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...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/233670 |
| Acceso en línea: | http://hdl.handle.net/10261/233670 |
| Access Level: | acceso abierto |
| id |
ES_a050b794aab4cf96a062bcaa780b072e |
|---|---|
| oai_identifier_str |
oai:digital.csic.es:10261/233670 |
| network_acronym_str |
ES |
| network_name_str |
España |
| repository_id_str |
|
| spelling |
A He i upper atmosphere around the warm Neptune GJ 3470 bPallé, EnricNortmann, L.Casasayas-Barris, N.Lampón, M.López-Puertas, ManuelCaballero, J. A.Sanz-Forcada, J.Lara, Luisa MaríaNagel, EvangelosYan, F.Alonso-Floriano, F. JavierAmado, Pedro J.Chen, G.Cifuentes, C.Cortés-Contreras, M.Czesla, S.Molaverdikhani, K.Montes, DavidPassegger, V.M.Quirrenbach, AndreasReiners, AnsgarRibas, IgnasiSánchez-López, Ángela MaríaSchweitzer, AndreasStangret, M.Zapatero Osorio, María RosaZechmeister, MathiasHigh 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 (23S) 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 Rp(λ)\Rp = 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 (23S) 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, is confined to a range of 3 × 1010 g s-1 for T = 6000 K to 10 × 1010 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.With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)Springer NatureConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501http://hdl.handle.net/10261/233670reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://dx.doi.org/10.1051/0004-6361/202037719Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2336702026-05-22T06:33:51Z |
| 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 Pallé, Enric |
| 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 |
Pallé, Enric Nortmann, L. Casasayas-Barris, N. Lampón, M. López-Puertas, Manuel Caballero, J. A. Sanz-Forcada, J. Lara, Luisa María Nagel, Evangelos Yan, F. Alonso-Floriano, F. Javier Amado, Pedro J. Chen, G. Cifuentes, C. Cortés-Contreras, M. Czesla, S. Molaverdikhani, K. Montes, David Passegger, V.M. Quirrenbach, Andreas Reiners, Ansgar Ribas, Ignasi Sánchez-López, Ángela María Schweitzer, Andreas Stangret, M. Zapatero Osorio, María Rosa Zechmeister, Mathias |
| author |
Pallé, Enric |
| author_facet |
Pallé, Enric Nortmann, L. Casasayas-Barris, N. Lampón, M. López-Puertas, Manuel Caballero, J. A. Sanz-Forcada, J. Lara, Luisa María Nagel, Evangelos Yan, F. Alonso-Floriano, F. Javier Amado, Pedro J. Chen, G. Cifuentes, C. Cortés-Contreras, M. Czesla, S. Molaverdikhani, K. Montes, David Passegger, V.M. Quirrenbach, Andreas Reiners, Ansgar Ribas, Ignasi Sánchez-López, Ángela María Schweitzer, Andreas Stangret, M. Zapatero Osorio, María Rosa Zechmeister, Mathias |
| author_role |
author |
| author2 |
Nortmann, L. Casasayas-Barris, N. Lampón, M. López-Puertas, Manuel Caballero, J. A. Sanz-Forcada, J. Lara, Luisa María Nagel, Evangelos Yan, F. Alonso-Floriano, F. Javier Amado, Pedro J. Chen, G. Cifuentes, C. Cortés-Contreras, M. Czesla, S. Molaverdikhani, K. Montes, David Passegger, V.M. Quirrenbach, Andreas Reiners, Ansgar Ribas, Ignasi Sánchez-López, Ángela María Schweitzer, Andreas Stangret, M. Zapatero Osorio, María Rosa Zechmeister, Mathias |
| 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 |
| dc.contributor.none.fl_str_mv |
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| 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 (23S) 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 Rp(λ)\Rp = 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 (23S) 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, is confined to a range of 3 × 1010 g s-1 for T = 6000 K to 10 × 1010 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 2021 2021 2021 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 |
| format |
article |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/233670 |
| url |
http://hdl.handle.net/10261/233670 |
| dc.language.none.fl_str_mv |
Inglés |
| language_invalid_str_mv |
Inglés |
| dc.relation.none.fl_str_mv |
http://dx.doi.org/10.1051/0004-6361/202037719 Sí |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess |
| eu_rights_str_mv |
openAccess |
| dc.publisher.none.fl_str_mv |
Springer Nature |
| publisher.none.fl_str_mv |
Springer Nature |
| 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_ |
1869415000632721408 |
| score |
15.811543 |