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

F. Lienhard et al.

Detalhes bibliográficos
Autores: Lienhard, Florian, Barrado y Navascués, David, Ribas, Ignasi
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2026
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/418623
Acesso em linha:http://hdl.handle.net/10261/418623
Access Level:acceso abierto
Palavra-chave:Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic
Planets and satellites: composition
Planets and satellites: fundamental parameters
Stars: individual (HD 85426)
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dc.title.none.fl_str_mv HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
title HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
spellingShingle HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
Lienhard, Florian
Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic
Planets and satellites: composition
Planets and satellites: fundamental parameters
Stars: individual (HD 85426)
title_short HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
title_full HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
title_fullStr HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
title_full_unstemmed HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
title_sort HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426
dc.creator.none.fl_str_mv Lienhard, Florian
Barrado y Navascués, David
Ribas, Ignasi
author Lienhard, Florian
author_facet Lienhard, Florian
Barrado y Navascués, David
Ribas, Ignasi
author_role author
author2 Barrado y Navascués, David
Ribas, Ignasi
author2_role author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Agencia Estatal de Investigación (España)
European Commission
Generalitat de Catalunya
European Research Council
Barrado y Navascués, David [0000-0002-5971-9242]
Ribas, Ignasi [0000-0002-6689-0312]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic
Planets and satellites: composition
Planets and satellites: fundamental parameters
Stars: individual (HD 85426)
topic Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic
Planets and satellites: composition
Planets and satellites: fundamental parameters
Stars: individual (HD 85426)
description F. Lienhard et al.
publishDate 2026
dc.date.none.fl_str_mv 2026
2026
2026
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/418623
url http://hdl.handle.net/10261/418623
dc.language.none.fl_str_mv Inglés
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The underlying dataset has been published as supplementary material of the article in the publisher platform at DOI 10.1093/mnras/staf1934
https://doi.org/10.1093/mnras/staf1934
Sí
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dc.publisher.none.fl_str_mv Royal Astronomical Society
Oxford University Press
publisher.none.fl_str_mv Royal Astronomical Society
Oxford University Press
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
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spelling HARPS-N, TESS, and CHEOPS discover a transiting sub-Neptune and two outer companions around the bright solar analogue HD 85426Lienhard, FlorianBarrado y Navascués, DavidRibas, IgnasiTechniques: photometricTechniques: radial velocitiesTechniques: spectroscopicPlanets and satellites: compositionPlanets and satellites: fundamental parametersStars: individual (HD 85426)F. Lienhard et al.This article uses data from the CHEOPS Guaranteed Time Observation programme CH PR100024.We provide a detailed characterization of the planetary system orbiting HD 85426 (TOI-1774). This bright G-type star (M∗: 0.99 M; R∗: 1.13 R; 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 824+11 −11 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 6.0+1.5 −1.6 M⊕ and 8.5+1.3 −1.4 M⊕, 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 M⊕ 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 2.78+0.05 −0.04 R⊕ and compute a transmission spectroscopy metric in the range of 82 to 115, making this planet a highly valuable target for atmospheric characterization.CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. CHEOPS data analysed in this article will be made available in the CHEOPS mission archive (https://cheops.unige.ch/archive_browser/). This paper made use of data collected by the TESS mission and are publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA’s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of data and/or services provided by the International Astronomical Union’s Minor Planet Center. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. AM acknowledges funding from a UKRI Future Leader Fellowship, grant number MR/X033244/1 and a UK Science and Technology Facilities Council (STFC) small grant ST/Y002334/1. ACC acknowledges support from STFC consolidated grant number ST/V000861/1and UKRI/ERC Synergy Grant EP/Z000181/1(REVEAL). BSL acknowledges funding from a UKRI Future Leader Fellowship (grant number MR/X033244/1). RDH is funded by the UK Science and Technology Facilities Council (STFC)’s Ernest Rutherford Fellowship (grant number ST/V004735/1). LBo, GBr, VNa, IPa, GPi, RRa, GSc, VSi, and TZi acknowledge support from CHEOPS ASI-INAF agreement n. 2019-29-HH.0. LBo acknowledges financial support from the Bando Ricerca Fondamentale INAF 2023, Mini-Grant: ‘Decoding the dynamical properties of planetary systems observed by TESS and CHEOPS through TTV analysis with parallel computing’. TZi acknowledges support from NVIDIA Academic Hardware Grant Program for the use of the Titan V GPU card and the Italian MUR Departments of Excellence grant 2023–2027 ‘Quantum Frontiers’. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. TWi acknowledges support from the UKSA and the University of Warwick. PM acknowledges support from STFC research grant number ST/R000638/1. SGS acknowledge support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). The Portuguese team thanks the Portuguese Space Agency for the provision of financial support in the framework of the PRODEX Programme of the European Space Agency (ESA) under contract number 4000142255. YAl acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. ACMC acknowledges support from the FCT, Portugal, through the CFisUC projects UIDB/04564/2020 and UIDP/04564/2020, with DOI identifiers 10.54499/UIDB/04564/2020 and 10.54499/UIDP/04564/2020, respectively. AC, AD, BE, KG, and JK acknowledge their role as ESA-appointed CHEOPS Science Team Members. DB, EP, EV, IR, and RA acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF ‘A way of making Europe’ through projects PID2021-125627OB-C31, PID2021-125627OB-C32, PID2021-127289NB-I00, PID2023-150468NB-I00 and PID2023-149439NB-C41. from the Centre of Excellence ‘Severo Ochoa’ award to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), the Centre of Excellence ‘María de Maeztu’ award to the Institut de Ciències de l’Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. SCCB acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) in the form of work contract through the Scientific Employment Incentive program with reference 2023.06687.CEECIND and DOI 10.54499/2023.06687.CEECIND/CP2839/CT0002. ABr was supported by the SNSA. CB and AS acknowledge support from the Swiss Space Office through the ESA PRODEX program. P.E.C. is funded by the Austrian Science Fund (FWF) Erwin Schroedinger Fellowship, programme J4595-N. This project was supported by the CNES. This work was supported by FCT—Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 through the research grants UIDB/04434/2020, UIDP/04434/2020, 2022.06962.PTDC. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B-OD acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. This project has received funding from the Swiss National Science Foundation for project 200021_200726. It has also been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grant 51NF40_205606. The authors acknowledge the financial support of the SNSF. MF and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 ‘Gaseous or rocky? Unveiling the nature of small worlds’. M.G. is an F.R.S.-FNRS Senior Research Associate. MNG is the ESA CHEOPS Project Scientist and Mission Representative. BMM is the ESA CHEOPS Project Scientist. KGI was the ESA CHEOPS Project Scientist until the end of December 2022 and Mission Representative until the end of January 2023. All of them are/were responsible for the Guest Observers (GO) Programme. None of them relay/relayed proprietary information between the GO and Guaranteed Time Observation (GTO) Programmes, nor do/did they decide on the definition and target selection of the GTO Programme. CHe acknowledges financial support from the Österreichische Akademie 1158 der Wissenschaften and from the European Union H2020-MSCA-ITN-2019 1159 under Grant Agreement no. 860470 (CHAMELEON). Calculations were performed using supercomputer resources provided by the Vienna Scientific Cluster (VSC). KWFL was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. AL and JK acknowledge support of the Swiss National Science Foundation under grant number TMSGI2_211697. ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. VVG is an F.R.S-FNRS Research Associate. JV acknowledges support from the Swiss National Science Foundation (SNSF) under grant PZ00P2_208945. NAW acknowledges UKSA grant ST/R004838/1.With funding from the Spanish government through the "Severo Ochoa Centre of Excelence" accreditation (CEX2019-000920-S)With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (CEX2020-001058-M)Peer reviewedRoyal Astronomical SocietyOxford University PressMinisterio de Ciencia e Innovación (España)Agencia Estatal de Investigación (España)European CommissionGeneralitat de CatalunyaEuropean Research CouncilBarrado y Navascués, David [0000-0002-5971-9242]Ribas, Ignasi [0000-0002-6689-0312]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202620262026info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/418623reponame:DIGITAL.CSIC. 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