI-1136 d	${1.12}_{- 0.13}^{+ 0.12}$ $1.12_{ - 0.13}^{ + 0.12}$	<0.5

WASP-189 b	0.13±0.02⁽⁹⁾	<0.3	HAT-P-57 b	<0.7±0.2⁽⁹⁾	<1

K2-77b	<2.5	<2.7	K2-25 b	–	<1.7⁽¹²⁾

AU Mic b	×⁽¹³⁾	<0.34⁽¹⁴⁾	K2-136 c	–	<2.3⁽¹⁸⁾

DS Tuc b	×⁽¹⁶⁾	–	WASP-52b	0.86±0.13⁽¹⁷⁾	3.44±0.31⁽¹⁸⁾

HAT-P-70 b	1.56±0.15⁽¹⁹⁾	–	WASP-8Ob	–	<0.85⁽²¹⁾

KELT-9b	1.15±0.05⁽¹⁰⁾	<0.33⁽¹¹⁾

TOI-2018 b^(†)	<l.5	${1.02}_{- 0.22}^{+ 0.19}$ $1.02_{ - 0.22}^{ + 0.19}$	TOI-1683b^(†)	–	<0.7
					0.84±0.17⁽⁶⁾

Notes. A cross (×) indicates when the stellar activity prevented to measure any planetary absorption or derive upper limits. ^(†)TOI-2018 b and TOI-1683 b are included in the table, but they are likely not young planets.⁽¹⁾ Casasayas-Barris et al. (2019).⁽²⁾ EW at 99% confidence of 5.7mÅ (Gaidos et al. 2020a).⁽³⁾ Stangret et al. (2021).⁽⁴⁾ Zhang et al. (2022c).⁽⁵⁾ Zhang et al. (2022b).⁽⁶⁾ Zhang et al. (2023b).⁽⁷⁾ Orell-Miquel et al. (2023). ⁽⁸⁾EW at 99% confidence of 4 m Å (Gaidos et al. 2023). ⁽⁹⁾Stangret et al. (2022).⁽¹⁰⁾ Yan & Henning (2018).⁽¹¹⁾ Nortmann et al. (2018).⁽¹²⁾ EW at 99% confidence of 17 mÅ (Gaidos et al. 2020b).⁽¹³⁾ Palle et al. (2020b).⁽¹⁴⁾ EW at 99% confidence of 3.7 mÅ (Hirano et al. 2020).⁽¹⁵⁾ EW at 99% confidence of 25 mÅ (Gaidos et al. 2021).⁽¹⁶⁾ Benatti et al. (2021).⁽¹⁷⁾ Chen et al. (2020).⁽¹⁸⁾ Kirk et al. (2022).⁽¹⁹⁾ Bello-Arufe et al. (2022).⁽²⁰⁾ Gaidos et al. (2022).⁽²¹⁾ Fossati et al. (2022).

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