TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

DOI: 
10.3847/1538-3881/ad4993
Publication date: 
11/07/2024
Main author: 
Thao, Pa Chia
IAA authors: 
Pozuelos, Francisco J.
Authors: 
Thao, Pa Chia;Mann, Andrew W.;Barber, Madyson G.;Kraus, Adam L.;Tofflemire, Benjamin M.;Bush, Jonathan L.;Wood, Mackenna L.;Collins, Karen A.;Vanderburg, Andrew;Quinn, Samuel N.;Zhou, George;Newton, Elisabeth R.;Ziegler, Carl;Law, Nicholas;Barkaoui, Khalid;Pozuelos, Francisco J.;Timmermans, Mathilde;Gillon, Michaël;Jehin, Emmanuël;Schwarz, Richard P.;Gan, Tianjun;Shporer, Avi;Horne, Keith;Sefako, Ramotholo;Suarez, Olga;Mekarnia, Djamel;Guillot, Tristan;Abe, Lyu;Triaud, Amaury H. M. J.;Radford, Don J.;Lopez Murillo, Ana Isabel;Ricker, George R.;Winn, Joshua N.;Jenkins, Jon M.;Bouma, Luke G.;Fausnaugh, Michael;Guerrero, Natalia M.;Kunimoto, Michelle
Journal: 
The Astronomical Journal
Publication type: 
Article
Volume: 
168
Pages: 
41
Abstract: 
Young (&lt;500 Myr) planets are critical to studying how planets form and evolve. Among these young planetary systems, multiplanet configurations are particularly useful, as they provide a means to control for variables within a system. Here, we report the discovery and characterization of a young planetary system, TOI-1224. We show that the planet host resides within a young population we denote as MELANGE-5. By employing a range of age-dating methods—isochrone fitting, lithium abundance analysis, gyrochronology, and Gaia excess variability—we estimate the age of MELANGE-5 to be 210 ± 27 Myr. MELANGE-5 is situated in close proximity to previously identified younger (80–110 Myr) associations, Crius 221 and Theia 424/Volans-Carina, motivating further work to map out the group boundaries. In addition to a planet candidate detected by the TESS pipeline and alerted as a TESS object of interest, TOI-1224 b, we identify a second planet, TOI-1224 c, using custom search tools optimized for young stars (Notch and LOCoR). We find that the planets are 2.10 ± 0.09 R <SUB>⊕</SUB> and 2.88 ± 0.10 R <SUB>⊕</SUB> and orbit their host star every 4.18 and 17.95 days, respectively. With their bright (K = 9.1 mag), small (R <SUB>*</SUB> = 0.44 R <SUB>⊙</SUB>), and cool (T <SUB>eff</SUB> = 3326 K) host star, these planets represent excellent candidates for atmospheric characterization with JWST.
Database: 
ADS
SCOPUS
URL: 
https://ui.adsabs.harvard.edu/#abs/2024AJ....168...41T/abstract
ADS Bibcode: 
2024AJ....168...41T
Keywords: 
Exoplanet astronomy;Transit photometry;Stellar ages;Young star clusters;Stellar activity;Transit timing variation method;486;1709;1581;1833;1580;1710;Astrophysics - Earth and Planetary Astrophysics