Paper

Three long period transiting giant planets from TESS

Suc, Vincent, Hartman, Joel D, Grieves, Nolan, Caldwell, Douglas A, Mordasini, Christoph, Boyle, Gavin, Cloutier, Ryan, Murgas, Felipe, Jenkins, Jon M, Vezie, Michael, Crouzet, Nicolas, Seager, Sara, Sarkis, Paula, Ziegler, Carl, Schlecker, Martin, Eberhardt, Jan, Winn, Joshua N, Daylan, Tansu, Barkaoui, Khalid, Collins, Karen A, Guillot, Tristan, Ricker, George, Chaverot, Guillaume, Dransfield, Georgina, Trifonov, Trifon, Mann, Andrew W, Youngblood, Allison, Henning, Thomas, Lendl, Monika, Torres, Pascal, Jordán, Andrés, Suarez, Olga, Villanueva, Steven, Kossakowski, Diana, Espinoza, Nestor, Muñoz, Diego J, Jones, Matías I, Rojas, Felipe I, Ulmer-Moll, Solène, Hobson, Melissa J, Schwarz, Rick P, Bouchy, François, Brahm, Rafael, Latham, David W, Deline, Adrien, Mireles, Ismael, Tala, Marcelo, Stockdale, Chris, Dragomir, Diana, Amaury H M J Triaud, Vanderspek, Roland, Palle, Enric, Ciardi, David R, Harris, Mallory, Evans, Phil

2023

Overview

We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single transit events in the light curves generated from the full frame images of the Transiting Exoplanet Survey Satellite (TESS). Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of \\(M_P\\)= 0.30 \\(\\pm\\) 0.04 \\(M_J\\) , a radius of \\(R_P\\)= 1.00 \\(\\pm\\) 0.02 \\(R_J\\) , and a low eccentricity orbit (e=0.15 \\(\\pm\\) 0.05) with a period of P= 30.08364 \\(\\pm\\) 0.00005 d . TOI 2338b has a mass of \\(M_P\\)= 5.98 \\(\\pm\\) 0.20 \\(M_J\\) , a radius of \\(R_P\\)= 1.00 \\(\\pm\\) 0.01 \\(R_J\\) , and a highly eccentric orbit (e= 0.676 \\(\\pm\\) 0.002 ) with a period of P= 22.65398 \\(\\pm\\) 0.00002 d . Finally, TOI 2589b has a mass of \\(M_P\\)= 3.50 \\(\\pm\\) 0.10 \\(M_J\\) , a radius of \\(R_P\\)= 1.08 \\(\\pm\\) 0.03 \\(R_J\\) , and an eccentric orbit (e = 0.522 \\(\\pm\\) 0.006 ) with a period of P= 61.6277 \\(\\pm\\) 0.0002 d . TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.

• Publisher: Cornell University Library, arXiv.org
• Subject: Eccentric orbits / Extrasolar planets / G stars / Jupiter / Light curve / Planet detection / Planetary orbits / Radial velocity / Satellite imagery / Transit