Strong near-infrared carbon in the Type Ia supernova iPTF13ebh
- Autores
- Hsiao, E. Y.; Burns, C. R.; Contreras, C.; Höflich, P.; Sand, D.; Marion, G. H.; Phillips, M. M.; Stritzinger, M.; González Gaitán, S.; Mason, R. E.; Folatelli, Gaston; Parent, E.; Gall, C.; Amanullah, R.; Anupama, G. C.; Arcavi, I.; Banerjee, D. P. K.; Beletsky, Y.; Blanc, G. A.; Bloom, J. S.; Brown, P. J.; Campillay, A.; Cao, Y.; De Cia, A.; Diamond, T.; Freedman, W. L.; Gonzalez, C.; Goobar, A.; Holmbo, S.; Howell, D. A.
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ~4 days.
Fil: Hsiao, E. Y. . Aarhus University; Dinamarca
Fil: Burns, C. R. . Carnegie Observatories; Estados Unidos
Fil: Contreras, C.. Carnegie Observatories, Las Campanas Observatory; Chile
Fil: Höflich, P.. Florida State University; Estados Unidos
Fil: Sand, D.. Texas Tech University; Estados Unidos
Fil: Marion, G. H. . University of Texas at Austin; Estados Unidos
Fil: Phillips, M. M. . Carnegie Observatories. Las Campanas Observatory; Chile
Fil: Stritzinger, M.. Aarhus University; Dinamarca
Fil: González Gaitán, S.. Universidad de Chile; Chile
Fil: Mason, R. E. . Gemini Observatory; Estados Unidos
Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de La Plata; Argentina
Fil: Parent, E.. Bishop’s University; Canadá
Fil: Gall, C.. Aarhus University; Dinamarca
Fil: Amanullah, R.. Stockholm University; Suecia
Fil: Anupama, G. C. . Indian Institute of Astrophysics; India
Fil: Arcavi, I.. University of California; Estados Unidos
Fil: Banerjee, D. P. K. . Physical Research Laboratory; India
Fil: Beletsky, Y.. Carnegie Observatories. Las Campanas Observatory; Chile
Fil: Blanc, G. A. . Carnegie Observatories; Chile
Fil: Bloom, J. S. . University of California; Estados Unidos
Fil: Brown, P. J. . Texas A&M University; Estados Unidos
Fil: Campillay, A.. Carnegie Observatories. Las Campanas Observatory; Chile
Fil: Cao, Y.. Lawrence Berkeley National Laboratory; Estados Unidos
Fil: De Cia, A. . Weizmann Institute of Science; Israel
Fil: Diamond, T.. Florida State University; Estados Unidos
Fil: Freedman, W. L.. Carnegie Observatories; Estados Unidos
Fil: Gonzalez, C.. Carnegie Observatories; Estados Unidos
Fil: Goobar, A.. Stockholm University; Suecia
Fil: Holmbo, S.. Aarhus University; Dinamarca
Fil: Howell, D. A.. Las Cumbres Observatory Global Telescope Network; Estados Unidos. University of California; Estados Unidos - Materia
-
Supernovae
Infrarred
IPTF13EBH (supernova) - 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:11336/13124
Ver los metadatos del registro completo
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Strong near-infrared carbon in the Type Ia supernova iPTF13ebhHsiao, E. Y. Burns, C. R. Contreras, C.Höflich, P.Sand, D.Marion, G. H. Phillips, M. M. Stritzinger, M.González Gaitán, S.Mason, R. E. Folatelli, GastonParent, E.Gall, C.Amanullah, R.Anupama, G. C. Arcavi, I.Banerjee, D. P. K. Beletsky, Y.Blanc, G. A. Bloom, J. S. Brown, P. J. Campillay, A.Cao, Y.De Cia, A. Diamond, T.Freedman, W. L.Gonzalez, C.Goobar, A.Holmbo, S.Howell, D. A.SupernovaeInfrarredIPTF13EBH (supernova)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ~4 days.Fil: Hsiao, E. Y. . Aarhus University; DinamarcaFil: Burns, C. R. . Carnegie Observatories; Estados UnidosFil: Contreras, C.. Carnegie Observatories, Las Campanas Observatory; ChileFil: Höflich, P.. Florida State University; Estados UnidosFil: Sand, D.. Texas Tech University; Estados UnidosFil: Marion, G. H. . University of Texas at Austin; Estados UnidosFil: Phillips, M. M. . Carnegie Observatories. Las Campanas Observatory; ChileFil: Stritzinger, M.. Aarhus University; DinamarcaFil: González Gaitán, S.. Universidad de Chile; ChileFil: Mason, R. E. . Gemini Observatory; Estados UnidosFil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de La Plata; ArgentinaFil: Parent, E.. Bishop’s University; CanadáFil: Gall, C.. Aarhus University; DinamarcaFil: Amanullah, R.. Stockholm University; SueciaFil: Anupama, G. C. . Indian Institute of Astrophysics; IndiaFil: Arcavi, I.. University of California; Estados UnidosFil: Banerjee, D. P. K. . Physical Research Laboratory; IndiaFil: Beletsky, Y.. Carnegie Observatories. Las Campanas Observatory; ChileFil: Blanc, G. A. . Carnegie Observatories; ChileFil: Bloom, J. S. . University of California; Estados UnidosFil: Brown, P. J. . Texas A&M University; Estados UnidosFil: Campillay, A.. Carnegie Observatories. Las Campanas Observatory; ChileFil: Cao, Y.. Lawrence Berkeley National Laboratory; Estados UnidosFil: De Cia, A. . Weizmann Institute of Science; IsraelFil: Diamond, T.. Florida State University; Estados UnidosFil: Freedman, W. L.. Carnegie Observatories; Estados UnidosFil: Gonzalez, C.. Carnegie Observatories; Estados UnidosFil: Goobar, A.. Stockholm University; SueciaFil: Holmbo, S.. Aarhus University; DinamarcaFil: Howell, D. A.. Las Cumbres Observatory Global Telescope Network; Estados Unidos. University of California; Estados UnidosEdp Sciences2015-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/13124Hsiao, E. Y. ; Burns, C. R. ; Contreras, C.; Höflich, P.; Sand, D.; et al.; Strong near-infrared carbon in the Type Ia supernova iPTF13ebh; Edp Sciences; Astronomy And Astrophysics; 578; A9; 6-2015; 9-270004-6361enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201425297info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/06/aa25297-14/aa25297-14.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:00:08Zoai:ri.conicet.gov.ar:11336/13124instacron: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 10:00:08.326CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| title |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| spellingShingle |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh Hsiao, E. Y. Supernovae Infrarred IPTF13EBH (supernova) |
| title_short |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| title_full |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| title_fullStr |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| title_full_unstemmed |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| title_sort |
Strong near-infrared carbon in the Type Ia supernova iPTF13ebh |
| dc.creator.none.fl_str_mv |
Hsiao, E. Y. Burns, C. R. Contreras, C. Höflich, P. Sand, D. Marion, G. H. Phillips, M. M. Stritzinger, M. González Gaitán, S. Mason, R. E. Folatelli, Gaston Parent, E. Gall, C. Amanullah, R. Anupama, G. C. Arcavi, I. Banerjee, D. P. K. Beletsky, Y. Blanc, G. A. Bloom, J. S. Brown, P. J. Campillay, A. Cao, Y. De Cia, A. Diamond, T. Freedman, W. L. Gonzalez, C. Goobar, A. Holmbo, S. Howell, D. A. |
| author |
Hsiao, E. Y. |
| author_facet |
Hsiao, E. Y. Burns, C. R. Contreras, C. Höflich, P. Sand, D. Marion, G. H. Phillips, M. M. Stritzinger, M. González Gaitán, S. Mason, R. E. Folatelli, Gaston Parent, E. Gall, C. Amanullah, R. Anupama, G. C. Arcavi, I. Banerjee, D. P. K. Beletsky, Y. Blanc, G. A. Bloom, J. S. Brown, P. J. Campillay, A. Cao, Y. De Cia, A. Diamond, T. Freedman, W. L. Gonzalez, C. Goobar, A. Holmbo, S. Howell, D. A. |
| author_role |
author |
| author2 |
Burns, C. R. Contreras, C. Höflich, P. Sand, D. Marion, G. H. Phillips, M. M. Stritzinger, M. González Gaitán, S. Mason, R. E. Folatelli, Gaston Parent, E. Gall, C. Amanullah, R. Anupama, G. C. Arcavi, I. Banerjee, D. P. K. Beletsky, Y. Blanc, G. A. Bloom, J. S. Brown, P. J. Campillay, A. Cao, Y. De Cia, A. Diamond, T. Freedman, W. L. Gonzalez, C. Goobar, A. Holmbo, S. Howell, D. A. |
| 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 author author author author |
| dc.subject.none.fl_str_mv |
Supernovae Infrarred IPTF13EBH (supernova) |
| topic |
Supernovae Infrarred IPTF13EBH (supernova) |
| 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 near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ~4 days. Fil: Hsiao, E. Y. . Aarhus University; Dinamarca Fil: Burns, C. R. . Carnegie Observatories; Estados Unidos Fil: Contreras, C.. Carnegie Observatories, Las Campanas Observatory; Chile Fil: Höflich, P.. Florida State University; Estados Unidos Fil: Sand, D.. Texas Tech University; Estados Unidos Fil: Marion, G. H. . University of Texas at Austin; Estados Unidos Fil: Phillips, M. M. . Carnegie Observatories. Las Campanas Observatory; Chile Fil: Stritzinger, M.. Aarhus University; Dinamarca Fil: González Gaitán, S.. Universidad de Chile; Chile Fil: Mason, R. E. . Gemini Observatory; Estados Unidos Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina. Universidad Nacional de La Plata; Argentina Fil: Parent, E.. Bishop’s University; Canadá Fil: Gall, C.. Aarhus University; Dinamarca Fil: Amanullah, R.. Stockholm University; Suecia Fil: Anupama, G. C. . Indian Institute of Astrophysics; India Fil: Arcavi, I.. University of California; Estados Unidos Fil: Banerjee, D. P. K. . Physical Research Laboratory; India Fil: Beletsky, Y.. Carnegie Observatories. Las Campanas Observatory; Chile Fil: Blanc, G. A. . Carnegie Observatories; Chile Fil: Bloom, J. S. . University of California; Estados Unidos Fil: Brown, P. J. . Texas A&M University; Estados Unidos Fil: Campillay, A.. Carnegie Observatories. Las Campanas Observatory; Chile Fil: Cao, Y.. Lawrence Berkeley National Laboratory; Estados Unidos Fil: De Cia, A. . Weizmann Institute of Science; Israel Fil: Diamond, T.. Florida State University; Estados Unidos Fil: Freedman, W. L.. Carnegie Observatories; Estados Unidos Fil: Gonzalez, C.. Carnegie Observatories; Estados Unidos Fil: Goobar, A.. Stockholm University; Suecia Fil: Holmbo, S.. Aarhus University; Dinamarca Fil: Howell, D. A.. Las Cumbres Observatory Global Telescope Network; Estados Unidos. University of California; Estados Unidos |
| description |
We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C i lines, and the C iλ1.0693 μm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C i compared to the weaker optical C ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Δm15(B) = 1.79 ± 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si iiλ0.6355 μm line, implying a long dark phase of ~4 days. |
| publishDate |
2015 |
| dc.date.none.fl_str_mv |
2015-06 |
| 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/11336/13124 Hsiao, E. Y. ; Burns, C. R. ; Contreras, C.; Höflich, P.; Sand, D.; et al.; Strong near-infrared carbon in the Type Ia supernova iPTF13ebh; Edp Sciences; Astronomy And Astrophysics; 578; A9; 6-2015; 9-27 0004-6361 |
| url |
http://hdl.handle.net/11336/13124 |
| identifier_str_mv |
Hsiao, E. Y. ; Burns, C. R. ; Contreras, C.; Höflich, P.; Sand, D.; et al.; Strong near-infrared carbon in the Type Ia supernova iPTF13ebh; Edp Sciences; Astronomy And Astrophysics; 578; A9; 6-2015; 9-27 0004-6361 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201425297 info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/06/aa25297-14/aa25297-14.html |
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openAccess |
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Edp Sciences |
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