Improved characterization of the TOI-2141 system: A dense sub-Neptune with non-transiting inner and outer companions

Aims. We aim to refine the fundamental parameters of the TOI-2141 planetary system, which includes a transiting sub-Neptune orbiting a Sun-like star on a relatively long orbit of 18.26 days, by combining new photometric and spectroscopic observations. Methods. We analyzed new space-based photometry from TESS and CHEOPS, as well as 61 radial velocity measurements from HARPS-N. We performed individual and joint photometric and RV analyses using several modeling tools within a Bayesian model comparison framework. Results. We refined the radius and mass of the transiting planet TOI-2141 b to 3.15 ± 0.04 R ⊕ and 20.1 ± 1.6 M ⊕ to levels that are five and two times more precise, respectively, than the previously reported values. Our radial velocity analysis reveals two additional non-transiting companions with orbital periods of 5.46 and 60.45 days. Despite the innermost planet’s high geometric transit probability, we found no evidence of transits in the photometric data. Conclusions. The bulk properties of TOI-2141 b suggest a significant volatile envelope atop an Earth-like core. The modeling indicates a hydrogen-rich atmosphere that could have experienced mild photoevaporation over the system’s history. Planets b and c are believed to exhibit a modest mutual inclination of at least ~2.4°.

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Journal
Astronomy and Astrophysics
Published
2025-09-22
DOI
https://doi.org/10.1051/0004-6361/202556515
Primary Topic
Astro and Planetary Science
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article
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article

Improved characterization of the TOI-2141 system: A dense sub-Neptune with non-transiting inner and outer companions

M. Gy. Szabó, D. Pollacco, A. Collier Cameron, N. Billot et al.
Astronomy and Astrophysics
Astro and Planetary Science
article

Improved characterization of the TOI-2141 system: A dense sub-Neptune with non-transiting inner and outer companions

M. Gy. Szabó, D. Pollacco, A. Collier Cameron, N. Billot, A. M. S. Smith, J. Laskar, T. Bárczy, S. Sulis, M. Guêdel, R. Luque, I. Ribas, M. Fridlund, L. Borsato, Sebastián Wolf, J. Asquier, M.N. Günther, J. Cabrera, V. Nascimbeni, A. Erikson, C. Broeg, L. L. Kiss, D. Gandolfi, D. Queloz, S. Ulmer-Moll, A. C. M. Correia, C. Mordasini, J. Korth, W. Baumjohann, A. Leleu, A. E. Simon, G. Piotto, B. Edwards, M. B. Davies, J.A. Egger, S. Udry, R. Alonso, C. Pezzotti, A. Deline, Roberto Ragazzoni, D. Ségransan, B. Ulmer, M. Lendl, A. Fortier, A. Derekas, R. Ottensamer, T. Keller, A. Brandeker, F. Biondi, K. W. F. Lam, K. G. Isaak, G. Olofsson, G. Mantovan, Ch. Helling, Y. Alibert, A. Heitzmann, H. Rauer, G. Scandariato, Nuno C. Santos, D. Barrado, G. Peter, B.-O. Demory, N. A. Walton, A. Bonfanti, A. Lecavelier des Étangs, M. Deleuil, S. C. C. Barros, M. Gillon, W. Benz, D. Ehrenreich, Patricio E. Cubillos, N. Rando, Demetrio Magrin, K. Gazeas, J. Venturini, L. Fossati, H.P. Osborn, M. Stalport, T. G. Wilson, B. Merín, E. Pallé, V. Van Grootel, Yoshi Nike Emilia Eschen, S. G. Sousa, E. Villaver, D. Piazza, O. D. S. Demangeon, Sz. Csizmadia, P. F. L. Maxted, D. Wolter, I. Pagano
article en

Abstract

Aims. We aim to refine the fundamental parameters of the TOI-2141 planetary system, which includes a transiting sub-Neptune orbiting a Sun-like star on a relatively long orbit of 18.26 days, by combining new photometric and spectroscopic observations. Methods. We analyzed new space-based photometry from TESS and CHEOPS, as well as 61 radial velocity measurements from HARPS-N. We performed individual and joint photometric and RV analyses using several modeling tools within a Bayesian model comparison framework. Results. We refined the radius and mass of the transiting planet TOI-2141 b to 3.15 ± 0.04 R ⊕ and 20.1 ± 1.6 M ⊕ to levels that are five and two times more precise, respectively, than the previously reported values. Our radial velocity analysis reveals two additional non-transiting companions with orbital periods of 5.46 and 60.45 days. Despite the innermost planet’s high geometric transit probability, we found no evidence of transits in the photometric data. Conclusions. The bulk properties of TOI-2141 b suggest a significant volatile envelope atop an Earth-like core. The modeling indicates a hydrogen-rich atmosphere that could have experienced mild photoevaporation over the system’s history. Planets b and c are believed to exhibit a modest mutual inclination of at least ~2.4°.

Astronomy and AstrophysicsVol. 704
Eötvös Loránd University (HU), University of Geneva (CH), University of Bern (CH), Leiden University (NL), Centre National de la Recherche Scientifique (FR), University of Vienna (AT), Austrian Academy of Sciences (AT), University of Padua (IT), University of Liège (BE), Universidade do Porto (PT), Lund University (SE), National and Kapodistrian University of Athens (GR), Aix-Marseille Université (FR), University of Cambridge (GB), Université Paris Sciences et Lettres (FR), Istituto Nazionale di Fisica Nucleare, Galileo Galilei Institute for Theoretical Physics (IT), NASA Exoplanet Science Institute (US), Institut d'Astrophysique de Paris (FR), European Space Agency (FR), Observatoire astronomique de Strasbourg (FR), Konkoly Observatory (HU), Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR) (DE), ETH Zurich (CH), University of Warwick (GB), Sorbonne Université (FR), Graz University of Technology (AT), Institute of Astrophysics and Space Sciences (PT), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Osservatorio Astrofisico di Torino (IT), Cavendish Hospital (GB), Institute of Space Sciences (ES), Instituto de Física Teórica (ES), Astrobiology Center (JP), Institute of Astronomy (RU), Osservatorio Astrofisico di Catania (IT), Scottish Universities Physics Alliance (GB), HUN-REN Research Centre for Astronomy and Earth Sciences (HU), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), AlbaNova (SE), Computational Physics (United States) (US), Instituto de Astrofísica de Andalucía (ES), Osservatorio Astronomico di Padova (IT), Leiden Observatory, European Space Research and Technology Centre (NL), Space Research Organisation Netherlands (NL), University of Turin (IT), Keele University (GB), Chalmers University of Technology (SE), Freie Universität Berlin (DE), University of Coimbra (PT)
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