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, Gaston; Dessart, Luc; Contreras, Carlos; Valle, Massimo Della; Freedman, Wendy L.; Hsiao, Eric Y.; Krisciunas, Kevin; Madore, Barry F.; Maza, José; Suntzeff, Nicholas B.; Prieto, Jose Luis; González, Luis; Cappellaro, Enrico; Navarrete, Mauricio; Pizzella, Alessandro; Ruiz, Maria 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.
Fil: Gutiérrez, Claudia P.. Universidad de Chile; Chile. University of Southampton; Reino Unido
Fil: Anderson, Joseph P.. European Southern Observatory Santiago; Chile
Fil: Hamuy, Mario. Universidad de Chile; Chile. Millennium Institute Of Astrophysics; Chile
Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile
Fil: González Gaitan, Santiago. Millennium Institute Of Astrophysics; Chile. Universidad de Chile; Chile
Fil: Stritzinger, Maximilian D.. University Aarhus; Dinamarca
Fil: Phillips, Mark M.. Las Campanas Observatory; Chile
Fil: Galbany, Lluis. University of Pittsburgh at Johnstown; Estados Unidos. University of Pittsburgh; Estados Unidos
Fil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Dessart, Luc. Universidad de Chile; Chile
Fil: Contreras, Carlos. Las Campanas Observatory; Chile
Fil: Valle, Massimo Della. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Freedman, Wendy L.. University of Chicago; Estados Unidos
Fil: Hsiao, Eric Y.. Florida State University; Estados Unidos
Fil: Krisciunas, Kevin. Texas A&M University; Estados Unidos
Fil: Madore, Barry F.. Observatories of the Carnegie Institution for Science; Estados Unidos
Fil: Maza, José. Universidad de Chile; Chile
Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos
Fil: Prieto, Jose Luis. Millennium Institute Of Astrophysics; Chile. Universidad Diego Portales; Chile
Fil: González, Luis. Universidad de Chile; Chile
Fil: Cappellaro, Enrico. Osservatorio Astronomico Di Padova; Chile
Fil: Navarrete, Mauricio. Las Campanas Observatory; Chile
Fil: Pizzella, Alessandro. Università di Padova; Italia
Fil: Ruiz, Maria T.. Universidad de Chile; Chile
Fil: Smith, R. Chris. Cerro Tololo Inter American Observatory; Chile
Fil: Turatto, Massimo. Osservatorio Astronomico Di Padova; Italia - Materia
-
Supernovae
Surveys
Photometric techniques
Spectroscophy - 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:11336/41312
Ver los metadatos del registro completo
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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, GastonDessart, LucContreras, CarlosValle, Massimo DellaFreedman, Wendy L.Hsiao, Eric Y.Krisciunas, KevinMadore, Barry F.Maza, JoséSuntzeff, Nicholas B.Prieto, Jose LuisGonzález, LuisCappellaro, EnricoNavarrete, MauricioPizzella, AlessandroRuiz, Maria T.Smith, R. ChrisTuratto, MassimoSupernovaeSurveysPhotometric techniquesSpectroscophyhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We 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.Fil: Gutiérrez, Claudia P.. Universidad de Chile; Chile. University of Southampton; Reino UnidoFil: Anderson, Joseph P.. European Southern Observatory Santiago; ChileFil: Hamuy, Mario. Universidad de Chile; Chile. Millennium Institute Of Astrophysics; ChileFil: Morrell, Nidia Irene. Las Campanas Observatory; ChileFil: González Gaitan, Santiago. Millennium Institute Of Astrophysics; Chile. Universidad de Chile; ChileFil: Stritzinger, Maximilian D.. University Aarhus; DinamarcaFil: Phillips, Mark M.. Las Campanas Observatory; ChileFil: Galbany, Lluis. University of Pittsburgh at Johnstown; Estados Unidos. University of Pittsburgh; Estados UnidosFil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Dessart, Luc. Universidad de Chile; ChileFil: Contreras, Carlos. Las Campanas Observatory; ChileFil: Valle, Massimo Della. Osservatorio Astronomico Di Capodimonte; ItaliaFil: Freedman, Wendy L.. University of Chicago; Estados UnidosFil: Hsiao, Eric Y.. Florida State University; Estados UnidosFil: Krisciunas, Kevin. Texas A&M University; Estados UnidosFil: Madore, Barry F.. Observatories of the Carnegie Institution for Science; Estados UnidosFil: Maza, José. Universidad de Chile; ChileFil: Suntzeff, Nicholas B.. Texas A&M University; Estados UnidosFil: Prieto, Jose Luis. Millennium Institute Of Astrophysics; Chile. Universidad Diego Portales; ChileFil: González, Luis. Universidad de Chile; ChileFil: Cappellaro, Enrico. Osservatorio Astronomico Di Padova; ChileFil: Navarrete, Mauricio. Las Campanas Observatory; ChileFil: Pizzella, Alessandro. Università di Padova; ItaliaFil: Ruiz, Maria T.. Universidad de Chile; ChileFil: Smith, R. Chris. Cerro Tololo Inter American Observatory; ChileFil: Turatto, Massimo. Osservatorio Astronomico Di Padova; ItaliaIOP Publishing2017-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/41312Gutiérrez, Claudia P.; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia Irene; González Gaitan, Santiago; et al.; Type II supernova spectral diversity, I: observations, sample characterization, and spectral line evolution; IOP Publishing; Astrophysical Journal; 850; 1; 11-20170004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa8f52info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/1538-4357/aa8f52/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:31:07Zoai:ri.conicet.gov.ar:11336/41312instacron: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:34982025-10-22 11:31:07.617CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| 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. Supernovae Surveys Photometric techniques Spectroscophy |
| 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, Gaston Dessart, Luc Contreras, Carlos Valle, Massimo Della Freedman, Wendy L. Hsiao, Eric Y. Krisciunas, Kevin Madore, Barry F. Maza, José Suntzeff, Nicholas B. Prieto, Jose Luis González, Luis Cappellaro, Enrico Navarrete, Mauricio Pizzella, Alessandro Ruiz, Maria 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, Gaston Dessart, Luc Contreras, Carlos Valle, Massimo Della Freedman, Wendy L. Hsiao, Eric Y. Krisciunas, Kevin Madore, Barry F. Maza, José Suntzeff, Nicholas B. Prieto, Jose Luis González, Luis Cappellaro, Enrico Navarrete, Mauricio Pizzella, Alessandro Ruiz, Maria 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, Gaston Dessart, Luc Contreras, Carlos Valle, Massimo Della Freedman, Wendy L. Hsiao, Eric Y. Krisciunas, Kevin Madore, Barry F. Maza, José Suntzeff, Nicholas B. Prieto, Jose Luis González, Luis Cappellaro, Enrico Navarrete, Mauricio Pizzella, Alessandro Ruiz, Maria 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 |
Supernovae Surveys Photometric techniques Spectroscophy |
| topic |
Supernovae Surveys Photometric techniques Spectroscophy |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| 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-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. Fil: Gutiérrez, Claudia P.. Universidad de Chile; Chile. University of Southampton; Reino Unido Fil: Anderson, Joseph P.. European Southern Observatory Santiago; Chile Fil: Hamuy, Mario. Universidad de Chile; Chile. Millennium Institute Of Astrophysics; Chile Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile Fil: González Gaitan, Santiago. Millennium Institute Of Astrophysics; Chile. Universidad de Chile; Chile Fil: Stritzinger, Maximilian D.. University Aarhus; Dinamarca Fil: Phillips, Mark M.. Las Campanas Observatory; Chile Fil: Galbany, Lluis. University of Pittsburgh at Johnstown; Estados Unidos. University of Pittsburgh; Estados Unidos Fil: Folatelli, Gaston. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Dessart, Luc. Universidad de Chile; Chile Fil: Contreras, Carlos. Las Campanas Observatory; Chile Fil: Valle, Massimo Della. Osservatorio Astronomico Di Capodimonte; Italia Fil: Freedman, Wendy L.. University of Chicago; Estados Unidos Fil: Hsiao, Eric Y.. Florida State University; Estados Unidos Fil: Krisciunas, Kevin. Texas A&M University; Estados Unidos Fil: Madore, Barry F.. Observatories of the Carnegie Institution for Science; Estados Unidos Fil: Maza, José. Universidad de Chile; Chile Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos Fil: Prieto, Jose Luis. Millennium Institute Of Astrophysics; Chile. Universidad Diego Portales; Chile Fil: González, Luis. Universidad de Chile; Chile Fil: Cappellaro, Enrico. Osservatorio Astronomico Di Padova; Chile Fil: Navarrete, Mauricio. Las Campanas Observatory; Chile Fil: Pizzella, Alessandro. Università di Padova; Italia Fil: Ruiz, Maria T.. Universidad de Chile; Chile Fil: Smith, R. Chris. Cerro Tololo Inter American Observatory; Chile Fil: Turatto, Massimo. Osservatorio Astronomico Di Padova; Italia |
| 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-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. |
| publishDate |
2017 |
| dc.date.none.fl_str_mv |
2017-11 |
| 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 |
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article |
| status_str |
publishedVersion |
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http://hdl.handle.net/11336/41312 Gutiérrez, Claudia P.; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia Irene; González Gaitan, Santiago; et al.; Type II supernova spectral diversity, I: observations, sample characterization, and spectral line evolution; IOP Publishing; Astrophysical Journal; 850; 1; 11-2017 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/41312 |
| identifier_str_mv |
Gutiérrez, Claudia P.; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia Irene; González Gaitan, Santiago; et al.; Type II supernova spectral diversity, I: observations, sample characterization, and spectral line evolution; IOP Publishing; Astrophysical Journal; 850; 1; 11-2017 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa8f52 info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/1538-4357/aa8f52/meta |
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openAccess |
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application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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