TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter

Autores: Lillo Box, J.; Gandolfi, D.; Armstrong, D. J.; Collins, K. A.; Nielsen, Louise D.; Luque, R.; Korth, J.; Sousa, S. G.; Quinn, S. N.; Acuña, L.; Howell, S. B.; Morello, G.; Hellier, C.; Giacalone, S.; Hoyer, S.; Stassun, K.; Palle, E.; Aguichine, A.; Mousis, O.; Adibekyan, V.; Azevedo Silva, T.; Barrado, D.; Deleuil, M.; Eastman, J. D.; Diaz, Rodrigo Fernando; Shectman, S.A.; Shporer, A.; Vezie, M.; Wang, S. X.; Zhou, G.
Año de publicación: 2023
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: 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.
Fil: Lillo Box, J.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
Fil: Gandolfi, D.. Università di Torino; Italia
Fil: Armstrong, D. J.. University of Warwick; Reino Unido
Fil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Nielsen, Louise D.. European Southern Observatory; Suiza
Fil: Luque, R.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España
Fil: Korth, J.. Chalmers University of Technology; Suecia
Fil: Sousa, S. G.. Universidad de Porto; Portugal
Fil: Quinn, S. N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Acuña, L.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Howell, S. B.. National Aeronautics and Space Administration; Estados Unidos
Fil: Morello, G.. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España
Fil: Hellier, C.. Keele University; Reino Unido
Fil: Giacalone, S.. University of California at Berkeley; Estados Unidos
Fil: Hoyer, S.. Aix Marseille Université; Francia
Fil: Stassun, K.. Vanderbilt University; Estados Unidos
Fil: Palle, E.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
Fil: Aguichine, A.. Aix Marseille Université; Francia
Fil: Mousis, O.. Aix Marseille Université; Francia
Fil: Adibekyan, V.. Universidad de Porto; Portugal. Centro de Astrofísica Da Universidade Do Porto; Portugal
Fil: Azevedo Silva, T.. Universidad de Porto; Portugal
Fil: Barrado, D.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España
Fil: Deleuil, M.. Aix Marseille Université; Francia
Fil: Eastman, J. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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
Fil: Shectman, S.A.. National Aeronautics and Space Administration; Estados Unidos
Fil: Shporer, A.. University of New Mexico; Estados Unidos
Fil: Vezie, M.. University of New Mexico; Estados Unidos
Fil: Wang, S. X.. Tsinghua University; China
Fil: Zhou, G.. University of Southern Queensland; Australia
Materia: PLANETS AND SATELLITES: COMPOSITION
PLANETS AND SATELLITES: DETECTION
PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: TOI-969
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
Nivel de accesibilidad: acceso abierto
Condiciones de uso: https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
Institución: Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador: oai:ri.conicet.gov.ar:11336/230504

Acceder

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repository_id_str	3498
network_name_str	CONICET Digital (CONICET)
spelling	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold JupiterLillo Box, J.Gandolfi, D.Armstrong, D. J.Collins, K. A.Nielsen, Louise D.Luque, R.Korth, J.Sousa, S. G.Quinn, S. N.Acuña, L.Howell, S. B.Morello, G.Hellier, C.Giacalone, S.Hoyer, S.Stassun, K.Palle, E.Aguichine, A.Mousis, O.Adibekyan, V.Azevedo Silva, T.Barrado, D.Deleuil, M.Eastman, J. D.Diaz, Rodrigo FernandoShectman, S.A.Shporer, A.Vezie, M.Wang, S. X.Zhou, G.PLANETS AND SATELLITES: COMPOSITIONPLANETS AND SATELLITES: DETECTIONPLANETS AND SATELLITES: FUNDAMENTAL PARAMETERSSTARS: INDIVIDUAL: TOI-969TECHNIQUES: PHOTOMETRICTECHNIQUES: RADIAL VELOCITIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. 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.Fil: Lillo Box, J.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; EspañaFil: Gandolfi, D.. Università di Torino; ItaliaFil: Armstrong, D. J.. University of Warwick; Reino UnidoFil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Nielsen, Louise D.. European Southern Observatory; SuizaFil: Luque, R.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Korth, J.. Chalmers University of Technology; SueciaFil: Sousa, S. G.. Universidad de Porto; PortugalFil: Quinn, S. N.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Acuña, L.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; FranciaFil: Howell, S. B.. National Aeronautics and Space Administration; Estados UnidosFil: Morello, G.. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; EspañaFil: Hellier, C.. Keele University; Reino UnidoFil: Giacalone, S.. University of California at Berkeley; Estados UnidosFil: Hoyer, S.. Aix Marseille Université; FranciaFil: Stassun, K.. Vanderbilt University; Estados UnidosFil: Palle, E.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; EspañaFil: Aguichine, A.. Aix Marseille Université; FranciaFil: Mousis, O.. Aix Marseille Université; FranciaFil: Adibekyan, V.. Universidad de Porto; Portugal. Centro de Astrofísica Da Universidade Do Porto; PortugalFil: Azevedo Silva, T.. Universidad de Porto; PortugalFil: Barrado, D.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; EspañaFil: Deleuil, M.. Aix Marseille Université; FranciaFil: Eastman, J. D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: 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; ArgentinaFil: Shectman, S.A.. National Aeronautics and Space Administration; Estados UnidosFil: Shporer, A.. University of New Mexico; Estados UnidosFil: Vezie, M.. University of New Mexico; Estados UnidosFil: Wang, S. X.. Tsinghua University; ChinaFil: Zhou, G.. University of Southern Queensland; AustraliaEDP Sciences2023-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/230504Lillo 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; 1-250004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202243879info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2023/01/aa43879-22/aa43879-22.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:08:44Zoai:ri.conicet.gov.ar:11336/230504instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:08:45.244CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
title	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
spellingShingle	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter Lillo Box, J. PLANETS AND SATELLITES: COMPOSITION PLANETS AND SATELLITES: DETECTION PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: TOI-969 TECHNIQUES: PHOTOMETRIC TECHNIQUES: RADIAL VELOCITIES
title_short	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
title_full	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
title_fullStr	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
title_full_unstemmed	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
title_sort	TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter
dc.creator.none.fl_str_mv	Lillo Box, J. Gandolfi, D. Armstrong, D. J. Collins, K. A. Nielsen, Louise D. Luque, R. Korth, J. Sousa, S. G. Quinn, S. N. Acuña, L. Howell, S. B. Morello, G. Hellier, C. Giacalone, S. Hoyer, S. Stassun, K. Palle, E. Aguichine, A. Mousis, O. Adibekyan, V. Azevedo Silva, T. Barrado, D. Deleuil, M. Eastman, J. D. Diaz, Rodrigo Fernando Shectman, S.A. Shporer, A. Vezie, M. Wang, S. X. Zhou, G.
author	Lillo Box, J.
author_facet	Lillo Box, J. Gandolfi, D. Armstrong, D. J. Collins, K. A. Nielsen, Louise D. Luque, R. Korth, J. Sousa, S. G. Quinn, S. N. Acuña, L. Howell, S. B. Morello, G. Hellier, C. Giacalone, S. Hoyer, S. Stassun, K. Palle, E. Aguichine, A. Mousis, O. Adibekyan, V. Azevedo Silva, T. Barrado, D. Deleuil, M. Eastman, J. D. Diaz, Rodrigo Fernando Shectman, S.A. Shporer, A. Vezie, M. Wang, S. X. Zhou, G.
author_role	author
author2	Gandolfi, D. Armstrong, D. J. Collins, K. A. Nielsen, Louise D. Luque, R. Korth, J. Sousa, S. G. Quinn, S. N. Acuña, L. Howell, S. B. Morello, G. Hellier, C. Giacalone, S. Hoyer, S. Stassun, K. Palle, E. Aguichine, A. Mousis, O. Adibekyan, V. Azevedo Silva, T. Barrado, D. Deleuil, M. Eastman, J. D. Diaz, Rodrigo Fernando Shectman, S.A. Shporer, A. Vezie, M. Wang, S. X. Zhou, G.
author2_role	author author author author author author author author author author author author author author author author author author author author author author author author author author author author author
dc.subject.none.fl_str_mv	PLANETS AND SATELLITES: COMPOSITION PLANETS AND SATELLITES: DETECTION PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: TOI-969 TECHNIQUES: PHOTOMETRIC TECHNIQUES: RADIAL VELOCITIES
topic	PLANETS AND SATELLITES: COMPOSITION PLANETS AND SATELLITES: DETECTION PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: TOI-969 TECHNIQUES: PHOTOMETRIC TECHNIQUES: RADIAL VELOCITIES
purl_subject.fl_str_mv	https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv	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. Fil: Lillo Box, J.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España Fil: Gandolfi, D.. Università di Torino; Italia Fil: Armstrong, D. J.. University of Warwick; Reino Unido Fil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Nielsen, Louise D.. European Southern Observatory; Suiza Fil: Luque, R.. Instituto de Astrofísica de Andalucía; España. Consejo Superior de Investigaciones Científicas; España Fil: Korth, J.. Chalmers University of Technology; Suecia Fil: Sousa, S. G.. Universidad de Porto; Portugal Fil: Quinn, S. N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Acuña, L.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia Fil: Howell, S. B.. National Aeronautics and Space Administration; Estados Unidos Fil: Morello, G.. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España Fil: Hellier, C.. Keele University; Reino Unido Fil: Giacalone, S.. University of California at Berkeley; Estados Unidos Fil: Hoyer, S.. Aix Marseille Université; Francia Fil: Stassun, K.. Vanderbilt University; Estados Unidos Fil: Palle, E.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España Fil: Aguichine, A.. Aix Marseille Université; Francia Fil: Mousis, O.. Aix Marseille Université; Francia Fil: Adibekyan, V.. Universidad de Porto; Portugal. Centro de Astrofísica Da Universidade Do Porto; Portugal Fil: Azevedo Silva, T.. Universidad de Porto; Portugal Fil: Barrado, D.. Consejo Superior de Investigaciones Científicas. Centro de Astrobiología; España Fil: Deleuil, M.. Aix Marseille Université; Francia Fil: Eastman, J. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos 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 Fil: Shectman, S.A.. National Aeronautics and Space Administration; Estados Unidos Fil: Shporer, A.. University of New Mexico; Estados Unidos Fil: Vezie, M.. University of New Mexico; Estados Unidos Fil: Wang, S. X.. Tsinghua University; China Fil: Zhou, G.. University of Southern Queensland; Australia
description	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.
publishDate	2023
dc.date.none.fl_str_mv	2023-01
dc.type.none.fl_str_mv	info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo
format	article
status_str	publishedVersion
dc.identifier.none.fl_str_mv	http://hdl.handle.net/11336/230504 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 0004-6361 CONICET Digital CONICET
url	http://hdl.handle.net/11336/230504
identifier_str_mv	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 0004-6361 CONICET Digital CONICET
dc.language.none.fl_str_mv	eng
language	eng
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dc.rights.none.fl_str_mv	info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
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rights_invalid_str_mv	https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
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dc.publisher.none.fl_str_mv	EDP Sciences
publisher.none.fl_str_mv	EDP Sciences
dc.source.none.fl_str_mv	reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas
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repository.name.fl_str_mv	CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv	dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score	13.22299

TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter

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