A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS

Creators: Bozhilov, Vladimir; Antonova, Desislava; Hobson, Melissa J.; Brahm, Rafael; Jordán, Andrés; Henning, Thomas; Eberhardt, Jan; Rojas, Felipe I.; Batygin, Konstantin; Torres-Miranda, Pascal; Stassun, Keivan G.; Millholland, Sarah C.; Stoeva, Denitza; Minev, Milen; Espinoza, Nestor; Ricker, George R.; Latham, David W.; Dragomir, Diana; Kunimoto, Michelle; Jenkins, Jon M.; Ting, Eric B.; Seager, Sara; Winn, Joshua N.; Villasenor, Jesus Noel; Bouma, Luke G.; Medina, Jennifer; Trifonov, Trifon

Abstract

We report the discovery of a super-Jovian 2:1 mean-motion resonance (MMR) pair around the G-type star TIC 279401253, whose dynamical architecture is a prospective benchmark for planet formation and orbital evolution analysis. The system was discovered thanks to a single-transit event recorded by the Transiting Exoplanet Survey Satellite mission, which pointed to a Jupiter-sized companion with poorly constrained orbital parameters. We began ground-based precise radial velocity (RV) monitoring with HARPS and FEROS within the Warm gIaNts with tEss survey to constrain the transiting body's period, mass, and eccentricity. The RV measurements revealed not one but two massive planets with periods of 76.80^(+0.06)_(−0.06) and 155.3^(+0.7)_(-0.7) days, respectively. A combined analysis of transit and RV data yields an inner transiting planet with a mass of 6.14^(+0.39)_(−0.42) M_(Jup) and a radius of 1.00^(+0.04)_(-0.04) R_(Jup), and an outer planet with a minimum mass of 8.02^(+0.18)_(-0.18) M_(Jup), indicating a massive giant pair. A detailed dynamical analysis of the system reveals that the planets are locked in a strong first-order, eccentricity-type 2:1 MMR, which makes TIC 279401253 one of the rare examples of truly resonant architectures supporting disk-induced planet migration. The bright host star, V ≈ 11.9 mag, the relatively short orbital period (P_b = 76.80^(+0.06)_(-0.06) days), and pronounced eccentricity (e = 0.448^(+0.028)_(-0.029)) make the transiting planet a valuable target for atmospheric investigation with the James Webb Space Telescope and ground-based extremely large telescopes.

Additional Information

© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO programmes 105.20GX.001, 108.22A8.001, 110.23YQ.001, and MPG programmes 0106.A-9014, 0107.A-9003, 0108.A-9003, 0109.A-9003, 0110.A-9011. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA's Science Mission directorate. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. V.B., D.A., D.S., M.M., and T.T. acknowledge support by the BNSF program "VIHREN-2021" project No. KP-06-DV-5/15.12.2021. T.T. acknowledges support by the DFG Research Unit FOR 2544 "Blue Planets around Red Stars" project No. KU 3625/2-1. A.J., R.B., M.H. and F.R. acknowledge support from ANID—Millennium Science Initiative—ICN12_009. D.D. acknowledges support from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136. A.J. acknowledges additional support from FONDECYT project 1210718. R.B. acknowledges support from FONDECYT project 11200751. This work was also funded by the Data Observatory Foundation. We thank Yair Judkovsky for useful discussion on the TTV analysis. We thank the anonymous reviewer for very helpful comments and suggestions.

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