Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b

Ulmer-Moll, S. et al.

Detalhes bibliográficos
Autores: Ulmer-Moll, S., Psaridi, Angelica
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/411288
Acesso em linha:http://hdl.handle.net/10261/411288
http://arxiv.org/abs/2509.15424v1
Access Level:acceso abierto
Palavra-chave:Methods: data analysis
Planets and satellites: detection
Planets and satellites: gaseous planets
Planets and satellites: individual: TOI-2449b
id ES_d7d5f95b02c1d99bc40a2feda682425d
oai_identifier_str oai:digital.csic.es:10261/411288
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
title Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
spellingShingle Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
Ulmer-Moll, S.
Methods: data analysis
Planets and satellites: detection
Planets and satellites: gaseous planets
Planets and satellites: individual: TOI-2449b
title_short Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
title_full Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
title_fullStr Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
title_full_unstemmed Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
title_sort Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 b
dc.creator.none.fl_str_mv Ulmer-Moll, S.
Psaridi, Angelica
author Ulmer-Moll, S.
author_facet Ulmer-Moll, S.
Psaridi, Angelica
author_role author
author2 Psaridi, Angelica
author2_role author
dc.contributor.none.fl_str_mv Agencia Estatal de Investigación (España)
Ministerio de Ciencia e Innovación (España)
Generalitat de Catalunya
European Commission
European Research Council
Ulmer-Moll, S. [0000-0003-2417-7006]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Methods: data analysis
Planets and satellites: detection
Planets and satellites: gaseous planets
Planets and satellites: individual: TOI-2449b
topic Methods: data analysis
Planets and satellites: detection
Planets and satellites: gaseous planets
Planets and satellites: individual: TOI-2449b
description Ulmer-Moll, S. et al.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/411288
http://arxiv.org/abs/2509.15424v1
url http://hdl.handle.net/10261/411288
http://arxiv.org/abs/2509.15424v1
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2020-001058-M
info:eu-repo/grantAgreement/EC/H2020/947660
Ulmer-Moll, S.; Gill, S.; Brahm, R. et..al.; 2025; TOI-2449 b radial velocity curves : J/A+A/703/A258; Centre de Donnees astronomique de Strasbourg; https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/703/A258
https://doi.org/10.1051/0004-6361/202555168
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869421043006832640
spelling Detection and characterisation of a 106-day transiting Jupiter : TOI-2449 b / NGTS-36 bUlmer-Moll, S.Psaridi, AngelicaMethods: data analysisPlanets and satellites: detectionPlanets and satellites: gaseous planetsPlanets and satellites: individual: TOI-2449bUlmer-Moll, S. et al.[Context] Only a handful of transiting giant exoplanets with orbital periods longer than 100 days are known. These warm exoplanets are valuable objects, as their radius and mass can be measured and lead to an in-depth characterisation of the planet’s properties. Thanks to low levels of stellar irradiation and large orbital distances, the atmospheric properties and orbital parameters of warm exoplanets remain relatively unaltered by their host star, giving new insights into planetary formation and evolution.[Aims] Our aim is to increase the sample of warm giant exoplanets with precise radii and masses. Our goal is to identify suitable candidates in the Transiting Exoplanet Survey Satellite data and perform follow-up observations with ground-based instruments.[Methods] We used the Next Generation Transit Survey (NGTS) to detect additional transits of planetary candidates in order to pinpoint their orbital period. We also monitored the target with several high-resolution spectrographs to measure the planetary mass and eccentricity. We studied the planet’s interior composition with a planetary evolution code to determine the planet’s metallicity.[Results] We report the discovery of a 106-day period Jupiter-sized planet around the G-type star TOI-2449/NGTS-36. We jointly modelled the photometric and radial velocity data and find that the planet has a mass of 0.70−0.04+0.05 MJ and a radius of 1.001 ± 0.009 RJ. The planetary orbit has a semi-major axis of 0.449 au and is slightly eccentric (e = 0.0098−0.030+0.028). We detected an additional 3-year signal in the radial velocity data that is likely due to the stellar magnetic cycle. Based on the planetary evolution models considered here, we find that TOI-2449 b/NGTS-36 b contains 11−5+6 M⊕ of heavy elements and has a marginal planet-to-star metal enrichment of 3.3−1.8+2.5. Assuming a Jupiter-like bond albedo, TOI-2449 b/NGTS-36 b has an equilibrium temperature of 400 K and is a good target for understanding nitrogen chemistry in cooler atmospheres.This work has been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF) under grants 51NF40_182901 and 5INF40_205606. The authors acknowledge the financial support of the SNSF This work is based on data collected under the NGTS project at the ESO Paranal Observatory. The NGTS facility is operated by a consortium institutes with support from the UK Science and Technology Facilities Council (STFC) under projects ST/M001962/1, ST/S002642/1 and ST/W003163/1. The contributions at the University of Warwick by SG, DB, PJW, RGW and DA have been supported by STFC through consolidated grants ST/P000495/1, STT000406/1 and ST/X001121/1. KA acknowledges support from the SNSF under the Post-doc Mobility grant P500PT_230225. ML acknowledges support of the SNSF under grant number PCEFP2194576. This paper made use of data collected by the TESS mission and are publicly available from the Mkulski 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. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Super-computing (NAS) Division at Ames Research Center for the production of the SPOC data products. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. R.B. acknowledges support from FONDECYT Project 1241963 and from ANID – Millennium Science Initiative – ICNI2_009. This work was funded by the Data Observatory Foundation. A.De. acknowledges financial support from the Swiss National Science Foundation (SNSF) for project 200021_200726. A.J. acknowledges support from ANID – Mllennium Science Initiative – ICNI2_009, AIM23-0001 and from FONDECYT project 1210718. M.T.P. acknowledges support from Fondecyt-ANID fellowship no. 3210253 and ASTRON-0037. A.P acknowledges support from the Unidad de Excelencia María de Maeztu CEX2020-001058-M programme and from the Generalitat de Catalunya/CERCA. 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”. GV has received support from the European Research Council (ERC) under the European Union s Horizon 2020 research and innovation programme (Grant Agreement No. 947660). Some of the observations in this paper made use of the High-Resolution Imaging instrument Zorro and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini South telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). C.A.W. would like to acknowledge support from the UK Science and Technology Facilities Council (STFC, grant number ST/X00094X/1). JSJ greatfully acknowledges support by FONDECYT grant 1240738 and from the ANID BASAL project FB210003. The contributions at the Mullard Space Science Laboratory by EMB have been supported by STFC through the consolidated grant ST/W001136/1. TR is supported by an STFC studentship.With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (CEX2020-001058-M)Peer reviewedEDP SciencesAgencia Estatal de Investigación (España)Ministerio de Ciencia e Innovación (España)Generalitat de CatalunyaEuropean CommissionEuropean Research CouncilUlmer-Moll, S. [0000-0003-2417-7006]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/411288http://arxiv.org/abs/2509.15424v1reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2020-001058-Minfo:eu-repo/grantAgreement/EC/H2020/947660Ulmer-Moll, S.; Gill, S.; Brahm, R. et..al.; 2025; TOI-2449 b radial velocity curves : J/A+A/703/A258; Centre de Donnees astronomique de Strasbourg; https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/703/A258https://doi.org/10.1051/0004-6361/202555168Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4112882026-05-22T06:33:51Z
score 15,81155

Registos relacionados