TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley

We report the discovery and characterization of two small transiting planets orbiting the bright M3.0 V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the planetary nature of both of them using prec...

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Detalles Bibliográficos
Autores: Caballero, J. A., Cifuentes, C., Montes Gutiérrez, David, otros, ...
Tipo de recurso: artículo
Fecha de publicación:2022
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/72735
Acceso en línea:https://hdl.handle.net/20.500.14352/72735
Access Level:acceso abierto
Palabra clave:52
Powered mass-loss
Irradiated gaseous exoplanets
Lomb-Scargle periodogram
M-dwarfs
Habitable-zone
Error-correction
Adaptive optics
Stellar
Catalog
Stars
Astrofísica
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network_acronym_str ES
network_name_str España
repository_id_str
spelling TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valleyCaballero, J. A.Cifuentes, C.Montes Gutiérrez, Davidotros, ...52Powered mass-lossIrradiated gaseous exoplanetsLomb-Scargle periodogramM-dwarfsHabitable-zoneError-correctionAdaptive opticsStellarCatalogStarsAstrofísicaWe report the discovery and characterization of two small transiting planets orbiting the bright M3.0 V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b (P_(b) = 1.88 d), has a planetary mass of M_(b) = 3.21 ± 0.24 M_(ꚛ) and a radius of R_(b) = 1.280^(+0.038)_(−0.039) R_(ꚛ), resulting in a density of ρ_(b) = 8.39^(+1.05)_(−0.92) g cm^(−3) , which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c (P_(c) = 15.53 d), we derive a mass of M_(c) = 6.64^(+0.67)_(−0.68) M_(ꚛ), a radius of R_(c) = 2.06 ± 0.04 R_(ꚛ), and a bulk density of ρ_(c) = 2.00^(+0.21)_(−0.19) g cm^(−3) , which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.EDP ScienciesUniversidad Complutense de Madrid20222022-10-2120222022-10-21journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/72735reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Atribución 3.0 Españahttps://creativecommons.org/licenses/by/3.0/es/info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/727352026-06-02T12:44:21Z
dc.title.none.fl_str_mv TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
title TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
spellingShingle TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
Caballero, J. A.
52
Powered mass-loss
Irradiated gaseous exoplanets
Lomb-Scargle periodogram
M-dwarfs
Habitable-zone
Error-correction
Adaptive optics
Stellar
Catalog
Stars
Astrofísica
title_short TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
title_full TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
title_fullStr TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
title_full_unstemmed TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
title_sort TOI-1468: a system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
dc.creator.none.fl_str_mv Caballero, J. A.
Cifuentes, C.
Montes Gutiérrez, David
otros, ...
author Caballero, J. A.
author_facet Caballero, J. A.
Cifuentes, C.
Montes Gutiérrez, David
otros, ...
author_role author
author2 Cifuentes, C.
Montes Gutiérrez, David
otros, ...
author2_role author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 52
Powered mass-loss
Irradiated gaseous exoplanets
Lomb-Scargle periodogram
M-dwarfs
Habitable-zone
Error-correction
Adaptive optics
Stellar
Catalog
Stars
Astrofísica
topic 52
Powered mass-loss
Irradiated gaseous exoplanets
Lomb-Scargle periodogram
M-dwarfs
Habitable-zone
Error-correction
Adaptive optics
Stellar
Catalog
Stars
Astrofísica
description We report the discovery and characterization of two small transiting planets orbiting the bright M3.0 V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b (P_(b) = 1.88 d), has a planetary mass of M_(b) = 3.21 ± 0.24 M_(ꚛ) and a radius of R_(b) = 1.280^(+0.038)_(−0.039) R_(ꚛ), resulting in a density of ρ_(b) = 8.39^(+1.05)_(−0.92) g cm^(−3) , which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c (P_(c) = 15.53 d), we derive a mass of M_(c) = 6.64^(+0.67)_(−0.68) M_(ꚛ), a radius of R_(c) = 2.06 ± 0.04 R_(ꚛ), and a bulk density of ρ_(c) = 2.00^(+0.21)_(−0.19) g cm^(−3) , which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022-10-21
2022
2022-10-21
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/72735
url https://hdl.handle.net/20.500.14352/72735
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución 3.0 España
https://creativecommons.org/licenses/by/3.0/es/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución 3.0 España
https://creativecommons.org/licenses/by/3.0/es/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciencies
publisher.none.fl_str_mv EDP Sciencies
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869405585077698560
score 15,301629

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