Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae

Autores
Pessi, Priscila Jael; Folatelli, Gaston; Anderson, J. P.; Bersten, Melina Cecilia; Burns, C.; Contreras, C.; Davis, S.; Englert Urrutia, Brenda Nahir; Hamuy, M.; Hsiao, Eric; Martinez, Laureano; Morrell, Nidia Irene; Phillips, M. M.; Suntzeff, N.; Stritzinger, M. D.
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Type II supernovae (SNe II) show strong hydrogen features in their spectra throughout their whole evolution, while type IIb supernovae (SNe IIb) spectra evolve from dominant hydrogen lines at early times to increasingly strong helium features later on. However, it is currently unclear whether the progenitors of these SN types form a continuum in pre-SN hydrogen mass or whether they are physically distinct. SN light-curve morphology directly relates to progenitor and explosion properties such as the amount of hydrogen in the envelope, the pre-SN radius, the explosion energy, and the synthesized mass of radioactive material. In this work, we study the morphology of the optical-wavelength light curves of hydrogen-rich SNe II and hydrogen-poor SNe IIb to test whether an observational continuum exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe IIb), we define a range of key observational parameters and present a comparative analysis between both types. We find a lack of events that bridge the observed properties of SNe II and IIb. Light-curve parameters such as rise times and post-maximum decline rates and curvatures clearly separate both SN types and we therefore conclude that there is no continuum, with the two SN types forming two observationally distinct families. In the V band a rise time of 17 d (SNe II lower and SNe IIb higher), and a magnitude difference between 30 and 40 d post-explosion of 0.4 mag (SNe II lower and SNe IIb higher) serve as approximate thresholds to differentiate both types.
Fil: Pessi, Priscila Jael. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Anderson, J. P.. European Southern Observatory Chile.; Chile
Fil: Bersten, Melina Cecilia. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados Unidos
Fil: Contreras, C.. Las Campanas Observatory; Chile. Space Telescope Science Institute; Estados Unidos
Fil: Davis, S.. Florida State University; Estados Unidos
Fil: Englert Urrutia, Brenda Nahir. Ministerio de Ciencia. Tecnología e Innovación Productiva. Agencia Nacional de Promoción Científica y Tecnológica; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Hamuy, M.. Universidad de Chile; Chile
Fil: Hsiao, Eric. Florida State University; Estados Unidos
Fil: Martinez, Laureano. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Morrell, Nidia Irene. Las Campanas Observatory; Chile. 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: Phillips, M. M.. Las Campanas Observatory; Chile
Fil: Suntzeff, N.. Texas A&M University; Estados Unidos
Fil: Stritzinger, M. D.. University Aarhus; Dinamarca
Materia
SN 2004FF
SN 2006Y
SN 2007FZ
SN 2008M
SN 2013AI
SN 2013FS)
SUPERNOVAE: GENERAL – SUPERNOVAE: INDIVIDUAL (SN 2001FA
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:11336/130077
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovaePessi, Priscila JaelFolatelli, GastonAnderson, J. P.Bersten, Melina CeciliaBurns, C.Contreras, C.Davis, S.Englert Urrutia, Brenda NahirHamuy, M.Hsiao, EricMartinez, LaureanoMorrell, Nidia IrenePhillips, M. M.Suntzeff, N.Stritzinger, M. D.SN 2004FFSN 2006YSN 2007FZSN 2008MSN 2013AISN 2013FS)SUPERNOVAE: GENERAL – SUPERNOVAE: INDIVIDUAL (SN 2001FAhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Type II supernovae (SNe II) show strong hydrogen features in their spectra throughout their whole evolution, while type IIb supernovae (SNe IIb) spectra evolve from dominant hydrogen lines at early times to increasingly strong helium features later on. However, it is currently unclear whether the progenitors of these SN types form a continuum in pre-SN hydrogen mass or whether they are physically distinct. SN light-curve morphology directly relates to progenitor and explosion properties such as the amount of hydrogen in the envelope, the pre-SN radius, the explosion energy, and the synthesized mass of radioactive material. In this work, we study the morphology of the optical-wavelength light curves of hydrogen-rich SNe II and hydrogen-poor SNe IIb to test whether an observational continuum exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe IIb), we define a range of key observational parameters and present a comparative analysis between both types. We find a lack of events that bridge the observed properties of SNe II and IIb. Light-curve parameters such as rise times and post-maximum decline rates and curvatures clearly separate both SN types and we therefore conclude that there is no continuum, with the two SN types forming two observationally distinct families. In the V band a rise time of 17 d (SNe II lower and SNe IIb higher), and a magnitude difference between 30 and 40 d post-explosion of 0.4 mag (SNe II lower and SNe IIb higher) serve as approximate thresholds to differentiate both types.Fil: Pessi, Priscila Jael. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Anderson, J. P.. European Southern Observatory Chile.; ChileFil: Bersten, Melina Cecilia. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados UnidosFil: Contreras, C.. Las Campanas Observatory; Chile. Space Telescope Science Institute; Estados UnidosFil: Davis, S.. Florida State University; Estados UnidosFil: Englert Urrutia, Brenda Nahir. Ministerio de Ciencia. Tecnología e Innovación Productiva. Agencia Nacional de Promoción Científica y Tecnológica; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Hamuy, M.. Universidad de Chile; ChileFil: Hsiao, Eric. Florida State University; Estados UnidosFil: Martinez, Laureano. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Morrell, Nidia Irene. Las Campanas Observatory; Chile. 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: Phillips, M. M.. Las Campanas Observatory; ChileFil: Suntzeff, N.. Texas A&M University; Estados UnidosFil: Stritzinger, M. D.. University Aarhus; DinamarcaWiley Blackwell Publishing, Inc2019-07-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/130077Pessi, Priscila Jael; Folatelli, Gaston; Anderson, J. P.; Bersten, Melina Cecilia; Burns, C.; et al.; Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 488; 3; 11-7-2019; 4239-42570035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/488/3/4239/5531326info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz1855info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1907.04653info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:34:16Zoai:ri.conicet.gov.ar:11336/130077instacron: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 10:34:16.826CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
title Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
spellingShingle Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
Pessi, Priscila Jael
SN 2004FF
SN 2006Y
SN 2007FZ
SN 2008M
SN 2013AI
SN 2013FS)
SUPERNOVAE: GENERAL – SUPERNOVAE: INDIVIDUAL (SN 2001FA
title_short Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
title_full Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
title_fullStr Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
title_full_unstemmed Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
title_sort Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae
dc.creator.none.fl_str_mv Pessi, Priscila Jael
Folatelli, Gaston
Anderson, J. P.
Bersten, Melina Cecilia
Burns, C.
Contreras, C.
Davis, S.
Englert Urrutia, Brenda Nahir
Hamuy, M.
Hsiao, Eric
Martinez, Laureano
Morrell, Nidia Irene
Phillips, M. M.
Suntzeff, N.
Stritzinger, M. D.
author Pessi, Priscila Jael
author_facet Pessi, Priscila Jael
Folatelli, Gaston
Anderson, J. P.
Bersten, Melina Cecilia
Burns, C.
Contreras, C.
Davis, S.
Englert Urrutia, Brenda Nahir
Hamuy, M.
Hsiao, Eric
Martinez, Laureano
Morrell, Nidia Irene
Phillips, M. M.
Suntzeff, N.
Stritzinger, M. D.
author_role author
author2 Folatelli, Gaston
Anderson, J. P.
Bersten, Melina Cecilia
Burns, C.
Contreras, C.
Davis, S.
Englert Urrutia, Brenda Nahir
Hamuy, M.
Hsiao, Eric
Martinez, Laureano
Morrell, Nidia Irene
Phillips, M. M.
Suntzeff, N.
Stritzinger, M. D.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv SN 2004FF
SN 2006Y
SN 2007FZ
SN 2008M
SN 2013AI
SN 2013FS)
SUPERNOVAE: GENERAL – SUPERNOVAE: INDIVIDUAL (SN 2001FA
topic SN 2004FF
SN 2006Y
SN 2007FZ
SN 2008M
SN 2013AI
SN 2013FS)
SUPERNOVAE: GENERAL – SUPERNOVAE: INDIVIDUAL (SN 2001FA
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Type II supernovae (SNe II) show strong hydrogen features in their spectra throughout their whole evolution, while type IIb supernovae (SNe IIb) spectra evolve from dominant hydrogen lines at early times to increasingly strong helium features later on. However, it is currently unclear whether the progenitors of these SN types form a continuum in pre-SN hydrogen mass or whether they are physically distinct. SN light-curve morphology directly relates to progenitor and explosion properties such as the amount of hydrogen in the envelope, the pre-SN radius, the explosion energy, and the synthesized mass of radioactive material. In this work, we study the morphology of the optical-wavelength light curves of hydrogen-rich SNe II and hydrogen-poor SNe IIb to test whether an observational continuum exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe IIb), we define a range of key observational parameters and present a comparative analysis between both types. We find a lack of events that bridge the observed properties of SNe II and IIb. Light-curve parameters such as rise times and post-maximum decline rates and curvatures clearly separate both SN types and we therefore conclude that there is no continuum, with the two SN types forming two observationally distinct families. In the V band a rise time of 17 d (SNe II lower and SNe IIb higher), and a magnitude difference between 30 and 40 d post-explosion of 0.4 mag (SNe II lower and SNe IIb higher) serve as approximate thresholds to differentiate both types.
Fil: Pessi, Priscila Jael. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Anderson, J. P.. European Southern Observatory Chile.; Chile
Fil: Bersten, Melina Cecilia. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Burns, C.. Observatories Of The Carnegie Institution For Science; Estados Unidos
Fil: Contreras, C.. Las Campanas Observatory; Chile. Space Telescope Science Institute; Estados Unidos
Fil: Davis, S.. Florida State University; Estados Unidos
Fil: Englert Urrutia, Brenda Nahir. Ministerio de Ciencia. Tecnología e Innovación Productiva. Agencia Nacional de Promoción Científica y Tecnológica; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Hamuy, M.. Universidad de Chile; Chile
Fil: Hsiao, Eric. Florida State University; Estados Unidos
Fil: Martinez, Laureano. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Morrell, Nidia Irene. Las Campanas Observatory; Chile. 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: Phillips, M. M.. Las Campanas Observatory; Chile
Fil: Suntzeff, N.. Texas A&M University; Estados Unidos
Fil: Stritzinger, M. D.. University Aarhus; Dinamarca
description Type II supernovae (SNe II) show strong hydrogen features in their spectra throughout their whole evolution, while type IIb supernovae (SNe IIb) spectra evolve from dominant hydrogen lines at early times to increasingly strong helium features later on. However, it is currently unclear whether the progenitors of these SN types form a continuum in pre-SN hydrogen mass or whether they are physically distinct. SN light-curve morphology directly relates to progenitor and explosion properties such as the amount of hydrogen in the envelope, the pre-SN radius, the explosion energy, and the synthesized mass of radioactive material. In this work, we study the morphology of the optical-wavelength light curves of hydrogen-rich SNe II and hydrogen-poor SNe IIb to test whether an observational continuum exists between the two. Using a sample of 95 SNe (73 SNe II and 22 SNe IIb), we define a range of key observational parameters and present a comparative analysis between both types. We find a lack of events that bridge the observed properties of SNe II and IIb. Light-curve parameters such as rise times and post-maximum decline rates and curvatures clearly separate both SN types and we therefore conclude that there is no continuum, with the two SN types forming two observationally distinct families. In the V band a rise time of 17 d (SNe II lower and SNe IIb higher), and a magnitude difference between 30 and 40 d post-explosion of 0.4 mag (SNe II lower and SNe IIb higher) serve as approximate thresholds to differentiate both types.
publishDate 2019
dc.date.none.fl_str_mv 2019-07-11
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/11336/130077
Pessi, Priscila Jael; Folatelli, Gaston; Anderson, J. P.; Bersten, Melina Cecilia; Burns, C.; et al.; Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 488; 3; 11-7-2019; 4239-4257
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/130077
identifier_str_mv Pessi, Priscila Jael; Folatelli, Gaston; Anderson, J. P.; Bersten, Melina Cecilia; Burns, C.; et al.; Comparison of the optical light curves of hydrogen-rich and hydrogen-poor type II supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 488; 3; 11-7-2019; 4239-4257
0035-8711
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://academic.oup.com/mnras/article/488/3/4239/5531326
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz1855
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1907.04653
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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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