The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf
- Autores
- Stritzinger, M. D.; Taddia, F.; Holmbo, S.; Baron, E.; Contreras, C.; Karamehmetoglu, E.; Phillips, M.M.; Sollerman, J.; Suntzeff, N.B.; Vinko, J.; Ashall, C.; Avila, C.; Burns, C. R.; Campillay, A.; Castellon, S.; Folatelli, Gaston; Galbany, L.; Hoeflich, Peter; Hsiao, E. Y.; Marion, G. H.; Morrell, Nidia Irene; Wheeler, J. C.
- Año de publicación
- 2020
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M, a 56Ni mass of 0.16 ± 0.02 M, and a progenitor-star radius of 28.0 ± 7.5 R. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of 20-25 M zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of 10 M and extended (∼100 R) envelopes also broadly match the observations of LSQ13abf.
Fil: Stritzinger, M. D.. University Aarhus; Dinamarca
Fil: Taddia, F.. University Aarhus; Dinamarca
Fil: Holmbo, S.. University Aarhus; Dinamarca
Fil: Baron, E.. University Aarhus; Dinamarca. Oklahoma State University; Estados Unidos
Fil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; Chile
Fil: Karamehmetoglu, E.. University Aarhus; Dinamarca. Stockholms Universitet; Suecia
Fil: Phillips, M.M.. Las Campanas Observatory; Chile
Fil: Sollerman, J.. Stockholms Universitet; Suecia
Fil: Suntzeff, N.B.. Texas A&M University; Estados Unidos
Fil: Vinko, J.. University of Texas at Austin; Estados Unidos
Fil: Ashall, C.. Florida State University; Estados Unidos
Fil: Avila, C.. Las Campanas Observatory; Chile
Fil: Burns, C. R.. Carnegie Observatories; Estados Unidos
Fil: Campillay, A.. Las Campanas Observatory; Chile
Fil: Castellon, S.. Las Campanas Observatory; Chile
Fil: Folatelli, Gaston. Universidad Nacional de La Plata; 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: Galbany, L.. Universidad de Granada; España
Fil: Hoeflich, Peter. Florida State University; Estados Unidos
Fil: Hsiao, E. Y.. Florida State University; Estados Unidos
Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos
Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile
Fil: Wheeler, J. C.. University of Texas at Austin; Estados Unidos - Materia
-
SUPERNOVAE: GENERAL
SUPERNOVAE: INDIVIDUAL: IPTF13BVN
SUPERNOVAE: INDIVIDUAL: LSQ13ABF
SUPERNOVAE: INDIVIDUAL: SN 1999EX
SUPERNOVAE: INDIVIDUAL: SN 2008D - 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:11336/145721
Ver los metadatos del registro completo
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The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abfStritzinger, M. D.Taddia, F.Holmbo, S.Baron, E.Contreras, C.Karamehmetoglu, E.Phillips, M.M.Sollerman, J.Suntzeff, N.B.Vinko, J.Ashall, C.Avila, C.Burns, C. R.Campillay, A.Castellon, S.Folatelli, GastonGalbany, L.Hoeflich, PeterHsiao, E. Y.Marion, G. H.Morrell, Nidia IreneWheeler, J. C.SUPERNOVAE: GENERALSUPERNOVAE: INDIVIDUAL: IPTF13BVNSUPERNOVAE: INDIVIDUAL: LSQ13ABFSUPERNOVAE: INDIVIDUAL: SN 1999EXSUPERNOVAE: INDIVIDUAL: SN 2008Dhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M, a 56Ni mass of 0.16 ± 0.02 M, and a progenitor-star radius of 28.0 ± 7.5 R. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of 20-25 M zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of 10 M and extended (∼100 R) envelopes also broadly match the observations of LSQ13abf.Fil: Stritzinger, M. D.. University Aarhus; DinamarcaFil: Taddia, F.. University Aarhus; DinamarcaFil: Holmbo, S.. University Aarhus; DinamarcaFil: Baron, E.. University Aarhus; Dinamarca. Oklahoma State University; Estados UnidosFil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; ChileFil: Karamehmetoglu, E.. University Aarhus; Dinamarca. Stockholms Universitet; SueciaFil: Phillips, M.M.. Las Campanas Observatory; ChileFil: Sollerman, J.. Stockholms Universitet; SueciaFil: Suntzeff, N.B.. Texas A&M University; Estados UnidosFil: Vinko, J.. University of Texas at Austin; Estados UnidosFil: Ashall, C.. Florida State University; Estados UnidosFil: Avila, C.. Las Campanas Observatory; ChileFil: Burns, C. R.. Carnegie Observatories; Estados UnidosFil: Campillay, A.. Las Campanas Observatory; ChileFil: Castellon, S.. Las Campanas Observatory; ChileFil: Folatelli, Gaston. Universidad Nacional de La Plata; 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: Galbany, L.. Universidad de Granada; EspañaFil: Hoeflich, Peter. Florida State University; Estados UnidosFil: Hsiao, E. Y.. Florida State University; Estados UnidosFil: Marion, G. H.. University of Texas at Austin; Estados UnidosFil: Morrell, Nidia Irene. Las Campanas Observatory; ChileFil: Wheeler, J. C.. University of Texas at Austin; Estados UnidosEDP Sciences2020-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/145721Stritzinger, M. D.; Taddia, F.; Holmbo, S.; Baron, E.; Contreras, C.; et al.; The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf; EDP Sciences; Astronomy and Astrophysics; 634; A21; 2-2020; 1-170004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201936619info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2020/02/aa36619-19/aa36619-19.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 Técnicas2025-09-29T09:32:27Zoai:ri.conicet.gov.ar:11336/145721instacron: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 09:32:27.66CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| title |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| spellingShingle |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf Stritzinger, M. D. SUPERNOVAE: GENERAL SUPERNOVAE: INDIVIDUAL: IPTF13BVN SUPERNOVAE: INDIVIDUAL: LSQ13ABF SUPERNOVAE: INDIVIDUAL: SN 1999EX SUPERNOVAE: INDIVIDUAL: SN 2008D |
| title_short |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| title_full |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| title_fullStr |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| title_full_unstemmed |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| title_sort |
The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf |
| dc.creator.none.fl_str_mv |
Stritzinger, M. D. Taddia, F. Holmbo, S. Baron, E. Contreras, C. Karamehmetoglu, E. Phillips, M.M. Sollerman, J. Suntzeff, N.B. Vinko, J. Ashall, C. Avila, C. Burns, C. R. Campillay, A. Castellon, S. Folatelli, Gaston Galbany, L. Hoeflich, Peter Hsiao, E. Y. Marion, G. H. Morrell, Nidia Irene Wheeler, J. C. |
| author |
Stritzinger, M. D. |
| author_facet |
Stritzinger, M. D. Taddia, F. Holmbo, S. Baron, E. Contreras, C. Karamehmetoglu, E. Phillips, M.M. Sollerman, J. Suntzeff, N.B. Vinko, J. Ashall, C. Avila, C. Burns, C. R. Campillay, A. Castellon, S. Folatelli, Gaston Galbany, L. Hoeflich, Peter Hsiao, E. Y. Marion, G. H. Morrell, Nidia Irene Wheeler, J. C. |
| author_role |
author |
| author2 |
Taddia, F. Holmbo, S. Baron, E. Contreras, C. Karamehmetoglu, E. Phillips, M.M. Sollerman, J. Suntzeff, N.B. Vinko, J. Ashall, C. Avila, C. Burns, C. R. Campillay, A. Castellon, S. Folatelli, Gaston Galbany, L. Hoeflich, Peter Hsiao, E. Y. Marion, G. H. Morrell, Nidia Irene Wheeler, J. C. |
| author2_role |
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: GENERAL SUPERNOVAE: INDIVIDUAL: IPTF13BVN SUPERNOVAE: INDIVIDUAL: LSQ13ABF SUPERNOVAE: INDIVIDUAL: SN 1999EX SUPERNOVAE: INDIVIDUAL: SN 2008D |
| topic |
SUPERNOVAE: GENERAL SUPERNOVAE: INDIVIDUAL: IPTF13BVN SUPERNOVAE: INDIVIDUAL: LSQ13ABF SUPERNOVAE: INDIVIDUAL: SN 1999EX SUPERNOVAE: INDIVIDUAL: SN 2008D |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M, a 56Ni mass of 0.16 ± 0.02 M, and a progenitor-star radius of 28.0 ± 7.5 R. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of 20-25 M zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of 10 M and extended (∼100 R) envelopes also broadly match the observations of LSQ13abf. Fil: Stritzinger, M. D.. University Aarhus; Dinamarca Fil: Taddia, F.. University Aarhus; Dinamarca Fil: Holmbo, S.. University Aarhus; Dinamarca Fil: Baron, E.. University Aarhus; Dinamarca. Oklahoma State University; Estados Unidos Fil: Contreras, C.. University Aarhus; Dinamarca. Las Campanas Observatory; Chile Fil: Karamehmetoglu, E.. University Aarhus; Dinamarca. Stockholms Universitet; Suecia Fil: Phillips, M.M.. Las Campanas Observatory; Chile Fil: Sollerman, J.. Stockholms Universitet; Suecia Fil: Suntzeff, N.B.. Texas A&M University; Estados Unidos Fil: Vinko, J.. University of Texas at Austin; Estados Unidos Fil: Ashall, C.. Florida State University; Estados Unidos Fil: Avila, C.. Las Campanas Observatory; Chile Fil: Burns, C. R.. Carnegie Observatories; Estados Unidos Fil: Campillay, A.. Las Campanas Observatory; Chile Fil: Castellon, S.. Las Campanas Observatory; Chile Fil: Folatelli, Gaston. Universidad Nacional de La Plata; 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: Galbany, L.. Universidad de Granada; España Fil: Hoeflich, Peter. Florida State University; Estados Unidos Fil: Hsiao, E. Y.. Florida State University; Estados Unidos Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile Fil: Wheeler, J. C.. University of Texas at Austin; Estados Unidos |
| description |
Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M, a 56Ni mass of 0.16 ± 0.02 M, and a progenitor-star radius of 28.0 ± 7.5 R. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of 20-25 M zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of 10 M and extended (∼100 R) envelopes also broadly match the observations of LSQ13abf. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020-02 |
| 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 |
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publishedVersion |
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http://hdl.handle.net/11336/145721 Stritzinger, M. D.; Taddia, F.; Holmbo, S.; Baron, E.; Contreras, C.; et al.; The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf; EDP Sciences; Astronomy and Astrophysics; 634; A21; 2-2020; 1-17 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/145721 |
| identifier_str_mv |
Stritzinger, M. D.; Taddia, F.; Holmbo, S.; Baron, E.; Contreras, C.; et al.; The Carnegie Supernova Project II: Early observations and progenitor constraints of the Type Ib supernova LSQ13abf; EDP Sciences; Astronomy and Astrophysics; 634; A21; 2-2020; 1-17 0004-6361 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201936619 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2020/02/aa36619-19/aa36619-19.html |
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openAccess |
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EDP Sciences |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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