Three warm Jupiters orbiting TOI-6628, TOI-3837, and TOI-5027 and one sub-Saturn orbiting TOI-2328
Trifonov, Trifon; Henning, Thomas; Bieryla, Allyson; Jordán, Andrés; Espinoza, Néstor; Brahm, Rafael; Rice, Malena; Kreidberg, Laura; Eberhardt, Jan; Schlecker, Martin; Collins, Karen A.; Seager, Sara; Boyle, Gavin; Teske, Johanna; Stockdale, Chris; Zambelli, Roberto; Watkins, Cristilyn N.; Ricker, George; Rose, Mark E.; Essack, Zahra; Thompson, Ian; Hobson, Melissa; Wang, Gavin; Jones, Matías; Acuña, Lorena; Winn, Joshua; Rojas, Felipe; Suc, Vincent; Tala Pinto, Marcelo; Reinarz, Yared; Csubry, Zoltan; Bakos, Gaspar; Hartmann, Joel; Knepper, Benjamin; Butler, Robert Paul; Crane, Jeffrey; Schectman, Steve; Osip, Dave
Chile, Germany, United States, Switzerland, Bulgaria, United Kingdom, Australia, Italy
Abstract
We report the discovery and characterization of three new transiting giant planets orbiting TOI-6628, TOI-3837, and TOI-5027 and one new warm sub-Saturn orbiting TOI-2328, whose transits events were detected in the light curves of the Transiting Exoplanet Survey Satellite (TESS) space mission. By combining TESS light curves with ground-based photometric and spectroscopic followup observations, we confirm the planetary nature of the observed transits and radial velocity variations. TOI-6628 b has a mass of 0.74±0.06 MJ and a radius of 0.98‑0.05+0.06 RJ and orbits a metal-rich star with a period of 18.18424 ± 0.00001 days and an eccentricity of 0.670‑0.016+0.015, making it one of the most eccentric orbits of all known warm giants. TOI-3837 b has a mass of 0.59±0.05 MJ and a radius of 0.97‑0.06+0.05 RJ and orbits its host star every 11.88865 ± 0.00003 days, with a moderate eccentricity of 0.221‑0.046+0.042. With a mass of 2.02±0.13 MJ and a radius of 0.96‑0.06+0.05 RJ, TOI-5027 b orbits its host star in an eccentric orbit with e = 0.385‑0.026+0.025 every 10.24368±0.00001 days. TOI-2328 b is a Saturn-like planet with a mass of 0.16±0.02 MJ and a radius of 0.89‑0.05+0.04 RJ; it orbits its host star in a nearly circular orbit with e = 0.057‑0.029+0.046 at a period of 17.10197±0.00001 days. All four planets have orbital periods above ten days, and our planet's interior structure models are consistent with a rocky-icy core with an H/He envelope, providing evidence supporting the core-accretion model of planet formation for this kind of planet.