Bibcode
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.
Referencia bibliográfica
Astronomy and Astrophysics
Fecha de publicación:
2
2024
Revista
Número de citas
0
Número de citas referidas
0
Descripción
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.
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.