Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy

Autores
Ferrari, Lucía; Folatelli, Gaston; Ertini, Keila Yael; Kuncarayakti, Hanindyo; Andrews, Jennifer E.
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Supernova (SN) 2023ixf was discovered in the galaxy M 101 in May 2023. Its proximity provided the scientific community an extremely valuable opportunity to study the characteristics of the SN and its progenitor. A point source detected on archival images and hydrodynamical modeling of the bolometric light curve have been used to constrain the former star’s properties. There is a significant variation in the published results regarding the initial mass of the progenitor. Nebular spectroscopy can be used to enhance our understanding of the SN and its progenitor. Aims. We determined the SN progenitor mass by studying the first published nebular spectrum, taken 259 days after the explosion. Methods. We analyzed the nebular spectrum taken with GMOS at the Gemini North Telescope. We identified typical emission lines, such as [O I], Hα, and [Ca II], among others. Some species’ line profiles show broad and narrow components, indicating two ejecta velocities and an asymmetric ejecta. We inferred the progenitor mass of SN 2023ixf by comparing its spectra with synthetic spectra and by measuring the forbidden oxygen doublet flux. Results. Based on the flux ratio and the direct comparison with spectra models, the progenitor star of SN 2023ixf had a MZAMS between 12 and 15 M⊙. We find that using the [O I] doublet flux provides a less tight constraint on the progenitor mass. Our results agree with those from hydrodynamical modeling of the early light curve and pre-explosion image estimates that point to a relatively low-mass progenitor.
Fil: Ferrari, Lucía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Ertini, Keila Yael. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Kuncarayakti, Hanindyo. University Of Turku; Finlandia
Fil: Andrews, Jennifer E.. Gemini Observatory; Estados Unidos
Materia
SUPERNOVAE:GENERAL
SUPERNOVAE:INDIVIDUAL:SN2023IXF
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/256779
Acceder
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spelling Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopyFerrari, LucíaFolatelli, GastonErtini, Keila YaelKuncarayakti, HanindyoAndrews, Jennifer E.SUPERNOVAE:GENERALSUPERNOVAE:INDIVIDUAL:SN2023IXFhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Supernova (SN) 2023ixf was discovered in the galaxy M 101 in May 2023. Its proximity provided the scientific community an extremely valuable opportunity to study the characteristics of the SN and its progenitor. A point source detected on archival images and hydrodynamical modeling of the bolometric light curve have been used to constrain the former star’s properties. There is a significant variation in the published results regarding the initial mass of the progenitor. Nebular spectroscopy can be used to enhance our understanding of the SN and its progenitor. Aims. We determined the SN progenitor mass by studying the first published nebular spectrum, taken 259 days after the explosion. Methods. We analyzed the nebular spectrum taken with GMOS at the Gemini North Telescope. We identified typical emission lines, such as [O I], Hα, and [Ca II], among others. Some species’ line profiles show broad and narrow components, indicating two ejecta velocities and an asymmetric ejecta. We inferred the progenitor mass of SN 2023ixf by comparing its spectra with synthetic spectra and by measuring the forbidden oxygen doublet flux. Results. Based on the flux ratio and the direct comparison with spectra models, the progenitor star of SN 2023ixf had a MZAMS between 12 and 15 M⊙. We find that using the [O I] doublet flux provides a less tight constraint on the progenitor mass. Our results agree with those from hydrodynamical modeling of the early light curve and pre-explosion image estimates that point to a relatively low-mass progenitor.Fil: Ferrari, Lucía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Ertini, Keila Yael. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Kuncarayakti, Hanindyo. University Of Turku; FinlandiaFil: Andrews, Jennifer E.. Gemini Observatory; Estados UnidosEDP Sciences2024-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/256779Ferrari, Lucía; Folatelli, Gaston; Ertini, Keila Yael; Kuncarayakti, Hanindyo; Andrews, Jennifer E.; Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy; EDP Sciences; Astronomy and Astrophysics; 687; L20; 7-2024; 1-60004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202450440info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450440info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:44:08Zoai:ri.conicet.gov.ar:11336/256779instacron: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:34982025-09-29 10:44:08.899CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
title Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
spellingShingle Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
Ferrari, Lucía
SUPERNOVAE:GENERAL
SUPERNOVAE:INDIVIDUAL:SN2023IXF
title_short Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
title_full Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
title_fullStr Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
title_full_unstemmed Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
title_sort Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy
dc.creator.none.fl_str_mv Ferrari, Lucía
Folatelli, Gaston
Ertini, Keila Yael
Kuncarayakti, Hanindyo
Andrews, Jennifer E.
author Ferrari, Lucía
author_facet Ferrari, Lucía
Folatelli, Gaston
Ertini, Keila Yael
Kuncarayakti, Hanindyo
Andrews, Jennifer E.
author_role author
author2 Folatelli, Gaston
Ertini, Keila Yael
Kuncarayakti, Hanindyo
Andrews, Jennifer E.
author2_role author
author
author
author
dc.subject.none.fl_str_mv SUPERNOVAE:GENERAL
SUPERNOVAE:INDIVIDUAL:SN2023IXF
topic SUPERNOVAE:GENERAL
SUPERNOVAE:INDIVIDUAL:SN2023IXF
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. Supernova (SN) 2023ixf was discovered in the galaxy M 101 in May 2023. Its proximity provided the scientific community an extremely valuable opportunity to study the characteristics of the SN and its progenitor. A point source detected on archival images and hydrodynamical modeling of the bolometric light curve have been used to constrain the former star’s properties. There is a significant variation in the published results regarding the initial mass of the progenitor. Nebular spectroscopy can be used to enhance our understanding of the SN and its progenitor. Aims. We determined the SN progenitor mass by studying the first published nebular spectrum, taken 259 days after the explosion. Methods. We analyzed the nebular spectrum taken with GMOS at the Gemini North Telescope. We identified typical emission lines, such as [O I], Hα, and [Ca II], among others. Some species’ line profiles show broad and narrow components, indicating two ejecta velocities and an asymmetric ejecta. We inferred the progenitor mass of SN 2023ixf by comparing its spectra with synthetic spectra and by measuring the forbidden oxygen doublet flux. Results. Based on the flux ratio and the direct comparison with spectra models, the progenitor star of SN 2023ixf had a MZAMS between 12 and 15 M⊙. We find that using the [O I] doublet flux provides a less tight constraint on the progenitor mass. Our results agree with those from hydrodynamical modeling of the early light curve and pre-explosion image estimates that point to a relatively low-mass progenitor.
Fil: Ferrari, Lucía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Ertini, Keila Yael. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Kuncarayakti, Hanindyo. University Of Turku; Finlandia
Fil: Andrews, Jennifer E.. Gemini Observatory; Estados Unidos
description Context. Supernova (SN) 2023ixf was discovered in the galaxy M 101 in May 2023. Its proximity provided the scientific community an extremely valuable opportunity to study the characteristics of the SN and its progenitor. A point source detected on archival images and hydrodynamical modeling of the bolometric light curve have been used to constrain the former star’s properties. There is a significant variation in the published results regarding the initial mass of the progenitor. Nebular spectroscopy can be used to enhance our understanding of the SN and its progenitor. Aims. We determined the SN progenitor mass by studying the first published nebular spectrum, taken 259 days after the explosion. Methods. We analyzed the nebular spectrum taken with GMOS at the Gemini North Telescope. We identified typical emission lines, such as [O I], Hα, and [Ca II], among others. Some species’ line profiles show broad and narrow components, indicating two ejecta velocities and an asymmetric ejecta. We inferred the progenitor mass of SN 2023ixf by comparing its spectra with synthetic spectra and by measuring the forbidden oxygen doublet flux. Results. Based on the flux ratio and the direct comparison with spectra models, the progenitor star of SN 2023ixf had a MZAMS between 12 and 15 M⊙. We find that using the [O I] doublet flux provides a less tight constraint on the progenitor mass. Our results agree with those from hydrodynamical modeling of the early light curve and pre-explosion image estimates that point to a relatively low-mass progenitor.
publishDate 2024
dc.date.none.fl_str_mv 2024-07
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/11336/256779
Ferrari, Lucía; Folatelli, Gaston; Ertini, Keila Yael; Kuncarayakti, Hanindyo; Andrews, Jennifer E.; Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy; EDP Sciences; Astronomy and Astrophysics; 687; L20; 7-2024; 1-6
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/256779
identifier_str_mv Ferrari, Lucía; Folatelli, Gaston; Ertini, Keila Yael; Kuncarayakti, Hanindyo; Andrews, Jennifer E.; Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy; EDP Sciences; Astronomy and Astrophysics; 687; L20; 7-2024; 1-6
0004-6361
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://www.aanda.org/10.1051/0004-6361/202450440
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450440
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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