The GAPS programme at TNG: L. TOI-4515 b: An eccentric warm Jupiter orbiting a 1.2 Gyr-old G-star

Carleo, I.; Malavolta, L.; Desidera, S.; Nardiello, D.; Wang, S.; Turrini, D.; Lanza, A. F.; Baratella, M.; Marzari, F.; Benatti, S.; Biazzo, K.; Bieryla, A.; Brahm, R.; Bonavita, M.; Collins, K. A.; Hellier, C.; Locci, D.; Hobson, M. J.; Maggio, A.; Mantovan, G.; Messina, S.; Pinamonti, M.; Rodriguez, J. E.; Sozzetti, A.; Stassun, K.; Wang, X. Y.; Ziegler, C.; Damasso, M.; Giacobbe, P.; Murgas, F.; Parviainen, H.; Andreuzzi, G.; Barkaoui, K.; Berlind, P.; Bignamini, A.; Borsa, F.; Briceño, C.; Brogi, M.; Cabona, L.; Calkins, M. L.; Capuzzo-Dolcetta, R.; Cecconi, M.; Colon, K. D.; Cosentino, R.; Dragomir, D.; Esquerdo, G. A.; Henning, T.; Ghedina, A.; Goeke, R. F.; Gratton, R.; Horta, F. Grau; Gupta, A. F.; Jenkins, J. M.; Jordán, A.; Knapic, C.; Latham, D. W.; Mireles, I.; Law, N.; Lorenzi, V.; Lund, M. B.; Maldonado, J.; Mann, A. W.; Molinari, E.; Pallé, E.; Paegert, M.; Pedani, M.; Quinn, S. N.; Scandariato, G.; Seager, S.; Winn, J. N.; Wohler, B.; Zingales, T.

Abstract

Context. Different theories have been developed to explain the origins and properties of close-in giant planets, but none of them alone can explain all of the properties of the warm Jupiters (WJs, Porb = 10–200 days). One of the most intriguing characteristics of WJs is that they have a wide range of orbital eccentricities, challenging our understanding of their formation and evolution.

Aims. The investigation of these systems is crucial in order to put constraints on formation and evolution theories. TESS is providing a significant sample of transiting WJs around stars bright enough to allow spectroscopic follow-up studies.

Methods. We carried out a radial velocity (RV) follow-up study of the TESS candidate TOI-4515 b with the high-resolution spectrograph HARPS-N in the context of the GAPS project, the aim of which is to characterize young giant planets, and the TRES and FEROS spectrographs. We then performed a joint analysis of the HARPS-N, TRES, FEROS, and TESS data in order to fully characterize this planetary system.

Results. We find that TOI-4515 b orbits a 1.2 Gyr-old G-star, has an orbital period of Pb = 15.266446 ± 0.000013 days, a mass of Mb = 2.01 ± 0.05 MJ, and a radius of Rb = 1.09 ± 0.04 RJ. We also find an eccentricity of e = 0.46 ± 0.01, placing this planet among the WJs with highly eccentric orbits. As no additional companion has been detected, this high eccentricity might be the consequence of past violent scattering events.

• Journal Article Type: Article
• Acceptance Date: Nov 13, 2023
• Online Publication Date: Feb 14, 2024
• Publication Date: 2024-02
• Deposit Date: May 10, 2024
• Journal: Astronomy & Astrophysics
• Print ISSN: 0004-6361
• Electronic ISSN: 1432-0746
• Publisher: EDP Sciences
• Peer Reviewed: Peer Reviewed
• Volume: 682
• Article Number: A135
• DOI: https://doi.org/10.1051/0004-6361/202348207
• Public URL: https://keele-repository.worktribe.com/output/825920
• Publisher URL: https://www.aanda.org/articles/aa/full_html/2024/02/aa48207-23/aa48207-23.html