Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution

Autores
Gutiérrez, Claudia P.; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia Irene; González Gaitan, Santiago; Stritzinger, Maximilian D.; Phillips, Mark M.; Galbany, Lluis; Folatelli, Gastón; Dessart, Luc; Contreras, Carlos; Della Valle, Massimo; Freedman, Wendy L.; Hsiao, Eric Y.; Krisciunas, Kevin; Madore, Barry F.; Maza, José; Suntzeff, Nicholas B.; Prieto, José Luis; González, Luis; Cappellaro, Enrico; Navarrete, Mauricio; Pizzella, Alessandro; Ruiz, María T.; Smith, R. Chris; Turatto, Massimo
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present 888 visual-wavelength spectra of 122 nearby type II supernovae (SNe II) obtained between 1986 and 2009, and ranging between 3 and 363 days post-explosion. In this first paper, we outline our observations and data reduction techniques, together with a characterization based on the spectral diversity of SNe II. A statistical analysis of the spectral matching technique is discussed as an alternative to nondetection constraints for estimating SN explosion epochs. The time evolution of spectral lines is presented and analyzed in terms of how this differs for SNe of different photometric, spectral, and environmental properties: velocities, pseudo-equivalent widths, decline rates, magnitudes, time durations, and environment metallicity. Our sample displays a large range in ejecta expansion velocities, from ∼9600 to ∼1500 km s-1 at 50 days post-explosion with a median Hα value of 7300 km s-1. This is most likely explained through differing explosion energies. Significant diversity is also observed in the absolute strength of spectral lines, characterized through their pseudo-equivalent widths. This implies significant diversity in both temperature evolution (linked to progenitor radius) and progenitor metallicity between different SNe II. Around 60% of our sample shows an extra absorption component on the blue side of the Hα P-Cygni profile ("Cachito" feature) between 7 and 120 days since explosion. Studying the nature of Cachito, we conclude that these features at early times (before ∼35 days) are associated with Si ii λ6355, while past the middle of the plateau phase they are related to high velocity (HV) features of hydrogen lines.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
supernovae: general
surveys
techniques: photometric
techniques: spectroscopic
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/87198

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/87198
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line EvolutionGutiérrez, Claudia P.Anderson, Joseph P.Hamuy, MarioMorrell, Nidia IreneGonzález Gaitan, SantiagoStritzinger, Maximilian D.Phillips, Mark M.Galbany, LluisFolatelli, GastónDessart, LucContreras, CarlosDella Valle, MassimoFreedman, Wendy L.Hsiao, Eric Y.Krisciunas, KevinMadore, Barry F.Maza, JoséSuntzeff, Nicholas B.Prieto, José LuisGonzález, LuisCappellaro, EnricoNavarrete, MauricioPizzella, AlessandroRuiz, María T.Smith, R. ChrisTuratto, MassimoCiencias Astronómicassupernovae: generalsurveystechniques: photometrictechniques: spectroscopicWe present 888 visual-wavelength spectra of 122 nearby type II supernovae (SNe II) obtained between 1986 and 2009, and ranging between 3 and 363 days post-explosion. In this first paper, we outline our observations and data reduction techniques, together with a characterization based on the spectral diversity of SNe II. A statistical analysis of the spectral matching technique is discussed as an alternative to nondetection constraints for estimating SN explosion epochs. The time evolution of spectral lines is presented and analyzed in terms of how this differs for SNe of different photometric, spectral, and environmental properties: velocities, pseudo-equivalent widths, decline rates, magnitudes, time durations, and environment metallicity. Our sample displays a large range in ejecta expansion velocities, from ∼9600 to ∼1500 km s<sup>-1</sup> at 50 days post-explosion with a median H<sub>α</sub> value of 7300 km s<sup>-1</sup>. This is most likely explained through differing explosion energies. Significant diversity is also observed in the absolute strength of spectral lines, characterized through their pseudo-equivalent widths. This implies significant diversity in both temperature evolution (linked to progenitor radius) and progenitor metallicity between different SNe II. Around 60% of our sample shows an extra absorption component on the blue side of the H<sub>α</sub> P-Cygni profile ("Cachito" feature) between 7 and 120 days since explosion. Studying the nature of Cachito, we conclude that these features at early times (before ∼35 days) are associated with Si ii λ6355, while past the middle of the plateau phase they are related to high velocity (HV) features of hydrogen lines.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2017info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/87198enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa8f52info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:17:09Zoai:sedici.unlp.edu.ar:10915/87198Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:17:10.242SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
title Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
spellingShingle Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
Gutiérrez, Claudia P.
Ciencias Astronómicas
supernovae: general
surveys
techniques: photometric
techniques: spectroscopic
title_short Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
title_full Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
title_fullStr Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
title_full_unstemmed Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
title_sort Type II Supernova Spectral Diversity. I. Observations, Sample Characterization, and Spectral Line Evolution
dc.creator.none.fl_str_mv Gutiérrez, Claudia P.
Anderson, Joseph P.
Hamuy, Mario
Morrell, Nidia Irene
González Gaitan, Santiago
Stritzinger, Maximilian D.
Phillips, Mark M.
Galbany, Lluis
Folatelli, Gastón
Dessart, Luc
Contreras, Carlos
Della Valle, Massimo
Freedman, Wendy L.
Hsiao, Eric Y.
Krisciunas, Kevin
Madore, Barry F.
Maza, José
Suntzeff, Nicholas B.
Prieto, José Luis
González, Luis
Cappellaro, Enrico
Navarrete, Mauricio
Pizzella, Alessandro
Ruiz, María T.
Smith, R. Chris
Turatto, Massimo
author Gutiérrez, Claudia P.
author_facet Gutiérrez, Claudia P.
Anderson, Joseph P.
Hamuy, Mario
Morrell, Nidia Irene
González Gaitan, Santiago
Stritzinger, Maximilian D.
Phillips, Mark M.
Galbany, Lluis
Folatelli, Gastón
Dessart, Luc
Contreras, Carlos
Della Valle, Massimo
Freedman, Wendy L.
Hsiao, Eric Y.
Krisciunas, Kevin
Madore, Barry F.
Maza, José
Suntzeff, Nicholas B.
Prieto, José Luis
González, Luis
Cappellaro, Enrico
Navarrete, Mauricio
Pizzella, Alessandro
Ruiz, María T.
Smith, R. Chris
Turatto, Massimo
author_role author
author2 Anderson, Joseph P.
Hamuy, Mario
Morrell, Nidia Irene
González Gaitan, Santiago
Stritzinger, Maximilian D.
Phillips, Mark M.
Galbany, Lluis
Folatelli, Gastón
Dessart, Luc
Contreras, Carlos
Della Valle, Massimo
Freedman, Wendy L.
Hsiao, Eric Y.
Krisciunas, Kevin
Madore, Barry F.
Maza, José
Suntzeff, Nicholas B.
Prieto, José Luis
González, Luis
Cappellaro, Enrico
Navarrete, Mauricio
Pizzella, Alessandro
Ruiz, María T.
Smith, R. Chris
Turatto, Massimo
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
dc.subject.none.fl_str_mv Ciencias Astronómicas
supernovae: general
surveys
techniques: photometric
techniques: spectroscopic
topic Ciencias Astronómicas
supernovae: general
surveys
techniques: photometric
techniques: spectroscopic
dc.description.none.fl_txt_mv We present 888 visual-wavelength spectra of 122 nearby type II supernovae (SNe II) obtained between 1986 and 2009, and ranging between 3 and 363 days post-explosion. In this first paper, we outline our observations and data reduction techniques, together with a characterization based on the spectral diversity of SNe II. A statistical analysis of the spectral matching technique is discussed as an alternative to nondetection constraints for estimating SN explosion epochs. The time evolution of spectral lines is presented and analyzed in terms of how this differs for SNe of different photometric, spectral, and environmental properties: velocities, pseudo-equivalent widths, decline rates, magnitudes, time durations, and environment metallicity. Our sample displays a large range in ejecta expansion velocities, from ∼9600 to ∼1500 km s<sup>-1</sup> at 50 days post-explosion with a median H<sub>α</sub> value of 7300 km s<sup>-1</sup>. This is most likely explained through differing explosion energies. Significant diversity is also observed in the absolute strength of spectral lines, characterized through their pseudo-equivalent widths. This implies significant diversity in both temperature evolution (linked to progenitor radius) and progenitor metallicity between different SNe II. Around 60% of our sample shows an extra absorption component on the blue side of the H<sub>α</sub> P-Cygni profile ("Cachito" feature) between 7 and 120 days since explosion. Studying the nature of Cachito, we conclude that these features at early times (before ∼35 days) are associated with Si ii λ6355, while past the middle of the plateau phase they are related to high velocity (HV) features of hydrogen lines.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description We present 888 visual-wavelength spectra of 122 nearby type II supernovae (SNe II) obtained between 1986 and 2009, and ranging between 3 and 363 days post-explosion. In this first paper, we outline our observations and data reduction techniques, together with a characterization based on the spectral diversity of SNe II. A statistical analysis of the spectral matching technique is discussed as an alternative to nondetection constraints for estimating SN explosion epochs. The time evolution of spectral lines is presented and analyzed in terms of how this differs for SNe of different photometric, spectral, and environmental properties: velocities, pseudo-equivalent widths, decline rates, magnitudes, time durations, and environment metallicity. Our sample displays a large range in ejecta expansion velocities, from ∼9600 to ∼1500 km s<sup>-1</sup> at 50 days post-explosion with a median H<sub>α</sub> value of 7300 km s<sup>-1</sup>. This is most likely explained through differing explosion energies. Significant diversity is also observed in the absolute strength of spectral lines, characterized through their pseudo-equivalent widths. This implies significant diversity in both temperature evolution (linked to progenitor radius) and progenitor metallicity between different SNe II. Around 60% of our sample shows an extra absorption component on the blue side of the H<sub>α</sub> P-Cygni profile ("Cachito" feature) between 7 and 120 days since explosion. Studying the nature of Cachito, we conclude that these features at early times (before ∼35 days) are associated with Si ii λ6355, while past the middle of the plateau phase they are related to high velocity (HV) features of hydrogen lines.
publishDate 2017
dc.date.none.fl_str_mv 2017
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/87198
url http://sedici.unlp.edu.ar/handle/10915/87198
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa8f52
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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