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

Creators: Carleo, Ilaria^{1, 2, 3}; Barrágan, Oscar⁴; Persson, Carina M.⁵; Fridlund, Malcolm^{5, 6}; Lam, Kristine W. F.⁷; Messina, Sergio⁸; Gandolfi, Davide⁹; Smith, Alexis M. S.⁷; Johnson, Marshall C.¹⁰; Cochran, William¹¹; Osborne, Hannah L. M.^{12, 13}; Brahm, Rafael^{14, 15}; Ciardi, David R.^{16, 17}; Collins, Karen A.¹⁸; Everett, Mark E.¹⁹; Giacalone, Steven¹⁷; Guenther, Eike W.²⁰; Hatzes, Artie²⁰; Hellier, Coel²¹; Horner, Jonathan²²; Kabáth, Petr²³; Korth, Judith²⁴; MacQueen, Phillip¹¹; Masseron, Thomas^{2, 3}; Murgas, Felipe^{2, 3}; Nowak, Grzegorz^{25, 2, 3}; Rodriguez, Joseph E.²⁶; Watkins, Cristilyn N.¹⁸; Wittenmyer, Rob²²; Zhou, George²²; Ziegler, Carl²⁷; Bieryla, Allyson¹⁸; Boyd, Patricia T.²⁸; Clark, Catherine A.^{16, 17}; Dressing, Courtney D.²⁹; Eastman, Jason D.¹⁸; Eberhardt, Jan³⁰; Endl, Michael¹¹; Espinoza, Nestor³¹; Fausnaugh, Michael^{32, 33}; Guerrero, Natalia M.^{33, 34}; Henning, Thomas³⁰; Hesse, Katharine³³; Hobson, Melissa J.³⁵; Howell, Steve B.³⁶; Jordán, Andrés^{14, 15}; Latham, David W.¹⁸; Lund, Michael B.^{16, 17}; Mireles, Ismael³⁷; Narita, Norio^{38, 2}; Tala Pinto, Marcelo^{14, 15}; Pugh, Teznie¹¹; Quinn, Samuel N.¹⁸; Ricker, George³³; Rodriguez, David R.³¹; Rojas, Felipe I.^{39, 15}; Rose, Mark E.³⁶; Rudat, Alexander³³; Sarkis, Paula³⁰; Savel, Arjun B.⁴⁰; Schlecker, Martin⁴¹; Schwarz, Richard P.¹⁸; Seager, Sara³³; Shporer, Avi³³; Smith, Jeffrey C.⁴²; Stassun, Keivan G.⁴³; Stockdale, Chris⁴⁴; Trifonov, Trifon^{30, 45, 46}; Vanderspek, Roland³³; Winn, Joshua N.⁴⁷; Wright, Duncan²²

1. Osservatorio Astrofisico di Torino
2. Instituto de Astrofísica de Canarias
3. University of La Laguna
4. University of Oxford
5. Chalmers University of Technology
6. Leiden University
7. German Aerospace Center
8. Osservatorio Astrofisico di Catania
9. University of Turin
10. The Ohio State University
11. The University of Texas at Austin
12. University College London
13. European Southern Observatory
14. Adolfo Ibáñez University
15. Millennium Institute of Astrophysics
16. NASA Exoplanet Science Institute
17. California Institute of Technology
18. Harvard-Smithsonian Center for Astrophysics
19. NOIRLab
20. Thüringer Landessternwarte Tautenburg
21. Keele University
22. University of Southern Queensland
23. Astronomical Institute
24. Lund University
25. Nicolaus Copernicus University
26. Michigan State University
27. Stephen F. Austin State University
28. Goddard Space Flight Center
29. University of California, Berkeley
30. Max Planck Institute for Astronomy
31. Space Telescope Science Institute
32. Texas Tech University
33. Massachusetts Institute of Technology
34. University of Florida
35. University of Geneva
36. Ames Research Center
37. University of New Mexico
38. University of Tokyo
39. Pontificia Universidad Católica de Chile
40. University of Maryland, College Park
41. University of Arizona
42. Search for Extraterrestrial Intelligence
43. Vanderbilt University
44. Hazelwood Observatory, Australia
45. Sofia University
46. Heidelberg University
47. Princeton University

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.

Copyright and License

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Acknowledgement

C.M.P. and M.F. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19 and 177/19). O.B. acknowledges that has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 865624). G.N. thanks to the research funding from the Ministry of Education and Science programme the “Excellence Initiative – Research University” conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toruń, Poland. P.K. acknowledges funding from LTT-20015 project. D.G. gratefully acknowledges the financial support from the grant for internationalization (GAND_GFI_23_01) provided by the University of Turin (Italy). M.T.P. acknowledges support from the Fondecyt-ANID Post-doctoral fellowship 3210253 and from the ANID Project ASTRO21-0037. A.J. and R.B. acknowledge support from ANID – Millennium Science Initiative – ICN12_009. R.B. acknowledges support from FONDECYT Project 1241963. A.J. acknowledges support from FONDECYT project 1210718. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/Exo-FOP5) 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. KAC and CNW acknowledge support from the TESS mission via subaward s3449 from MIT. D.R.C. and C.A.C. acknowledge partial support from NASA Grant 18-2XRP18_2-0007. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognise their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt Kent is situated. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). The results reported herein benefitted from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. This work is partly supported by JSPS KAKENHI Grant Number JPJP24H00017 and JSPS Bilateral Program Number JPJSBP120249910.

Data Availability

Radial velocity data is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/690/A18

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