학술논문
TOI-4600 b and c: Two long-period giant planets orbiting an early K dwarf
Document Type
Working Paper
Author
Mireles, Ismael; Dragomir, Diana; Osborn, Hugh P.; Hesse, Katharine; Collins, Karen A.; Villanueva, Steven; Bieryla, Allyson; Ciardi, David R.; Stassun, Keivan G.; Harris, Mallory; Lissauer, Jack J.; Schwarz, Richard P.; Srdoc, Gregor; Barkaoui, Khalid; Riffeser, Arno; McLeod, Kim K.; Pepper, Joshua; Grieves, Nolan; Passegger, Vera Maria; Ulmer-Moll, Solène; Rodriguez, Joseph E.; Feliz, Dax L.; Quinn, Samuel; Boyle, Andrew W.; Fausnaugh, Michael; Kunimoto, Michelle; Rowden, Pamela; Vanderburg, Andrew; Wohler, Bill; Jenkins, Jon M.; Latham, David W.; Ricker, George R.; Seager, Sara; Winn, Joshua N.
Source
Subject
Language
Abstract
We report the discovery and validation of two long-period giant exoplanets orbiting the early K dwarf TOI-4600 (V=12.6, T=11.9), first detected using observations from the Transiting Exoplanet Survey Satellite (TESS) by the TESS Single Transit Planet Candidate Working Group (TSTPC-WG). The inner planet, TOI-4600 b, has a radius of 6.80$\pm$0.31 R$_{\oplus}$ and an orbital period of 82.69 d. The outer planet, TOI-4600 c, has a radius of 9.42$\pm$0.42 R$_{\oplus}$ and an orbital period of 482.82 d, making it the longest-period confirmed or validated planet discovered by TESS to date. We combine TESS photometry and ground-based spectroscopy, photometry, and high-resolution imaging to validate the two planets. With equilibrium temperatures of 347 K and 191 K, respectively, TOI-4600 b and c add to the small but growing population of temperate giant exoplanets that bridge the gap between hot/warm Jupiters and the solar system's gas giants. TOI-4600 is a promising target for further transit and precise RV observations to measure masses and orbits for the planets as well as search for additional non-transiting planets. Additionally, with Transit Spectroscopy Metric (TSM) values of $\sim$30, both planets are amenable for atmospheric characterization with JWST. Altogether will lend insight into the formation and evolution of planet systems with multiple giant exoplanets.
Comment: Accepted for publication in ApJL
Comment: Accepted for publication in ApJL