A joint effort to discover and characterize two resonant mini-Neptunes around TOI-1803 with TESS, HARPS-N, and CHEOPS

Context. The discovery and characterization of mini-Neptunes hold a potentially crucial impact on planetary formation and evolution theories. Estimating their orbital parameters and atmospheric properties would provide valuable hints to improve formation and atmospheric models. Aims. We present the discovery of two mini-Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe in detail their orbital architecture and suggest some possible formation and evolution scenarios. Methods. Using CHEOPS, TESS, and HARPS-N datasets, we estimated the radius and the mass of both planets. We used a multidimensional Gaussian process with a quasi-periodic kernel to disentangle the planetary components from the stellar activity in the HARPS-N dataset. We performed dynamical modeling to explain the orbital configuration and performed planetary formation and evolution simulations. For the least dense planet, we assumed different atmospheric compositions and defined possible atmospheric scenarios with simulated JWST observations. Results. TOI-1803 b and TOI-1803 c have orbital periods of ∼6.3 and ∼12.9 days, respectively, residing in close proximity to a 2:1 orbital resonance. Ground-based photometric follow-up observations have revealed significant transit timing variations (TTV) with an amplitude of ∼10 min and ∼40 min, respectively, for planets b and -c. With the masses computed from the radial velocities dataset, we obtained a density of (0.39 ± 0.10) ρ ⊕ and (0.076 ± 0.038) ρ ⊕ for planets b and -c, respectively. TOI-1803 c is among the least dense mini-Neptunes currently known, and due to its inflated atmosphere, it is a suitable target for transmission spectroscopy with JWST. With NIRSpec observations, we could understand whether the planet has kept its primary atmosphere or not, which would constrain our formation models. Conclusions. We report the discovery of two mini-Neptunes close to a 2:1 orbital resonance. The detection of significant TTVs from ground-based photometry opens scenarios for a more precise mass determination. TOI-1803 c is one of the least dense mini-Neptunes known so far, and it is of great interest among the scientific community since it could constrain current formation scenarios. JWST observations could give us valuable insights to characterize this interesting system.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-02-18
DOI
https://doi.org/10.1051/0004-6361/202451180
Citations
2
Primary Topic
Solar and Space Plasma Dynamics
Type
article
Field-Weighted Citation Impact
2.31
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article

A joint effort to discover and characterize two resonant mini-Neptunes around TOI-1803 with TESS, HARPS-N, and CHEOPS

D. Polychroni, M. Deleuil, A. S. Bonomo, M. Gy. Szabó et al.
2 citations
Astronomy and Astrophysics
Solar and Space Plasma Dynamics
2.31
article

A joint effort to discover and characterize two resonant mini-Neptunes around TOI-1803 with TESS, HARPS-N, and CHEOPS

D. Polychroni, M. Deleuil, A. S. Bonomo, M. Gy. Szabó, D.R. Ciardi, L. Cabona, A. Collier Cameron, Pau Bosch-Cabot, H. Rauer, A. Bekkelien, A. M. S. Smith, J. Schlieder, E.C. Matthews, D. Magrin, L.G. Bouma, Jon M. Jenkins, S. Desidera, S. Sulis, D. Pollacco, L. Malavolta, A. Shporer, L. Borsato, M.N. Günther, P. F. L. Maxted, R. Claudi, V. Nascimbeni, M. Lendl, Akihiko Fukui, L. L. Kiss, Joseph D. Twicken, D. Queloz, L. Naponiello, E. Pallé, A. Maggio, M. Fridlund, A. F. Lanza, S. Seager, A. C. M. Correia, A. Deline, C. Mordasini, J. Korth, N.C. Santos, A. E. Simon, G. Piotto, M. B. Davies, Sébastien Salmon, Diana Dragomir, J.A. Egger, N. Billot, Rachel A. Matson, T. Zingales, P. Leonardi, F. Ratti, Karen A. Collins, R. Alonso, A. Sozzetti, G. Peter, Steve B. Howell, D. N. Baker, A. Fortier, D. Locci, Roberto Ragazzoni, L. Fossati, G. Lacedelli, D. Ségransan, M. J. Hooton, D. Turrini, I. Carleo, A. Derekas, A. Lecavelier des Etangs, I. Ribas, M. Damasso, K. W. F. Lam, K. G. Isaak, T. Bárczy, G. Andreuzzi, G. Mantovan, L. Delrez, Y. Alibert, Ch. Helling, Ben Falk, Khalid Barkaoui, Scott McDermott, C. Broeg, M. Gillon, A. Heitzmann, G. Scandariato, F. Biassoni, S. Udry, D. Barrado, N. A. Walton, Erica J. Gonzales, R. Cosentino, W. Benz, W. Baumjohann, A. Erikson, S. C. C. Barros, Tony Beck, D. Ehrenreich, P. Guerra, M. Munari, Patricio E. Cubillos, D. Nardiello, D. Gandolfi, Norio Narita, K. Gazeas, J. Venturini, Brice-Olivier Demory, O. D. S. Demangeon, R.P. Schwarz, Billy Edwards, M. Stalport, A. Brandeker, G. Olofsson, T. G. Wilson, A. Bignamini, A. Bonfanti, E. Villaver, Allyson Bieryla, M. Steinberger, V. Van Grootel, S. G. Sousa, N. Rando, M. Pinamonti, J. Laskar, M. Güdel, I. Pagano, C. Beichman, L. Mancini, J. N., Sz. Csizmadia, R. Ottensamer, J.M. Ian Crossfield
article en
2 citations

Abstract

Context. The discovery and characterization of mini-Neptunes hold a potentially crucial impact on planetary formation and evolution theories. Estimating their orbital parameters and atmospheric properties would provide valuable hints to improve formation and atmospheric models. Aims. We present the discovery of two mini-Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe in detail their orbital architecture and suggest some possible formation and evolution scenarios. Methods. Using CHEOPS, TESS, and HARPS-N datasets, we estimated the radius and the mass of both planets. We used a multidimensional Gaussian process with a quasi-periodic kernel to disentangle the planetary components from the stellar activity in the HARPS-N dataset. We performed dynamical modeling to explain the orbital configuration and performed planetary formation and evolution simulations. For the least dense planet, we assumed different atmospheric compositions and defined possible atmospheric scenarios with simulated JWST observations. Results. TOI-1803 b and TOI-1803 c have orbital periods of ∼6.3 and ∼12.9 days, respectively, residing in close proximity to a 2:1 orbital resonance. Ground-based photometric follow-up observations have revealed significant transit timing variations (TTV) with an amplitude of ∼10 min and ∼40 min, respectively, for planets b and -c. With the masses computed from the radial velocities dataset, we obtained a density of (0.39 ± 0.10) ρ ⊕ and (0.076 ± 0.038) ρ ⊕ for planets b and -c, respectively. TOI-1803 c is among the least dense mini-Neptunes currently known, and due to its inflated atmosphere, it is a suitable target for transmission spectroscopy with JWST. With NIRSpec observations, we could understand whether the planet has kept its primary atmosphere or not, which would constrain our formation models. Conclusions. We report the discovery of two mini-Neptunes close to a 2:1 orbital resonance. The detection of significant TTVs from ground-based photometry opens scenarios for a more precise mass determination. TOI-1803 c is one of the least dense mini-Neptunes known so far, and it is of great interest among the scientific community since it could constrain current formation scenarios. JWST observations could give us valuable insights to characterize this interesting system.

Astronomy and AstrophysicsVol. 695
Eötvös Loránd University (HU), University of Geneva (CH), University of Insubria (IT), University of Rome Tor Vergata (IT), University of Bern (CH), Austin College (US), Leiden University (NL), California Institute of Technology (US), Ames Research Center (US), Centre National de la Recherche Scientifique (FR), Space Telescope Science Institute (US), University of Vienna (AT), Goddard Space Flight Center (US), Institute of Space Sciences (ES), Austrian Academy of Sciences (AT), University of Padua (IT), University of Kansas (US), University of Liège (BE), Universidad de La Laguna (ES), Stockholm University (SE), University of St Andrews (GB), University of New Mexico (US), Universidade do Porto (PT), University of California, Santa Cruz (US), Lund University (SE), University of Trento (IT), National and Kapodistrian University of Athens (GR), Princeton University (US), Aix-Marseille Université (FR), University of Cambridge (GB), NASA Exoplanet Science Institute (US), Astronomical Observatory of Rome (IT), Trieste Astronomical Observatory (IT), Institut d'Astrophysique de Paris (FR), Konkoly Observatory (HU), Brera Astronomical Observatory (IT), 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), Space Research Institute (AT), Institut d'Estudis Espacials de Catalunya (ES), Osservatorio Astrofisico di Torino (IT), Cavendish Hospital (GB), Max Planck Institute for Astronomy (DE), Astrobiology Center (JP), Université Bourgogne Franche-Comté (FR), Institute of Astronomy (RU), Osservatorio Astrofisico di Catania (IT), Center for Astrophysics Harvard & Smithsonian (US), Osservatorio Astronomico di Palermo (IT), HUN-REN Research Centre for Astronomy and Earth Sciences (HU), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), AlbaNova (SE), Tokyo Metropolitan Komaba High School (JP), LogicMill Technology (United States) (US), Szent Imre Egyetemi Oktatókórház (HU), Osservatorio Astronomico di Padova (IT), Telescopio Nazionale Galileo (ES), Leiden Observatory, European Space Research and Technology Centre (NL), American Institute of Aeronautics and Astronautics (US), Space Research Organisation Netherlands (NL), Institut de Mécanique Céleste et de Calcul des Éphémérides (FR), University of Turin (IT), Keele University (GB), Massachusetts Institute of Technology (US), Chalmers University of Technology (SE), The University of Tokyo (JP), Freie Universität Berlin (DE), University of Coimbra (PT), Search for Extraterrestrial Intelligence (US), KU Leuven (BE)
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