Kossakowski, D, Kemmer, J, Bluhm, P, Stock, S, Caballero, JA, Bejar, VJS, Cardona Guillen, C, Lodieu, N, Collins, KA, Oshagh, M, Schlecker, M, Espinoza, N, Palle, E, Henning, T, Kreidberg, L, Kuerster, M, Amado, PJ, Anderson, DR, Morales, JC, Cartwright, S, Charbonneau, D, Chaturvedi, P, Cifuentes, C, Conti, DM, Cortes-Contreras, M, Dreizler, S, Galadi-Enriquez, D, Guerra, P, Hart, R, Hellier, C, Henze, C, Herrero, E, Jeffers, SV, Jenkins, JM, Jensen, ELN, Kaminski, A, Kielkopf, JF, Kunimoto, M, Lafarga, M, Latham, DW, Lillo-Box, J, Luque, R, Molaverdikhani, K, Montes, D, Morello, G, Morgan, EH, Nowak, G, Pavlov, A, Perger, M, Quintana, EV, Quirrenbach, A, Reffert, S, Reiners, A, Ricker, G, Ribas, I, Lopez, CR, Osorio, MRZ, Seager, S, Schoefer, P, Schweitzer, A, Trifonov, T, Vanaverbeke, S, Vanderspek, R, West, R, Winn, J and Zechmeister, M (2021) TOI-1201 b: A mini-Neptune transiting a bright and moderately young M dwarf. Astronomy and Astrophysics, 656 (A124). ISSN 0004-6361

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Abstract

We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf (J ≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observations. With an orbital period of 2.49 d, TOI-1201 b is a warm mini-Neptune with a radius of Rb = 2.415 ± 0.090 R⊕. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of Mb = 6.28 ± 0.88 M⊕ and, thus, an estimated bulk density of 2.45−0.42+0.48 g cm−3. The spectroscopic observations additionally show evidence of a signal with a period of 19 d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19 d signal to the stellar rotation period (Prot = 19–23 d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is anexcellent target for atmosphere characterization (the transmission spectroscopy metric is 97−16+21) with the upcoming James Webb Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision.

Item Type: Article
Additional Information: Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society.
Uncontrolled Keywords: techniques: photometric; techniques: radial velocities; planetary systems; stars: individual: TOI-1201; stars: individual: TIC-29 960 110; stars: low-mass
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 19 Jan 2022 13:36
Last Modified: 17 Feb 2022 15:58
URI: https://eprints.keele.ac.uk/id/eprint/10515

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