2024A&A...682A.135C

Query : 2024A&A...682A.135C

2024A&A...682A.135C - Astronomy and Astrophysics, volume 682A135 (2024/2-1)

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., BRICENO 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.G., GUPTA A.F., JENKINS J.M., JORDAN A., KNAPIC C., LATHAM D.W., MIRELES I., LAW N., LORENZI V., LUND M.B., MALDONADO J., MANN A.W., MOLINARI E., PALLE E., PAEGERT M., PEDANI M., QUINN S.N., SCANDARIATO G., SEAGER S., WINN J.N., WOHLER B. and ZINGALES T.

Abstract (from CDS):

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.

Abstract Copyright: © The Authors 2024

Journal keyword(s): methods: observational - techniques: photometric - techniques: radial velocities - planets and satellites: detection - planets and satellites: gaseous planets - stars: fundamental parameters

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 TOI-4515 * 01 24 44.6874285672 +21 30 46.976111064   12.87 11.94     ~ 7 0
2 TOI-4515b Pl 01 24 44.6874285672 +21 30 46.976111064           ~ 7 0
3 SDSS J012444.81+213100.8 * 01 24 44.8201341967 +21 31 00.962012939           ~ 1 0
4 Cl Melotte 25 OpC 04 30 27.4 +16 46 43           ~ 3309 0
5 BD+39 2643 MS* 13 25 07.9957316160 +38 55 20.944920864   11.131 10.257 9.736   K8V 60 0

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