Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of P b =5.8 days, a mass of M b =0.9 M J , and a radius of R b =1.3 R J , with a planetary density of 0.477 g cm −3 . TOI-2485 b has an orbital period of P b =11.2 days, a mass of M b =2.4 M J , and a radius of R b =1.1 R J with a density of 2.36 g cm −3 . Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-08-23
DOI
https://doi.org/10.1051/0004-6361/202451313
Citations
1
Primary Topic
Astro and Planetary Science
Type
article
Field-Weighted Citation Impact
0.33

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article

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Samuel N. Quinn, Arjun B. Savel, Ismael Mireles, A. M. S. Smith et al.
1 citations
Astronomy and Astrophysics
Astro and Planetary Science
0.33
article

Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b

Samuel N. Quinn, Arjun B. Savel, Ismael Mireles, A. M. S. Smith, Jan Eberhardt, Patricia T. Boyd, Marcelo Tala Pinto, Martin Schlecker, T. Masseron, F. Murgas, Katharine Hesse, Steven Giacalone, David W. Latham, D. Gandolfi, Michael B. Lund, Rafael Brahm, O. Barragán, E. W. Guenther, Mark E. Rose, Courtney D. Dressing, Chris Stockdale, Steve B. Howell, H. L. M. Osborne, J. Korth, Sara Seager, I. Carleo, P. Kábath, Mark E. Everett, Richard P. Schwarz, A. P. Hatzes, K. W. F. Lam, C. M. Persson, S. Messina, Néstor Espinoza, Michael Fausnaugh, G. Ricker, Teznie Pugh, Catherine A. Clark, Andrés Jordán, Marshall C. Johnson, Carl Ziegler, P. Sarkis, Jonathan Horner, Avi Shporer, Jeffrey C. Smith, George Zhou, Trifon Trifonov, C. Hellier, Jason D. Eastman, Natalia Guerrero, David R. Ciardi, Norio Narita, Thomas Henning, M. Fridlund, D. J. Wright, Joseph E. Rodriguez, Mélissa J. Hobson, Felipe Rojas, William D. Cochran, Keivan G. Stassun, G. Nowak, Allyson Bieryla, David R. Rodriguez, Michael Endl, Roland Vanderspek, Phillip J. MacQueen, Karen A. Collins, Alexander Rudat, Cristilyn N. Watkins, Rob Wittenmyer, Joshua N. Winn
article en
1 citations

Abstract

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of P b =5.8 days, a mass of M b =0.9 M J , and a radius of R b =1.3 R J , with a planetary density of 0.477 g cm −3 . TOI-2485 b has an orbital period of P b =11.2 days, a mass of M b =2.4 M J , and a radius of R b =1.1 R J with a density of 2.36 g cm −3 . Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.

Astronomy and AstrophysicsVol. 690
University of Geneva (CH), Leiden University (NL), California Institute of Technology (US), Texas Tech University (US), Ames Research Center (US), Space Telescope Science Institute (US), Goddard Space Flight Center (US), European Southern Observatory (DE), Jet Propulsion Laboratory (US), University of Arizona (US), Universidad de La Laguna (ES), Pontificia Universidad Católica de Chile (CL), University of New Mexico (US), University of Southern Queensland (AU), Lund University (SE), Vanderbilt University (US), Princeton University (US), Stephen F. Austin State University (US), Adolfo Ibáñez University (CL), Heidelberg University (DE), NASA Exoplanet Science Institute (US), Czech Academy of Sciences, Astronomical Institute (CZ), Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR) (DE), Nicolaus Copernicus University (PL), University of Florida (US), University of Oxford (GB), Millennium Institute of Astrophysics (CL), Osservatorio Astrofisico di Torino (IT), Max Planck Institute for Astronomy (DE), Astrobiology Center (JP), Université Bourgogne Franche-Comté (FR), Osservatorio Astrofisico di Catania (IT), Center for Astrophysics Harvard & Smithsonian (US), Instituto de Astrofísica de Canarias (ES), NSF NOIRLab (US), Tokyo Metropolitan Komaba High School (JP), Thüringer Landessternwarte Tautenburg (DE), Ellinbank Observatory (AU), Leiden Observatory, University College London (GB), American Institute of Aeronautics and Astronautics (US), The Ohio State University (US), University of Turin (IT), Keele University (GB), Sofia University "St. Kliment Ohridski" (BG), Massachusetts Institute of Technology (US), Chalmers University of Technology (SE), University of Maryland, College Park (US), The University of Tokyo (JP), The University of Texas at Austin (US), Michigan State University (US), Search for Extraterrestrial Intelligence (US), University of California, Berkeley (US)
National Science Foundation, National Aeronautics and Space Administration, George Mason University, California Institute of Technology, University of Louisville, University of Texas at Austin, European Commission, University of New South Wales, University of Southern Queensland, Swedish National Space Agency, Ministry of Science, ICT and Future Planning, Nuclear Safety and Security Commission, Uniwersytet Mikolaja Kopernika w Toruniu, Università degli Studi di Torino, Nanjing University, Agencia Nacional de Investigación y Desarrollo, Jet Propulsion Laboratory, Science Mission Directorate, Japan Society for the Promotion of Science
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Astro and Planetary Science
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