TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf
- Autores
- Schanche, N.; Pozuelos, F. J.; Günther, M. N.; Wells, R. D.; Burgasser, A. J.; Chinchilla, P.; Delrez, L.; Ducrot, E.; Garcia, L. J.; Gómez Maqueo Chew, Y.; Jofre, Jorge Emiliano; Rackham, B. V.; Sebastian, D.; Stassun, K. G.; Stern, D.; Timmermans, M.; Barkaoui, K.; Belinski, A.; Benkhaldoun, Z.; Benz, W.; Bieryla, A.; Bouchy, F.; Burdanov, A.; Charbonneau, D.; Christiansen, J. L.; Collins, K. A.; Demory, Brice Olivier; Dévora Pajares, M.; De Wit, J.; Dragomir, D.
- Año de publicación
- 2022
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e ∼ 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star. Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R⊕ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet’s low equilibrium temperature (∼256 K), its host star’s small size (R∗ = 0.311 ± 0.015) and relative infrared brightness (Kmag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy.
Fil: Schanche, N.. University of Bern; Suiza
Fil: Pozuelos, F. J.. Université de Liège; Bélgica
Fil: Günther, M. N.. Massachusetts Institute of Technology; Estados Unidos. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos
Fil: Wells, R. D.. University of Bern; Suiza
Fil: Burgasser, A. J.. University of California at San Diego; Estados Unidos
Fil: Chinchilla, P.. Université de Liège; Bélgica. Instituto de Astrofísica de Canarias; España
Fil: Delrez, L.. Université de Liège; Bélgica
Fil: Ducrot, E.. Université de Liège; Bélgica
Fil: Garcia, L. J.. Université de Liège; Bélgica
Fil: Gómez Maqueo Chew, Y.. Universidad Nacional Autónoma de México. Instituto de Astronomía; México
Fil: Jofre, Jorge Emiliano. Universidad Nacional Autónoma de México. Instituto de Astronomía; México. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Rackham, B. V.. Massachusetts Institute of Technology; Estados Unidos
Fil: Sebastian, D.. University of Birmingham; Reino Unido
Fil: Stassun, K. G.. Vanderbilt University; Estados Unidos
Fil: Stern, D.. California Instituto Of Technology. Departament Of Mechanical And Civil Engineering; Estados Unidos
Fil: Timmermans, M.. Université de Liège; Bélgica
Fil: Barkaoui, K.. Université de Liège; Bélgica. Cadi Ayyad University; Marruecos
Fil: Belinski, A.. Moscow State University; Rusia
Fil: Benkhaldoun, Z.. Cadi Ayyad University; Marruecos
Fil: Benz, W.. University of Bern; Suiza
Fil: Bieryla, A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Bouchy, F.. Observatorio de Ginebra; Suiza
Fil: Burdanov, A.. Massachusetts Institute of Technology; Estados Unidos
Fil: Charbonneau, D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Christiansen, J. L.. Centro de Análisis y Procesamiento Infrarrojo; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos
Fil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Demory, Brice Olivier. University of Bern; Suiza
Fil: Dévora Pajares, M.. Universidad de Granada; España
Fil: De Wit, J.. Massachusetts Institute of Technology; Estados Unidos
Fil: Dragomir, D.. University of New Mexico; Estados Unidos - Materia
-
PLANETS AND SATELLITES: DETECTION
STARS: INDIVIDUAL: TIC 198485881
STARS: INDIVIDUAL: TOI-2257
TECHNIQUES: PHOTOMETRIC - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/188864
Ver los metadatos del registro completo
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TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarfSchanche, N.Pozuelos, F. J.Günther, M. N.Wells, R. D.Burgasser, A. J.Chinchilla, P.Delrez, L.Ducrot, E.Garcia, L. J.Gómez Maqueo Chew, Y.Jofre, Jorge EmilianoRackham, B. V.Sebastian, D.Stassun, K. G.Stern, D.Timmermans, M.Barkaoui, K.Belinski, A.Benkhaldoun, Z.Benz, W.Bieryla, A.Bouchy, F.Burdanov, A.Charbonneau, D.Christiansen, J. L.Collins, K. A.Demory, Brice OlivierDévora Pajares, M.De Wit, J.Dragomir, D.PLANETS AND SATELLITES: DETECTIONSTARS: INDIVIDUAL: TIC 198485881STARS: INDIVIDUAL: TOI-2257TECHNIQUES: PHOTOMETRIChttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e ∼ 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star. Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R⊕ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet’s low equilibrium temperature (∼256 K), its host star’s small size (R∗ = 0.311 ± 0.015) and relative infrared brightness (Kmag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy.Fil: Schanche, N.. University of Bern; SuizaFil: Pozuelos, F. J.. Université de Liège; BélgicaFil: Günther, M. N.. Massachusetts Institute of Technology; Estados Unidos. Agencia Espacial Europea. European Space Research And Technology Centre.; Países BajosFil: Wells, R. D.. University of Bern; SuizaFil: Burgasser, A. J.. University of California at San Diego; Estados UnidosFil: Chinchilla, P.. Université de Liège; Bélgica. Instituto de Astrofísica de Canarias; EspañaFil: Delrez, L.. Université de Liège; BélgicaFil: Ducrot, E.. Université de Liège; BélgicaFil: Garcia, L. J.. Université de Liège; BélgicaFil: Gómez Maqueo Chew, Y.. Universidad Nacional Autónoma de México. Instituto de Astronomía; MéxicoFil: Jofre, Jorge Emiliano. Universidad Nacional Autónoma de México. Instituto de Astronomía; México. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Rackham, B. V.. Massachusetts Institute of Technology; Estados UnidosFil: Sebastian, D.. University of Birmingham; Reino UnidoFil: Stassun, K. G.. Vanderbilt University; Estados UnidosFil: Stern, D.. California Instituto Of Technology. Departament Of Mechanical And Civil Engineering; Estados UnidosFil: Timmermans, M.. Université de Liège; BélgicaFil: Barkaoui, K.. Université de Liège; Bélgica. Cadi Ayyad University; MarruecosFil: Belinski, A.. Moscow State University; RusiaFil: Benkhaldoun, Z.. Cadi Ayyad University; MarruecosFil: Benz, W.. University of Bern; SuizaFil: Bieryla, A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Bouchy, F.. Observatorio de Ginebra; SuizaFil: Burdanov, A.. Massachusetts Institute of Technology; Estados UnidosFil: Charbonneau, D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Christiansen, J. L.. Centro de Análisis y Procesamiento Infrarrojo; Estados Unidos. National Aeronautics and Space Administration; Estados UnidosFil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Demory, Brice Olivier. University of Bern; SuizaFil: Dévora Pajares, M.. Universidad de Granada; EspañaFil: De Wit, J.. Massachusetts Institute of Technology; Estados UnidosFil: Dragomir, D.. University of New Mexico; Estados UnidosEDP Sciences2022-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/188864Schanche, N.; Pozuelos, F. J.; Günther, M. N.; Wells, R. D.; Burgasser, A. J.; et al.; TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf; EDP Sciences; Astronomy and Astrophysics; 657; 1-2022; 1-180004-63611432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2022/01/aa42280-21/aa42280-21.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202142280info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2111.01749info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:36:22Zoai:ri.conicet.gov.ar:11336/188864instacron: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 14:36:22.319CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| title |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| spellingShingle |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf Schanche, N. PLANETS AND SATELLITES: DETECTION STARS: INDIVIDUAL: TIC 198485881 STARS: INDIVIDUAL: TOI-2257 TECHNIQUES: PHOTOMETRIC |
| title_short |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| title_full |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| title_fullStr |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| title_full_unstemmed |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| title_sort |
TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf |
| dc.creator.none.fl_str_mv |
Schanche, N. Pozuelos, F. J. Günther, M. N. Wells, R. D. Burgasser, A. J. Chinchilla, P. Delrez, L. Ducrot, E. Garcia, L. J. Gómez Maqueo Chew, Y. Jofre, Jorge Emiliano Rackham, B. V. Sebastian, D. Stassun, K. G. Stern, D. Timmermans, M. Barkaoui, K. Belinski, A. Benkhaldoun, Z. Benz, W. Bieryla, A. Bouchy, F. Burdanov, A. Charbonneau, D. Christiansen, J. L. Collins, K. A. Demory, Brice Olivier Dévora Pajares, M. De Wit, J. Dragomir, D. |
| author |
Schanche, N. |
| author_facet |
Schanche, N. Pozuelos, F. J. Günther, M. N. Wells, R. D. Burgasser, A. J. Chinchilla, P. Delrez, L. Ducrot, E. Garcia, L. J. Gómez Maqueo Chew, Y. Jofre, Jorge Emiliano Rackham, B. V. Sebastian, D. Stassun, K. G. Stern, D. Timmermans, M. Barkaoui, K. Belinski, A. Benkhaldoun, Z. Benz, W. Bieryla, A. Bouchy, F. Burdanov, A. Charbonneau, D. Christiansen, J. L. Collins, K. A. Demory, Brice Olivier Dévora Pajares, M. De Wit, J. Dragomir, D. |
| author_role |
author |
| author2 |
Pozuelos, F. J. Günther, M. N. Wells, R. D. Burgasser, A. J. Chinchilla, P. Delrez, L. Ducrot, E. Garcia, L. J. Gómez Maqueo Chew, Y. Jofre, Jorge Emiliano Rackham, B. V. Sebastian, D. Stassun, K. G. Stern, D. Timmermans, M. Barkaoui, K. Belinski, A. Benkhaldoun, Z. Benz, W. Bieryla, A. Bouchy, F. Burdanov, A. Charbonneau, D. Christiansen, J. L. Collins, K. A. Demory, Brice Olivier Dévora Pajares, M. De Wit, J. Dragomir, D. |
| 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: DETECTION STARS: INDIVIDUAL: TIC 198485881 STARS: INDIVIDUAL: TOI-2257 TECHNIQUES: PHOTOMETRIC |
| topic |
PLANETS AND SATELLITES: DETECTION STARS: INDIVIDUAL: TIC 198485881 STARS: INDIVIDUAL: TOI-2257 TECHNIQUES: PHOTOMETRIC |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.7 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e ∼ 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star. Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R⊕ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet’s low equilibrium temperature (∼256 K), its host star’s small size (R∗ = 0.311 ± 0.015) and relative infrared brightness (Kmag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy. Fil: Schanche, N.. University of Bern; Suiza Fil: Pozuelos, F. J.. Université de Liège; Bélgica Fil: Günther, M. N.. Massachusetts Institute of Technology; Estados Unidos. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos Fil: Wells, R. D.. University of Bern; Suiza Fil: Burgasser, A. J.. University of California at San Diego; Estados Unidos Fil: Chinchilla, P.. Université de Liège; Bélgica. Instituto de Astrofísica de Canarias; España Fil: Delrez, L.. Université de Liège; Bélgica Fil: Ducrot, E.. Université de Liège; Bélgica Fil: Garcia, L. J.. Université de Liège; Bélgica Fil: Gómez Maqueo Chew, Y.. Universidad Nacional Autónoma de México. Instituto de Astronomía; México Fil: Jofre, Jorge Emiliano. Universidad Nacional Autónoma de México. Instituto de Astronomía; México. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina Fil: Rackham, B. V.. Massachusetts Institute of Technology; Estados Unidos Fil: Sebastian, D.. University of Birmingham; Reino Unido Fil: Stassun, K. G.. Vanderbilt University; Estados Unidos Fil: Stern, D.. California Instituto Of Technology. Departament Of Mechanical And Civil Engineering; Estados Unidos Fil: Timmermans, M.. Université de Liège; Bélgica Fil: Barkaoui, K.. Université de Liège; Bélgica. Cadi Ayyad University; Marruecos Fil: Belinski, A.. Moscow State University; Rusia Fil: Benkhaldoun, Z.. Cadi Ayyad University; Marruecos Fil: Benz, W.. University of Bern; Suiza Fil: Bieryla, A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Bouchy, F.. Observatorio de Ginebra; Suiza Fil: Burdanov, A.. Massachusetts Institute of Technology; Estados Unidos Fil: Charbonneau, D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Christiansen, J. L.. Centro de Análisis y Procesamiento Infrarrojo; Estados Unidos. National Aeronautics and Space Administration; Estados Unidos Fil: Collins, K. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Demory, Brice Olivier. University of Bern; Suiza Fil: Dévora Pajares, M.. Universidad de Granada; España Fil: De Wit, J.. Massachusetts Institute of Technology; Estados Unidos Fil: Dragomir, D.. University of New Mexico; Estados Unidos |
| description |
Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e ∼ 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star. Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R⊕ and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet’s low equilibrium temperature (∼256 K), its host star’s small size (R∗ = 0.311 ± 0.015) and relative infrared brightness (Kmag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy. |
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2022 |
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2022-01 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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http://hdl.handle.net/11336/188864 Schanche, N.; Pozuelos, F. J.; Günther, M. N.; Wells, R. D.; Burgasser, A. J.; et al.; TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf; EDP Sciences; Astronomy and Astrophysics; 657; 1-2022; 1-18 0004-6361 1432-0746 CONICET Digital CONICET |
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http://hdl.handle.net/11336/188864 |
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Schanche, N.; Pozuelos, F. J.; Günther, M. N.; Wells, R. D.; Burgasser, A. J.; et al.; TOI-2257 b: A highly eccentric long-period sub-Neptune transiting a nearby M dwarf; EDP Sciences; Astronomy and Astrophysics; 657; 1-2022; 1-18 0004-6361 1432-0746 CONICET Digital CONICET |
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