Type II supernovae as probes of environment metallicity: observations of host He II regions

Autores
Anderson, J. P.; Gutiérrez, C. P.; Dessart, L.; Hamuy, M.; Galbany, L.; Morrell, Nidia Irene; Stritzinger, M. D.; Phillips, M. M.; Folatelli, Gastón; Boffin, H. M. J.; Jaeger, T. de; Kuncarayakti, H.; Prieto, J. L.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims. To assess this accuracy we present a sample of type II supernova host H II-region spectroscopy, from which environment oxygen abundances have been derived. These environment abundances are compared to the observed strength of metal lines in supernova spectra. Methods. Combining our sample with measurements from the literature, we present oxygen abundances of 119 host H II regions by extracting emission line fluxes and using abundance diagnostics. These abundances are then compared to equivalent widths of Fe II 5018 Å at various time and colour epochs. Results. Our distribution of inferred type II supernova host H II-region abundances has a range of ∼0.6 dex. We confirm the dearth of type II supernovae exploding at metallicities lower than those found (on average) in the Large Magellanic Cloud. The equivalent width of Fe II 5018 Å at 50 days post-explosion shows a statistically significant correlation with host H II-region oxygen abundance. The strength of this correlation increases if one excludes abundance measurements derived far from supernova explosion sites. The correlation significance also increases if we only analyse a "gold" IIP sample, and if a colour epoch is used in place of time. In addition, no evidence is found of a correlation between progenitor metallicity and supernova light-curve or spectral properties - except for that stated above with respect to Fe II 5018 Å equivalent widths - suggesting progenitor metallicity is not a driving factor in producing the diversity that is observed in our sample. Conclusions. This study provides observational evidence of the usefulness of type II supernovae as metallicity indicators. We finish with a discussion of the methodology needed to use supernova spectra as independent metallicity diagnostics throughout the Universe.
Este documento tiene una corrección (ver documento relacionado).
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
galaxies: abundances
HII regions
supernovae: general
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:10915/86643
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/86643
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Type II supernovae as probes of environment metallicity: observations of host He II regionsAnderson, J. P.Gutiérrez, C. P.Dessart, L.Hamuy, M.Galbany, L.Morrell, Nidia IreneStritzinger, M. D.Phillips, M. M.Folatelli, GastónBoffin, H. M. J.Jaeger, T. deKuncarayakti, H.Prieto, J. L.Ciencias Astronómicasgalaxies: abundancesHII regionssupernovae: generalContext. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims. To assess this accuracy we present a sample of type II supernova host H II-region spectroscopy, from which environment oxygen abundances have been derived. These environment abundances are compared to the observed strength of metal lines in supernova spectra. Methods. Combining our sample with measurements from the literature, we present oxygen abundances of 119 host H II regions by extracting emission line fluxes and using abundance diagnostics. These abundances are then compared to equivalent widths of Fe II 5018 Å at various time and colour epochs. Results. Our distribution of inferred type II supernova host H II-region abundances has a range of ∼0.6 dex. We confirm the dearth of type II supernovae exploding at metallicities lower than those found (on average) in the Large Magellanic Cloud. The equivalent width of Fe II 5018 Å at 50 days post-explosion shows a statistically significant correlation with host H II-region oxygen abundance. The strength of this correlation increases if one excludes abundance measurements derived far from supernova explosion sites. The correlation significance also increases if we only analyse a "gold" IIP sample, and if a colour epoch is used in place of time. In addition, no evidence is found of a correlation between progenitor metallicity and supernova light-curve or spectral properties - except for that stated above with respect to Fe II 5018 Å equivalent widths - suggesting progenitor metallicity is not a driving factor in producing the diversity that is observed in our sample. Conclusions. This study provides observational evidence of the usefulness of type II supernovae as metallicity indicators. We finish with a discussion of the methodology needed to use supernova spectra as independent metallicity diagnostics throughout the Universe.Este documento tiene una corrección (ver documento relacionado).Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2016info: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/10915/86643enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527691info:eu-repo/semantics/reference/hdl/10915/87052info: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:UNLP2025-10-22T16:57:42Zoai:sedici.unlp.edu.ar:10915/86643Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:57:42.23SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Type II supernovae as probes of environment metallicity: observations of host He II regions
title Type II supernovae as probes of environment metallicity: observations of host He II regions
spellingShingle Type II supernovae as probes of environment metallicity: observations of host He II regions
Anderson, J. P.
Ciencias Astronómicas
galaxies: abundances
HII regions
supernovae: general
title_short Type II supernovae as probes of environment metallicity: observations of host He II regions
title_full Type II supernovae as probes of environment metallicity: observations of host He II regions
title_fullStr Type II supernovae as probes of environment metallicity: observations of host He II regions
title_full_unstemmed Type II supernovae as probes of environment metallicity: observations of host He II regions
title_sort Type II supernovae as probes of environment metallicity: observations of host He II regions
dc.creator.none.fl_str_mv Anderson, J. P.
Gutiérrez, C. P.
Dessart, L.
Hamuy, M.
Galbany, L.
Morrell, Nidia Irene
Stritzinger, M. D.
Phillips, M. M.
Folatelli, Gastón
Boffin, H. M. J.
Jaeger, T. de
Kuncarayakti, H.
Prieto, J. L.
author Anderson, J. P.
author_facet Anderson, J. P.
Gutiérrez, C. P.
Dessart, L.
Hamuy, M.
Galbany, L.
Morrell, Nidia Irene
Stritzinger, M. D.
Phillips, M. M.
Folatelli, Gastón
Boffin, H. M. J.
Jaeger, T. de
Kuncarayakti, H.
Prieto, J. L.
author_role author
author2 Gutiérrez, C. P.
Dessart, L.
Hamuy, M.
Galbany, L.
Morrell, Nidia Irene
Stritzinger, M. D.
Phillips, M. M.
Folatelli, Gastón
Boffin, H. M. J.
Jaeger, T. de
Kuncarayakti, H.
Prieto, J. L.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
galaxies: abundances
HII regions
supernovae: general
topic Ciencias Astronómicas
galaxies: abundances
HII regions
supernovae: general
dc.description.none.fl_txt_mv Context. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims. To assess this accuracy we present a sample of type II supernova host H II-region spectroscopy, from which environment oxygen abundances have been derived. These environment abundances are compared to the observed strength of metal lines in supernova spectra. Methods. Combining our sample with measurements from the literature, we present oxygen abundances of 119 host H II regions by extracting emission line fluxes and using abundance diagnostics. These abundances are then compared to equivalent widths of Fe II 5018 Å at various time and colour epochs. Results. Our distribution of inferred type II supernova host H II-region abundances has a range of ∼0.6 dex. We confirm the dearth of type II supernovae exploding at metallicities lower than those found (on average) in the Large Magellanic Cloud. The equivalent width of Fe II 5018 Å at 50 days post-explosion shows a statistically significant correlation with host H II-region oxygen abundance. The strength of this correlation increases if one excludes abundance measurements derived far from supernova explosion sites. The correlation significance also increases if we only analyse a "gold" IIP sample, and if a colour epoch is used in place of time. In addition, no evidence is found of a correlation between progenitor metallicity and supernova light-curve or spectral properties - except for that stated above with respect to Fe II 5018 Å equivalent widths - suggesting progenitor metallicity is not a driving factor in producing the diversity that is observed in our sample. Conclusions. This study provides observational evidence of the usefulness of type II supernovae as metallicity indicators. We finish with a discussion of the methodology needed to use supernova spectra as independent metallicity diagnostics throughout the Universe.
Este documento tiene una corrección (ver documento relacionado).
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description Context. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims. To assess this accuracy we present a sample of type II supernova host H II-region spectroscopy, from which environment oxygen abundances have been derived. These environment abundances are compared to the observed strength of metal lines in supernova spectra. Methods. Combining our sample with measurements from the literature, we present oxygen abundances of 119 host H II regions by extracting emission line fluxes and using abundance diagnostics. These abundances are then compared to equivalent widths of Fe II 5018 Å at various time and colour epochs. Results. Our distribution of inferred type II supernova host H II-region abundances has a range of ∼0.6 dex. We confirm the dearth of type II supernovae exploding at metallicities lower than those found (on average) in the Large Magellanic Cloud. The equivalent width of Fe II 5018 Å at 50 days post-explosion shows a statistically significant correlation with host H II-region oxygen abundance. The strength of this correlation increases if one excludes abundance measurements derived far from supernova explosion sites. The correlation significance also increases if we only analyse a "gold" IIP sample, and if a colour epoch is used in place of time. In addition, no evidence is found of a correlation between progenitor metallicity and supernova light-curve or spectral properties - except for that stated above with respect to Fe II 5018 Å equivalent widths - suggesting progenitor metallicity is not a driving factor in producing the diversity that is observed in our sample. Conclusions. This study provides observational evidence of the usefulness of type II supernovae as metallicity indicators. We finish with a discussion of the methodology needed to use supernova spectra as independent metallicity diagnostics throughout the Universe.
publishDate 2016
dc.date.none.fl_str_mv 2016
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/10915/86643
url http://sedici.unlp.edu.ar/handle/10915/86643
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527691
info:eu-repo/semantics/reference/hdl/10915/87052
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
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reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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