| Issue |
A&A
Volume 670, February 2023
|
|
|---|---|---|
| Article Number | A42 | |
| Number of page(s) | 12 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361/202244347 | |
| Published online | 03 February 2023 | |
L 363-38 b: A planet newly discovered with ESPRESSO orbiting a nearby M dwarf star
1
ETH Zurich, Institute for Particle Physics and Astrophysics,
Wolfgang-Pauli-Strasse 27,
8093
Zurich, Switzerland
e-mail: lia.sartori@phys.ethz.ch
2
Département d’Astronomie, Université de Genève,
Chemin Pegasi 51,
1290
Versoix, Switzerland
3
Space Research Institute, Austrian Academy of Sciences,
Schmiedlstr. 6,
8042
Graz, Austria
Received:
24
June
2022
Accepted:
25
October
2022
Context. Planets around stars in the solar neighbourhood will be prime targets for characterisation with upcoming large space- and ground-based facilities. Since large-scale exoplanet searches will not be feasible with such telescopes, it is crucial to use currently available data and instruments to find possible target planets before next-generation facilities come online.
Aims. We aim to detect new extrasolar planets around stars in the solar neighbourhood via blind radial velocity (RV) searching with ESPRESSO. Our target sample consists of nearby stars (d < 11 pc) with few (<10) or no previous RV measurements.
Methods. We used 31 radial velocity measurements obtained with ESPRESSO at the VLT between December 2020 and February 2022 of the nearby M dwarf star (M★ = 0.21 M⊙, d = 10.23 pc) L 363-38 to derive the orbital parameters of the newly discovered planet. In addition, we used TESS photometry and archival VLT/NaCo high-contrast imaging data to put further constraints on the orbit inclination and the possible planetary system architecture around L 363-38.
Results. We present the detection of a new extrasolar planet orbiting the nearby M dwarf star L 363-38. L 363-38 b is a planet with a minimum mass of mp sin(i) = 4.67 ± 0.43 M⊕ orbiting its star with a period of P = 8.781 ± 0.007 days, corresponding to a semi-major axis of a = 0.048 ± 0.006 AU, which is smaller than the inner edge of the habitable zone. We further estimate a minimum radius of rp sin(i) ≈ 1.55–2.75 R⊕ and an equilibrium temperature of Teq ≈ 330 K.
Conclusions. With this study, we further demonstrate the potential of the state-of-the-art spectrograph ESPRESSO in detecting and investigating planetary systems around nearby M dwarf stars, which were inaccessible to previous instruments such HARPS.
Key words: planets and satellites: detection / techniques: radial velocities / planets and satellites: fundamental parameters / stars: individual: L 363-38
© The Authors 2023
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.
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