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dc.contributor.author
Lillo Box, J.
dc.contributor.author
Gandolfi, D.
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Armstrong, D. J.
dc.contributor.author
Collins, K. A.
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Nielsen, Louise D.
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dc.contributor.author
Luque, R.
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Korth, J.
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Sousa, S. G.
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Quinn, S. N.
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Acuña, L.
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Howell, S. B.
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Morello, G.
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Hellier, C.
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Giacalone, S.
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Hoyer, S.
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Stassun, K.
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Palle, E.
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Aguichine, A.
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Mousis, O.
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Adibekyan, V.
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Azevedo Silva, T.
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Barrado, D.
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Deleuil, M.
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Eastman, J. D.
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Diaz, Rodrigo Fernando
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Shectman, S.A.
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Shporer, A.
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Vezie, M.
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Wang, S. X.
dc.contributor.author
Zhou, G.
dc.date.available
2024-03-14T12:01:58Z
dc.date.issued
2023-01
dc.identifier.citation
Lillo Box, J.; Gandolfi, D.; Armstrong, D. J.; Collins, K. A.; Nielsen, Louise D.; et al.; TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter; EDP Sciences; Astronomy and Astrophysics; 669; 1-2023; 1-25
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/230504
dc.description.abstract
Context. The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. Aims. In this paper we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star. Methods. We use a set of precise radial velocity observations from HARPS, PFS and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system. Results. We find that TOI-969 b is a transiting close-in (Pb ∼ 1.82 days) mini-Neptune planet (mb = 9.1 +1.1 −1.0 M⊕, Rb = 2.765+0.088 −0.097 R⊕), thus placing it on the lower boundary of the hot-Neptune desert (Teq,b = 941 ± 31 K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of Pc = 1700+290 −280 days and a minimum mass of mc sin ic = 11.3 +1.1 −0.9 MJup, and with a highly-eccentric orbit of ec = 0.628+0.043 −0.036. Conclusions. The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93, and it orbits a moderately bright (G = 11.3 mag) star, thus becoming an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
PLANETS AND SATELLITES: COMPOSITION
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PLANETS AND SATELLITES: DETECTION
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PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
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STARS: INDIVIDUAL: TOI-969
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TECHNIQUES: PHOTOMETRIC
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TECHNIQUES: RADIAL VELOCITIES
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2024-02-28T10:30:26Z
dc.journal.volume
669
dc.journal.pagination
1-25
dc.journal.pais
Francia
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dc.description.fil
Fil: Lillo Box, J.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
dc.description.fil
Fil: Gandolfi, D.. Università di Torino; Italia
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Fil: Armstrong, D. J.. University of Warwick; Reino Unido
dc.description.fil
Fil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
dc.description.fil
Fil: Nielsen, Louise D.. European Southern Observatory; Suiza
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Fil: Luque, R.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
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Fil: Korth, J.. Chalmers University of Technology; Suecia
dc.description.fil
Fil: Sousa, S. G.. Universidad de Porto; Portugal
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Fil: Quinn, S. N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Acuña, L.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
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Fil: Howell, S. B.. National Aeronautics and Space Administration; Estados Unidos
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Fil: Morello, G.. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España
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Fil: Hellier, C.. Keele University; Reino Unido
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Fil: Giacalone, S.. University of California at Berkeley; Estados Unidos
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Fil: Hoyer, S.. Aix Marseille Université; Francia
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Fil: Stassun, K.. Vanderbilt University; Estados Unidos
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Fil: Palle, E.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
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Fil: Aguichine, A.. Aix Marseille Université; Francia
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Fil: Mousis, O.. Aix Marseille Université; Francia
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Fil: Adibekyan, V.. Universidad de Porto; Portugal. Centro de Astrofísica Da Universidade Do Porto; Portugal
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Fil: Azevedo Silva, T.. Universidad de Porto; Portugal
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Fil: Barrado, D.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
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Fil: Deleuil, M.. Aix Marseille Université; Francia
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Fil: Eastman, J. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
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Fil: Shectman, S.A.. National Aeronautics and Space Administration; Estados Unidos
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Fil: Shporer, A.. University of New Mexico; Estados Unidos
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Fil: Vezie, M.. University of New Mexico; Estados Unidos
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Fil: Wang, S. X.. Tsinghua University; China
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Fil: Zhou, G.. University of Southern Queensland; Australia
dc.journal.title
Astronomy and Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/202243879
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/01/aa43879-22/aa43879-22.html
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