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HARPS-N, TESS, and CHEOPS∗ discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426

  • F. Lienhard
  • , A. Mortier
  • , A. Collier Cameron
  • , M. Cretignier
  • , L. Borsato
  • , A. Anna John
  • , J. A. Egger
  • , M. Stalport
  • , T. G. Wilson
  • , A. Deline
  • , A. Fortier
  • , D. W. Latham
  • , L. Malavolta
  • , P. F.L. Maxted
  • , S. G. Sousa
  • , S. L. Grimm
  • , L. Buchhave
  • , Y. Alibert
  • , B. S. Lakeland
  • , X. Dumusque
  • J. Cabrera, L. Naponiello, A. C.M. Correia, F. Rescigno, L. Fossati, A. Sozzetti, R. Alonso, T. Bárczy, D. Barrado, S. C.C. Barros, W. Baumjohann, W. Benz, N. Billot, A. Brandeker, C. Broeg, K. Collins, Sz Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, O. D.S. Demangeon, B. O. Demory, A. Derekas, B. Edwards, D. Ehrenreich, A. Erikson, M. Fridlund, D. Gandolfi, K. Gazeas, M. Gillon, M. Güdel, M. N. Günther, R. Haywood, A. Heitzmann, Ch Helling, K. G. Isaak, J. M. Jenkins, L. L. Kiss, J. Korth, K. W.F. Lam, J. Laskar, A. Lecavelier Des Etangs, A. Leleu, M. Lendl, D. Magrin, A. F.Martínez Fiorenzano, B. Merín, C. Mordasini, V. Nascimbeni, G. Olofsson, H. P. Osborn, R. Ottensamer, I. Pagano, L. Palethorpe, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, K. Rice, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M.S. Smith, S. Sulis, Gy M. Szabó, S. Udry, S. Ulmer-Moll, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton, T. Zingales
  • ETH Zurich
  • University of Birmingham
  • University of St Andrews
  • University of Oxford
  • INAF Osservatorio Astronomico di Padova
  • University of Bern, Institute of Applied Physics
  • University of Liège
  • University of Warwick
  • Université de Genève
  • University of Bern
  • Center for Astrophysics | Harvard & Smithsonian
  • University of Padova
  • Keele University
  • Ipatimup Diagnósticos
  • University of Zurich
  • Technical University of Denmark
  • University of Exeter
  • DLR
  • Istituto di Astrofisica e Planetologia Spaziali (IAPS)
  • University of Coimbra
  • Space Research Institute
  • Instituto de Astrofisica de Canarias
  • Research Unit; CIBERNED and Universidad de La Laguna
  • Admatis Ltd.
  • ESAC campus
  • Stockholm University
  • Lund University
  • LAM
  • University of Bern, Faculty of Medicine
  • Eötvös Loránd University
  • SRON - Netherlands Institute for Space Research
  • University of Geneva
  • University of Leiden
  • Onsala Space Observatory
  • University of Turin
  • University of Athens
  • University of Vienna
  • ESTEC - European Space Research and Technology Centre
  • Graz University of Technology
  • NASA Ames Research Center
  • Konkoly Observatory
  • Sorbonne Univ.
  • Institut d’Astrophysique de Paris
  • Inaf - Fund. Galileo Galilei
  • INAF Osservatorio Astrofisico di Catania
  • University of Edinburgh, Institute for Astronomy
  • University of Edinburgh
  • University of Cambridge
  • Free University of Berlin
  • Campus UAB
  • Institut d’Estudis Espacials de Catalunya (IEEC)
  • HUN-REN–ELTE Exoplanet Research Group
  • Institute of Astronomy

Résultats de recherche: Contribution à un journalArticleRevue par des pairs

Résumé

We provide a detailed characterization of the planetary system orbiting HD 85426 (TOI-1774). This bright G-type star (: 0.99;: 1.13; age: 7.4 Gyr; V mag: 8.25) hosts a transiting sub-Neptune, HD 85426 b, with an orbital period of 16.71 d and a blackbody equilibrium temperature of K. By jointly analysing HARPS-N RVs, TESS, and CHEOPS photometric data and using two different stellar activity mitigation techniques, we constrain planet b's mass to and, depending on the mitigation technique. We investigate the dependence of these results on the priors, data selection, and inclusion of other Keplerians in the modelling. Using this approach, we identify the presence of two non-transiting planetary companions with minimum masses near 10 and orbital periods of 35.7 and 89 d. Additionally, we reject the initial hypothesis that the 35.7-d periodic signal was due to stellar activity. We also determine HD 85426 b's radius to be and compute a transmission spectroscopy metric in the range of 82 to 115, making this planet a highly valuable target for atmospheric characterization.

langue originaleAnglais
Numéro d'articlestaf1934
journalMonthly Notices of the Royal Astronomical Society
Volume545
Numéro de publication3
Les DOIs
étatPublié - 1 janv. 2026
Modification externeOui

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