Author:
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.,Grau Horta F.,Gupta A. F.,Jenkins J.M.,Jord'an 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
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, P$_ orb $ = 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. 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. 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. We find that TOI-4515\,b orbits a 1.2 Gyr-old G-star, has an orbital period of P$_ b 0.000013$ days, a mass of M$_ b J $, and a radius of R$_ b J $. We also find an eccentricity of e\,=\,$0.46 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.
Subject
Space and Planetary Science,Astronomy and Astrophysics