Validation and atmospheric exploration of the sub-Neptune TOI-2136b around a nearby M3 dwarf

Kawauchi, Kiyoe; Murgas, F.; Πάλλη, Ε.; Narita, Norio; Fukui, A.; Hirano, Teruyuki; Parviainen, H.; Ishikawa, Hiroyuki; Watanabe, Noriharu; Esparaza-Borges, E.; Kuzuhara, Masayuki; Orell-Miquel, J.; Krishnamurthy, Vigneshwaran; Mori, M.; Kagetani, Taiki; Zou, Y.; Isogai, Keisuke; Livingston, John H.; Howell, Steve B.; Crouzet, Nicolas; Leon, Jerome de; Kimura, Tadahiro; Kodama, Takanori; Korth, J.; Kurita, S.; Laza-Ramos, A.; Luque, R.; Madrigal-Aguado, A.; Miyakawa, Kohei; Morello, Giuseppe; Nishiumi, Taku; Rodríguez, G. E. Fernández; Sánchez-Benavente, Manuel; Stangret, M.; Teng, Huan-Yu; Terada, Yuka; Gnilka, Crystal L.; Guerrero, Natalia; Harakawa, Hiroki; Hodapp, Klaus W.; Hori, Yasunori; Ikoma, Masahiro; Jacobson, Shane; Konishi, Mihoko; Kotani, Takayuki; Kudo, Tomoyuki; Kurokowa, T.; Kusakabe, Nobuhiko; Nishikawa, Jun; Omiya, Masashi; Serizawa, Takuma; Tamura, Motohide; Ueda, Akitoshi; Vievard, Sébastien

doi:10.1051/0004-6361/202243381

Cited by 6 publications

(1 citation statement)

References 98 publications

(72 reference statements)

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“…To date, more than 30 planets have been investigated for the 10833 Å helium line. Of these, most have been nondetections (e.g., Kasper et al 2020;Krishnamurthy et al 2021;Vissapragada et al 2021;Zhang et al 2021;Kawauchi et al 2022), but there have been many detections as well (e.g., Allart et al 2018;Nortmann et al 2018;Salz et al 2018;Ninan et al 2020;Paragas et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Nondetection of Helium in the Hot Jupiter WASP-48b

Bennett

Redfield

Oklopčić

et al. 2023

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Hot Jupiters orbiting extremely close to their host star may experience atmospheric escape due to the large amounts of high-energy radiation they receive. Understanding the conditions under which this occurs is critical, as atmospheric escape is believed to be a driving factor in sculpting planetary populations. In recent years, the near-infrared 10833 Å helium feature has been found to be a promising spectral signature of atmospheric escape. We use transmission spectroscopy to search for excess helium absorption in the extended atmosphere of WASP-48b, a hot Jupiter orbiting a slightly evolved, rapidly rotating F star. The data were collected using the Habitable-zone Planet Finder spectrograph on the Hobby–Eberly Telescope. Observations were taken over the course of seven nights, from which we obtain three transits. No detectable helium absorption is seen, as absorption depth is measured to −0.0025 ± 0.0021, or 1.2σ from a null detection. This nondetection follows our current understanding of decreasing stellar activity (and thus high-energy radiation) with age. We use a 1D isothermal Parker wind model to compare with our observations and find that our nondetection can best be explained with a low planetary mass-loss rate and high thermosphere temperature. We explore our results within the context of the full sample of helium detections and nondetections to date. Surprisingly, comparing helium absorption with the stellar activity index log R HK ′ reveals a large spread in the correlation between these two factors, suggesting that there are additional parameters influencing the helium absorption strength.

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Section: Introductionmentioning

confidence: 99%

Nondetection of Helium in the Hot Jupiter WASP-48b

Bennett

Redfield

Oklopčić

et al. 2023

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Chemical conditions on Hycean worlds

Madhusudhan,

Moses,

Rigby

et al. 2023

Faraday Discuss.

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TOI-1442 b and TOI-2445 b: Two potentially rocky ultra-short period planets around M dwarfs

Morello¹,

Parviainen²,

Murgas³

et al. 2023

A&A

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Context. Exoplanets with orbital periods of less than one day are known as ultra-short period (USP) planets. They are relatively rare products of planetary formation and evolution processes, but especially favourable for characterisation with current planet detection methods. At the time of writing, 125 USP planets have already been confirmed. Aims. Our aim is to validate the planetary nature of two new transiting planet candidates around M dwarfs announced by the NASA Transiting Exoplanet Survey Satellite (TESS), registered as TESS Objects of Interest (TOIs) TOI-1442.01 and TOI-2445.01. Methods. We used TESS data, ground-based photometric light curves, and Subaru/IRD spectrograph radial velocity (RV) measurements to validate both planetary candidates and to establish their physical properties. Results. TOI-1442 b is a validated exoplanet with an orbital period of P = 0.4090682 ± 0.0000004 d, a radius of R p = 1.15 ± 0.06 R ⊕ , and equilibrium temperature of T p,eq = 1357 +49−42 K. TOI-2445 b is also validated with an orbital period of P = 0.3711286 ± 0.0000004 d, a radius of R p = 1.33 ± 0.09 R ⊕ , and equilibrium temperature of T p,eq = 1330 +61−56 K. Their physical properties align with current empirical trends and formation theories of USP planets. Based on the RV measurements, we set 3σ upper mass limits of 8 M ⊕ and 20 M ⊕ , thus confirming the non-stellar, sub-Jovian nature of both transiting objects. More RV measurements will be needed to constrain the planetary masses and mean densities, and the predicted presence of outer planetary companions. These targets extend the small sample of USP planets orbiting around M dwarfs up to 21 members. They are also among the 20 most suitable terrestrial planets for atmospheric characterisation via secondary eclipse with the James Webb Space Telescope, according to a widespread emission spectroscopy metric.

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Validation and atmospheric exploration of the sub-Neptune TOI-2136b around a nearby M3 dwarf

Cited by 6 publications

References 98 publications

Nondetection of Helium in the Hot Jupiter WASP-48b

Nondetection of Helium in the Hot Jupiter WASP-48b

Chemical conditions on Hycean worlds

TOI-1442 b and TOI-2445 b: Two potentially rocky ultra-short period planets around M dwarfs

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