A He I upper atmosphere around the warm Neptune GJ 3470 b

High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of plane...

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Detalles Bibliográficos
Autores: Cortés Contreras, Miriam, Montes Gutiérrez, David
Tipo de recurso: artículo
Fecha de publicación:2020
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/6502
Acceso en línea:https://hdl.handle.net/20.500.14352/6502
Access Level:acceso abierto
Palabra clave:52
High-resolution spectroscopy
Mass
Stars
Absorption
Parameters
Exoplanets
Astrofísica
Astronomía (Física)
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spelling A He I upper atmosphere around the warm Neptune GJ 3470 bCortés Contreras, MiriamMontes Gutiérrez, David52High-resolution spectroscopyMassStarsAbsorptionParametersExoplanetsAstrofísicaAstronomía (Física)High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of planetary systems. Here, we report our observations of three transits of GJ 3470 b with CARMENES in search of He (23S) absorption. On one of the nights, the He I region was heavily contaminated by OH− telluric emission and, thus, it was not useful for our purposes. The remaining two nights had a very different signal-to-noise ratio (S/N) due to weather. They both indicate the presence of He (2^(3)S) absorption in the transmission spectrum of GJ 3470 b , although a statistically valid detection can only be claimed for the night with higher S/N. For that night, we retrieved a 1.5 ± 0.3% absorption depth, translating into a R_(p)(λ)/R_(p) = 1.15 ± 0.14 at this wavelength. Spectro-photometric light curves for this same night also indicate the presence of extra absorption during the planetary transit with a consistent absorption depth. The He (2^(3)S) absorption is modeled in detail using a radiative transfer code, and the results of our modeling efforts are compared to the observations. We find that the mass-loss rate, Ṁ , is confined to a range of 3 × 10^(10) g s^(−1) for T = 6000 K to 10 × 10^(10) g s^(−1) for T = 9000 K. We discuss the physical mechanisms and implications of the He I detection in GJ 3470 b and put it in context as compared to similar detections and non-detections in other Neptune-size planets. We also present improved stellar and planetary parameter determinations based on our visible and near-infrared observations.EDP ScienciesUniversidad Complutense de Madrid20202020-06-1120202020-06-11journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/6502reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/65022026-06-02T12:44:21Z
dc.title.none.fl_str_mv A He I upper atmosphere around the warm Neptune GJ 3470 b
title A He I upper atmosphere around the warm Neptune GJ 3470 b
spellingShingle A He I upper atmosphere around the warm Neptune GJ 3470 b
Cortés Contreras, Miriam
52
High-resolution spectroscopy
Mass
Stars
Absorption
Parameters
Exoplanets
Astrofísica
Astronomía (Física)
title_short A He I upper atmosphere around the warm Neptune GJ 3470 b
title_full A He I upper atmosphere around the warm Neptune GJ 3470 b
title_fullStr A He I upper atmosphere around the warm Neptune GJ 3470 b
title_full_unstemmed A He I upper atmosphere around the warm Neptune GJ 3470 b
title_sort A He I upper atmosphere around the warm Neptune GJ 3470 b
dc.creator.none.fl_str_mv Cortés Contreras, Miriam
Montes Gutiérrez, David
author Cortés Contreras, Miriam
author_facet Cortés Contreras, Miriam
Montes Gutiérrez, David
author_role author
author2 Montes Gutiérrez, David
author2_role author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 52
High-resolution spectroscopy
Mass
Stars
Absorption
Parameters
Exoplanets
Astrofísica
Astronomía (Física)
topic 52
High-resolution spectroscopy
Mass
Stars
Absorption
Parameters
Exoplanets
Astrofísica
Astronomía (Física)
description High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of planetary systems. Here, we report our observations of three transits of GJ 3470 b with CARMENES in search of He (23S) absorption. On one of the nights, the He I region was heavily contaminated by OH− telluric emission and, thus, it was not useful for our purposes. The remaining two nights had a very different signal-to-noise ratio (S/N) due to weather. They both indicate the presence of He (2^(3)S) absorption in the transmission spectrum of GJ 3470 b , although a statistically valid detection can only be claimed for the night with higher S/N. For that night, we retrieved a 1.5 ± 0.3% absorption depth, translating into a R_(p)(λ)/R_(p) = 1.15 ± 0.14 at this wavelength. Spectro-photometric light curves for this same night also indicate the presence of extra absorption during the planetary transit with a consistent absorption depth. The He (2^(3)S) absorption is modeled in detail using a radiative transfer code, and the results of our modeling efforts are compared to the observations. We find that the mass-loss rate, Ṁ , is confined to a range of 3 × 10^(10) g s^(−1) for T = 6000 K to 10 × 10^(10) g s^(−1) for T = 9000 K. We discuss the physical mechanisms and implications of the He I detection in GJ 3470 b and put it in context as compared to similar detections and non-detections in other Neptune-size planets. We also present improved stellar and planetary parameter determinations based on our visible and near-infrared observations.
publishDate 2020
dc.date.none.fl_str_mv 2020
2020-06-11
2020
2020-06-11
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/20.500.14352/6502
url https://hdl.handle.net/20.500.14352/6502
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
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
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
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