Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials

Autores
Duvvuri, Girish M.; Pineda, J. Sebastian; Berta Thompson, Zachory; Brown, Alexander; France, K.; Kowalski, A.; Redfield, S.; Tilipman, Dennis; Vieytes, Mariela Cristina; Wilson, David J.; Youngblood, Allison; Froning, C.; Linsky, J. L.; Parke Loyd, R. O.; Mauas, Pablo Jacobo David; Miguel, Yamila; Newton, Elisabeth R.; Rugheimer, Sarah; Christian Schneider, P.
Año de publicación
2021
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Characterizing the atmospheres of planets orbiting M dwarfs requires understanding the spectral energy distributions of M dwarfs over planetary lifetimes. Surveys like MUSCLES, HAZMAT, and FUMES have collected multiwavelength spectra across the spectral type's range of T eff and activity, but the extreme ultraviolet (EUV, 100-912 Å) flux of most of these stars remains unobserved because of obscuration by the interstellar medium compounded with limited detector sensitivity. While targets with observable EUV flux exist, there is no currently operational facility observing between 150 and 912 Å. Inferring the spectra of exoplanet hosts in this regime is critical to studying the evolution of planetary atmospheres because the EUV heats the top of the thermosphere and drives atmospheric escape. This paper presents our implementation of the differential emission measure technique to reconstruct the EUV spectra of cool dwarfs. We characterize our method's accuracy and precision by applying it to the Sun and AU Mic. We then apply it to three fainter M dwarfs: GJ 832, Barnard's star, and TRAPPIST-1. We demonstrate that with the strongest far-ultraviolet (FUV, 912-1700 Å) emission lines, observed with the Hubble Space Telescope and/or Far Ultraviolet Spectroscopic Explorer, and a coarse X-ray spectrum from either the Chandra X-ray Observatory or XMM-Newton, we can reconstruct the Sun's EUV spectrum to within a factor of 1.8, with our model's formal uncertainties encompassing the data. We report the integrated EUV flux of our M dwarf sample with uncertainties of a factor of 2-7 depending on available data quality.
Fil: Duvvuri, Girish M.. State University of Colorado at Boulder; Estados Unidos
Fil: Pineda, J. Sebastian. State University of Colorado at Boulder; Estados Unidos
Fil: Berta Thompson, Zachory. State University of Colorado at Boulder; Estados Unidos
Fil: Brown, Alexander. State University of Colorado at Boulder; Estados Unidos
Fil: France, K.. State University of Colorado at Boulder; Estados Unidos
Fil: Kowalski, A.. State University of Colorado at Boulder; Estados Unidos
Fil: Redfield, S.. State University of Colorado at Boulder; Estados Unidos
Fil: Tilipman, Dennis. State University of Colorado at Boulder; Estados Unidos
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wilson, David J.. State University of Colorado at Boulder; Estados Unidos
Fil: Youngblood, Allison. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, C.. State University of Colorado at Boulder; Estados Unidos
Fil: Linsky, J. L.. State University of Colorado at Boulder; Estados Unidos
Fil: Parke Loyd, R. O.. State University of Colorado at Boulder; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones 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: Miguel, Yamila. State University of Colorado at Boulder; Estados Unidos
Fil: Newton, Elisabeth R.. State University of Colorado at Boulder; Estados Unidos
Fil: Rugheimer, Sarah. State University of Colorado at Boulder; Estados Unidos
Fil: Christian Schneider, P.. State University of Colorado at Boulder; Estados Unidos
Materia
Solar and Stellar Astrophysics
Earth and Planetary Astrophysics
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/182676
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/182676
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure PolynomialsDuvvuri, Girish M.Pineda, J. SebastianBerta Thompson, ZachoryBrown, AlexanderFrance, K.Kowalski, A.Redfield, S.Tilipman, DennisVieytes, Mariela CristinaWilson, David J.Youngblood, AllisonFroning, C.Linsky, J. L.Parke Loyd, R. O.Mauas, Pablo Jacobo DavidMiguel, YamilaNewton, Elisabeth R.Rugheimer, SarahChristian Schneider, P.Solar and Stellar AstrophysicsEarth and Planetary Astrophysicshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Characterizing the atmospheres of planets orbiting M dwarfs requires understanding the spectral energy distributions of M dwarfs over planetary lifetimes. Surveys like MUSCLES, HAZMAT, and FUMES have collected multiwavelength spectra across the spectral type's range of T eff and activity, but the extreme ultraviolet (EUV, 100-912 Å) flux of most of these stars remains unobserved because of obscuration by the interstellar medium compounded with limited detector sensitivity. While targets with observable EUV flux exist, there is no currently operational facility observing between 150 and 912 Å. Inferring the spectra of exoplanet hosts in this regime is critical to studying the evolution of planetary atmospheres because the EUV heats the top of the thermosphere and drives atmospheric escape. This paper presents our implementation of the differential emission measure technique to reconstruct the EUV spectra of cool dwarfs. We characterize our method's accuracy and precision by applying it to the Sun and AU Mic. We then apply it to three fainter M dwarfs: GJ 832, Barnard's star, and TRAPPIST-1. We demonstrate that with the strongest far-ultraviolet (FUV, 912-1700 Å) emission lines, observed with the Hubble Space Telescope and/or Far Ultraviolet Spectroscopic Explorer, and a coarse X-ray spectrum from either the Chandra X-ray Observatory or XMM-Newton, we can reconstruct the Sun's EUV spectrum to within a factor of 1.8, with our model's formal uncertainties encompassing the data. We report the integrated EUV flux of our M dwarf sample with uncertainties of a factor of 2-7 depending on available data quality.Fil: Duvvuri, Girish M.. State University of Colorado at Boulder; Estados UnidosFil: Pineda, J. Sebastian. State University of Colorado at Boulder; Estados UnidosFil: Berta Thompson, Zachory. State University of Colorado at Boulder; Estados UnidosFil: Brown, Alexander. State University of Colorado at Boulder; Estados UnidosFil: France, K.. State University of Colorado at Boulder; Estados UnidosFil: Kowalski, A.. State University of Colorado at Boulder; Estados UnidosFil: Redfield, S.. State University of Colorado at Boulder; Estados UnidosFil: Tilipman, Dennis. State University of Colorado at Boulder; Estados UnidosFil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wilson, David J.. State University of Colorado at Boulder; Estados UnidosFil: Youngblood, Allison. State University of Colorado at Boulder; Estados UnidosFil: Froning, C.. State University of Colorado at Boulder; Estados UnidosFil: Linsky, J. L.. State University of Colorado at Boulder; Estados UnidosFil: Parke Loyd, R. O.. State University of Colorado at Boulder; Estados UnidosFil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones 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: Miguel, Yamila. State University of Colorado at Boulder; Estados UnidosFil: Newton, Elisabeth R.. State University of Colorado at Boulder; Estados UnidosFil: Rugheimer, Sarah. State University of Colorado at Boulder; Estados UnidosFil: Christian Schneider, P.. State University of Colorado at Boulder; Estados UnidosIOP Publishing2021-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/182676Duvvuri, Girish M.; Pineda, J. Sebastian; Berta Thompson, Zachory; Brown, Alexander; France, K.; et al.; Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials; IOP Publishing; Astrophysical Journal; 913; 1; 5-2021; 1-370004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abeaafinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abeaafinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-11-12T09:56:32Zoai:ri.conicet.gov.ar:11336/182676instacron: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:34982025-11-12 09:56:33.155CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
title Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
spellingShingle Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
Duvvuri, Girish M.
Solar and Stellar Astrophysics
Earth and Planetary Astrophysics
title_short Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
title_full Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
title_fullStr Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
title_full_unstemmed Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
title_sort Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
dc.creator.none.fl_str_mv Duvvuri, Girish M.
Pineda, J. Sebastian
Berta Thompson, Zachory
Brown, Alexander
France, K.
Kowalski, A.
Redfield, S.
Tilipman, Dennis
Vieytes, Mariela Cristina
Wilson, David J.
Youngblood, Allison
Froning, C.
Linsky, J. L.
Parke Loyd, R. O.
Mauas, Pablo Jacobo David
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Christian Schneider, P.
author Duvvuri, Girish M.
author_facet Duvvuri, Girish M.
Pineda, J. Sebastian
Berta Thompson, Zachory
Brown, Alexander
France, K.
Kowalski, A.
Redfield, S.
Tilipman, Dennis
Vieytes, Mariela Cristina
Wilson, David J.
Youngblood, Allison
Froning, C.
Linsky, J. L.
Parke Loyd, R. O.
Mauas, Pablo Jacobo David
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Christian Schneider, P.
author_role author
author2 Pineda, J. Sebastian
Berta Thompson, Zachory
Brown, Alexander
France, K.
Kowalski, A.
Redfield, S.
Tilipman, Dennis
Vieytes, Mariela Cristina
Wilson, David J.
Youngblood, Allison
Froning, C.
Linsky, J. L.
Parke Loyd, R. O.
Mauas, Pablo Jacobo David
Miguel, Yamila
Newton, Elisabeth R.
Rugheimer, Sarah
Christian Schneider, P.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Solar and Stellar Astrophysics
Earth and Planetary Astrophysics
topic Solar and Stellar Astrophysics
Earth and Planetary Astrophysics
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Characterizing the atmospheres of planets orbiting M dwarfs requires understanding the spectral energy distributions of M dwarfs over planetary lifetimes. Surveys like MUSCLES, HAZMAT, and FUMES have collected multiwavelength spectra across the spectral type's range of T eff and activity, but the extreme ultraviolet (EUV, 100-912 Å) flux of most of these stars remains unobserved because of obscuration by the interstellar medium compounded with limited detector sensitivity. While targets with observable EUV flux exist, there is no currently operational facility observing between 150 and 912 Å. Inferring the spectra of exoplanet hosts in this regime is critical to studying the evolution of planetary atmospheres because the EUV heats the top of the thermosphere and drives atmospheric escape. This paper presents our implementation of the differential emission measure technique to reconstruct the EUV spectra of cool dwarfs. We characterize our method's accuracy and precision by applying it to the Sun and AU Mic. We then apply it to three fainter M dwarfs: GJ 832, Barnard's star, and TRAPPIST-1. We demonstrate that with the strongest far-ultraviolet (FUV, 912-1700 Å) emission lines, observed with the Hubble Space Telescope and/or Far Ultraviolet Spectroscopic Explorer, and a coarse X-ray spectrum from either the Chandra X-ray Observatory or XMM-Newton, we can reconstruct the Sun's EUV spectrum to within a factor of 1.8, with our model's formal uncertainties encompassing the data. We report the integrated EUV flux of our M dwarf sample with uncertainties of a factor of 2-7 depending on available data quality.
Fil: Duvvuri, Girish M.. State University of Colorado at Boulder; Estados Unidos
Fil: Pineda, J. Sebastian. State University of Colorado at Boulder; Estados Unidos
Fil: Berta Thompson, Zachory. State University of Colorado at Boulder; Estados Unidos
Fil: Brown, Alexander. State University of Colorado at Boulder; Estados Unidos
Fil: France, K.. State University of Colorado at Boulder; Estados Unidos
Fil: Kowalski, A.. State University of Colorado at Boulder; Estados Unidos
Fil: Redfield, S.. State University of Colorado at Boulder; Estados Unidos
Fil: Tilipman, Dennis. State University of Colorado at Boulder; Estados Unidos
Fil: Vieytes, Mariela Cristina. Consejo Nacional de Investigaciones 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: Wilson, David J.. State University of Colorado at Boulder; Estados Unidos
Fil: Youngblood, Allison. State University of Colorado at Boulder; Estados Unidos
Fil: Froning, C.. State University of Colorado at Boulder; Estados Unidos
Fil: Linsky, J. L.. State University of Colorado at Boulder; Estados Unidos
Fil: Parke Loyd, R. O.. State University of Colorado at Boulder; Estados Unidos
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones 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: Miguel, Yamila. State University of Colorado at Boulder; Estados Unidos
Fil: Newton, Elisabeth R.. State University of Colorado at Boulder; Estados Unidos
Fil: Rugheimer, Sarah. State University of Colorado at Boulder; Estados Unidos
Fil: Christian Schneider, P.. State University of Colorado at Boulder; Estados Unidos
description Characterizing the atmospheres of planets orbiting M dwarfs requires understanding the spectral energy distributions of M dwarfs over planetary lifetimes. Surveys like MUSCLES, HAZMAT, and FUMES have collected multiwavelength spectra across the spectral type's range of T eff and activity, but the extreme ultraviolet (EUV, 100-912 Å) flux of most of these stars remains unobserved because of obscuration by the interstellar medium compounded with limited detector sensitivity. While targets with observable EUV flux exist, there is no currently operational facility observing between 150 and 912 Å. Inferring the spectra of exoplanet hosts in this regime is critical to studying the evolution of planetary atmospheres because the EUV heats the top of the thermosphere and drives atmospheric escape. This paper presents our implementation of the differential emission measure technique to reconstruct the EUV spectra of cool dwarfs. We characterize our method's accuracy and precision by applying it to the Sun and AU Mic. We then apply it to three fainter M dwarfs: GJ 832, Barnard's star, and TRAPPIST-1. We demonstrate that with the strongest far-ultraviolet (FUV, 912-1700 Å) emission lines, observed with the Hubble Space Telescope and/or Far Ultraviolet Spectroscopic Explorer, and a coarse X-ray spectrum from either the Chandra X-ray Observatory or XMM-Newton, we can reconstruct the Sun's EUV spectrum to within a factor of 1.8, with our model's formal uncertainties encompassing the data. We report the integrated EUV flux of our M dwarf sample with uncertainties of a factor of 2-7 depending on available data quality.
publishDate 2021
dc.date.none.fl_str_mv 2021-05
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/11336/182676
Duvvuri, Girish M.; Pineda, J. Sebastian; Berta Thompson, Zachory; Brown, Alexander; France, K.; et al.; Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials; IOP Publishing; Astrophysical Journal; 913; 1; 5-2021; 1-37
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/182676
identifier_str_mv Duvvuri, Girish M.; Pineda, J. Sebastian; Berta Thompson, Zachory; Brown, Alexander; France, K.; et al.; Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials; IOP Publishing; Astrophysical Journal; 913; 1; 5-2021; 1-37
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abeaaf
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abeaaf
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
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 12.976206

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