Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae
- Autores
- Ashall, C.; Lu, J.; Hsiao, E. Y.; Hoeflich, P.; Phillips, M. M.; Galbany, Lluís; Burns, C. R.; Contreras, C.; Krisciunas, K.; Morrell, Nidia Irene; Stritzinger, M. D.; Suntzeff, Nicholas B.; Taddia, F.; Anais, J.; Baron, E.; Brown, P. J.; Busta, L.; Campillay, A.; Castellón, S.; Corco, C.; Davis, S.; Folatelli, Gaston; Förster, F.; Freedman, W. L.; Gonzaléz, C.; Hamuy, M.; Holmbo, S.; Kirshner, R. P.; Kumar, S.; Marion, G. H.; Mazzali, P.; Morokuma, T.; Nugent, P. E.; Persson, S. E.; Piro, A. L.; Roth, M.; Salgado, F.; Sand, D.J.; Seron, J.; Shahbandeh, M.; Shappee, B. J.
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present a multiwavelength photometric and spectroscopic analysis of 13 super-Chandrasekhar-mass/2003fg-like Type Ia supernovae (SNe Ia). Nine of these objects were observed by the Carnegie Supernova Project. The 2003fg-like SNe have slowly declining light curves (Δm 15(B) < 1.3 mag), and peak absolute B-band magnitudes of -19 < M B < -21 mag. Many of the 2003fg-like SNe are located in the same part of the luminosity-width relation as normal SNe Ia. In the optical B and V bands, the 2003fg-like SNe look like normal SNe Ia, but at redder wavelengths they diverge. Unlike other luminous SNe Ia, the 2003fg-like SNe generally have only one i-band maximum, which peaks after the epoch of the B-band maximum, while their near-IR (NIR) light-curve rise times can be ⪆40 days longer than those of normal SNe Ia. They are also at least 1 mag brighter in the NIR bands than normal SNe Ia, peaking above M H = -19 mag, and generally have negative Hubble residuals, which may be the cause of some systematics in dark-energy experiments. Spectroscopically, the 2003fg-like SNe exhibit peculiarities such as unburnt carbon well past maximum light, a large spread (8000-12,000 km s-1) in Si ii λ6355 velocities at maximum light with no rapid early velocity decline, and no clear H-band break at +10 days. We find that SNe with a larger pseudo-equivalent width of C ii at maximum light have lower Si ii λ6355 velocities and more slowly declining light curves. There are also multiple factors that contribute to the peak luminosity of 2003fg-like SNe. The explosion of a C-O degenerate core inside a carbon-rich envelope is consistent with these observations. Such a configuration may come from the core-degenerate scenario.
Fil: Ashall, C.. University Hawaii Institute For Astronomy; Estados Unidos
Fil: Lu, J.. Florida State University; Estados Unidos
Fil: Hsiao, E. Y.. Florida State University; Estados Unidos
Fil: Hoeflich, P.. Florida State University; Estados Unidos
Fil: Phillips, M. M.. Las Campanas Observatory; Chile
Fil: Galbany, Lluís. Instituto de Ciencias del Espacio; España
Fil: Burns, C. R.. Las Campanas Observatory; Chile
Fil: Contreras, C.. Las Campanas Observatory; Chile
Fil: Krisciunas, K.. Texas A&M University; Estados Unidos
Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile
Fil: Stritzinger, M. D.. University Aarhus; Dinamarca
Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos
Fil: Taddia, F.. University Aarhus; Dinamarca
Fil: Anais, J.. Las Campanas Observatory; Chile
Fil: Baron, E.. Oklahoma State University; Estados Unidos. Universitat Hamburg; Alemania
Fil: Brown, P. J.. Texas A&M University; Estados Unidos
Fil: Busta, L.. Las Campanas Observatory; Chile
Fil: Campillay, A.. Universidad de La Serena; Chile
Fil: Castellón, S.. Las Campanas Observatory; Chile
Fil: Corco, C.. Las Campanas Observatory; Chile. Soar Telescope; Chile
Fil: Davis, S.. University of California at Davis; Estados Unidos
Fil: Folatelli, Gaston. 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: Förster, F.. Universidad de Chile; Chile. Instituto Milenio de Astrofísica; Chile
Fil: Freedman, W. L.. University of Chicago; Estados Unidos
Fil: Gonzaléz, C.. Las Campanas Observatory; Chile
Fil: Hamuy, M.. Universidad de Chile; Chile
Fil: Holmbo, S.. University Aarhus; Dinamarca
Fil: Kirshner, R. P.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Kumar, S.. Florida State University; Estados Unidos
Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos
Fil: Mazzali, P.. Liverpool John Moores University; Reino Unido
Fil: Morokuma, T.. The University Of Tokyo; Japón
Fil: Nugent, P. E.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos
Fil: Persson, S. E.. Las Campanas Observatory; Chile
Fil: Piro, A. L.. Las Campanas Observatory; Chile
Fil: Roth, M.. Las Campanas Observatory; Chile
Fil: Salgado, F.. Las Campanas Observatory; Chile
Fil: Sand, D.J.. University of Arizona; Estados Unidos
Fil: Seron, J.. Las Campanas Observatory; Chile
Fil: Shahbandeh, M.. Florida State University; Estados Unidos
Fil: Shappee, B. J.. University Hawaii Institute For Astronomy; Estados Unidos - Materia
- SUPERNOVAE
- 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:11336/169535
Ver los metadatos del registro completo
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Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia SupernovaeAshall, C.Lu, J.Hsiao, E. Y.Hoeflich, P.Phillips, M. M.Galbany, LluísBurns, C. R.Contreras, C.Krisciunas, K.Morrell, Nidia IreneStritzinger, M. D.Suntzeff, Nicholas B.Taddia, F.Anais, J.Baron, E.Brown, P. J.Busta, L.Campillay, A.Castellón, S.Corco, C.Davis, S.Folatelli, GastonFörster, F.Freedman, W. L.Gonzaléz, C.Hamuy, M.Holmbo, S.Kirshner, R. P.Kumar, S.Marion, G. H.Mazzali, P.Morokuma, T.Nugent, P. E.Persson, S. E.Piro, A. L.Roth, M.Salgado, F.Sand, D.J.Seron, J.Shahbandeh, M.Shappee, B. J.SUPERNOVAEhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a multiwavelength photometric and spectroscopic analysis of 13 super-Chandrasekhar-mass/2003fg-like Type Ia supernovae (SNe Ia). Nine of these objects were observed by the Carnegie Supernova Project. The 2003fg-like SNe have slowly declining light curves (Δm 15(B) < 1.3 mag), and peak absolute B-band magnitudes of -19 < M B < -21 mag. Many of the 2003fg-like SNe are located in the same part of the luminosity-width relation as normal SNe Ia. In the optical B and V bands, the 2003fg-like SNe look like normal SNe Ia, but at redder wavelengths they diverge. Unlike other luminous SNe Ia, the 2003fg-like SNe generally have only one i-band maximum, which peaks after the epoch of the B-band maximum, while their near-IR (NIR) light-curve rise times can be ⪆40 days longer than those of normal SNe Ia. They are also at least 1 mag brighter in the NIR bands than normal SNe Ia, peaking above M H = -19 mag, and generally have negative Hubble residuals, which may be the cause of some systematics in dark-energy experiments. Spectroscopically, the 2003fg-like SNe exhibit peculiarities such as unburnt carbon well past maximum light, a large spread (8000-12,000 km s-1) in Si ii λ6355 velocities at maximum light with no rapid early velocity decline, and no clear H-band break at +10 days. We find that SNe with a larger pseudo-equivalent width of C ii at maximum light have lower Si ii λ6355 velocities and more slowly declining light curves. There are also multiple factors that contribute to the peak luminosity of 2003fg-like SNe. The explosion of a C-O degenerate core inside a carbon-rich envelope is consistent with these observations. Such a configuration may come from the core-degenerate scenario.Fil: Ashall, C.. University Hawaii Institute For Astronomy; Estados UnidosFil: Lu, J.. Florida State University; Estados UnidosFil: Hsiao, E. Y.. Florida State University; Estados UnidosFil: Hoeflich, P.. Florida State University; Estados UnidosFil: Phillips, M. M.. Las Campanas Observatory; ChileFil: Galbany, Lluís. Instituto de Ciencias del Espacio; EspañaFil: Burns, C. R.. Las Campanas Observatory; ChileFil: Contreras, C.. Las Campanas Observatory; ChileFil: Krisciunas, K.. Texas A&M University; Estados UnidosFil: Morrell, Nidia Irene. Las Campanas Observatory; ChileFil: Stritzinger, M. D.. University Aarhus; DinamarcaFil: Suntzeff, Nicholas B.. Texas A&M University; Estados UnidosFil: Taddia, F.. University Aarhus; DinamarcaFil: Anais, J.. Las Campanas Observatory; ChileFil: Baron, E.. Oklahoma State University; Estados Unidos. Universitat Hamburg; AlemaniaFil: Brown, P. J.. Texas A&M University; Estados UnidosFil: Busta, L.. Las Campanas Observatory; ChileFil: Campillay, A.. Universidad de La Serena; ChileFil: Castellón, S.. Las Campanas Observatory; ChileFil: Corco, C.. Las Campanas Observatory; Chile. Soar Telescope; ChileFil: Davis, S.. University of California at Davis; Estados UnidosFil: Folatelli, Gaston. 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: Förster, F.. Universidad de Chile; Chile. Instituto Milenio de Astrofísica; ChileFil: Freedman, W. L.. University of Chicago; Estados UnidosFil: Gonzaléz, C.. Las Campanas Observatory; ChileFil: Hamuy, M.. Universidad de Chile; ChileFil: Holmbo, S.. University Aarhus; DinamarcaFil: Kirshner, R. P.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kumar, S.. Florida State University; Estados UnidosFil: Marion, G. H.. University of Texas at Austin; Estados UnidosFil: Mazzali, P.. Liverpool John Moores University; Reino UnidoFil: Morokuma, T.. The University Of Tokyo; JapónFil: Nugent, P. E.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados UnidosFil: Persson, S. E.. Las Campanas Observatory; ChileFil: Piro, A. L.. Las Campanas Observatory; ChileFil: Roth, M.. Las Campanas Observatory; ChileFil: Salgado, F.. Las Campanas Observatory; ChileFil: Sand, D.J.. University of Arizona; Estados UnidosFil: Seron, J.. Las Campanas Observatory; ChileFil: Shahbandeh, M.. Florida State University; Estados UnidosFil: Shappee, B. J.. University Hawaii Institute For Astronomy; Estados UnidosIOP Publishing2021-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/169535Ashall, C.; Lu, J.; Hsiao, E. Y.; Hoeflich, P.; Phillips, M. M.; et al.; Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae; IOP Publishing; Astrophysical Journal; 922; 2; 12-2021; 1-410004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ac19acinfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ac19acinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:36:28Zoai:ri.conicet.gov.ar:11336/169535instacron: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:34982025-10-15 15:36:28.423CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| title |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| spellingShingle |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae Ashall, C. SUPERNOVAE |
| title_short |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| title_full |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| title_fullStr |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| title_full_unstemmed |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| title_sort |
Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae |
| dc.creator.none.fl_str_mv |
Ashall, C. Lu, J. Hsiao, E. Y. Hoeflich, P. Phillips, M. M. Galbany, Lluís Burns, C. R. Contreras, C. Krisciunas, K. Morrell, Nidia Irene Stritzinger, M. D. Suntzeff, Nicholas B. Taddia, F. Anais, J. Baron, E. Brown, P. J. Busta, L. Campillay, A. Castellón, S. Corco, C. Davis, S. Folatelli, Gaston Förster, F. Freedman, W. L. Gonzaléz, C. Hamuy, M. Holmbo, S. Kirshner, R. P. Kumar, S. Marion, G. H. Mazzali, P. Morokuma, T. Nugent, P. E. Persson, S. E. Piro, A. L. Roth, M. Salgado, F. Sand, D.J. Seron, J. Shahbandeh, M. Shappee, B. J. |
| author |
Ashall, C. |
| author_facet |
Ashall, C. Lu, J. Hsiao, E. Y. Hoeflich, P. Phillips, M. M. Galbany, Lluís Burns, C. R. Contreras, C. Krisciunas, K. Morrell, Nidia Irene Stritzinger, M. D. Suntzeff, Nicholas B. Taddia, F. Anais, J. Baron, E. Brown, P. J. Busta, L. Campillay, A. Castellón, S. Corco, C. Davis, S. Folatelli, Gaston Förster, F. Freedman, W. L. Gonzaléz, C. Hamuy, M. Holmbo, S. Kirshner, R. P. Kumar, S. Marion, G. H. Mazzali, P. Morokuma, T. Nugent, P. E. Persson, S. E. Piro, A. L. Roth, M. Salgado, F. Sand, D.J. Seron, J. Shahbandeh, M. Shappee, B. J. |
| author_role |
author |
| author2 |
Lu, J. Hsiao, E. Y. Hoeflich, P. Phillips, M. M. Galbany, Lluís Burns, C. R. Contreras, C. Krisciunas, K. Morrell, Nidia Irene Stritzinger, M. D. Suntzeff, Nicholas B. Taddia, F. Anais, J. Baron, E. Brown, P. J. Busta, L. Campillay, A. Castellón, S. Corco, C. Davis, S. Folatelli, Gaston Förster, F. Freedman, W. L. Gonzaléz, C. Hamuy, M. Holmbo, S. Kirshner, R. P. Kumar, S. Marion, G. H. Mazzali, P. Morokuma, T. Nugent, P. E. Persson, S. E. Piro, A. L. Roth, M. Salgado, F. Sand, D.J. Seron, J. Shahbandeh, M. Shappee, B. J. |
| 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 author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
SUPERNOVAE |
| topic |
SUPERNOVAE |
| 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 a multiwavelength photometric and spectroscopic analysis of 13 super-Chandrasekhar-mass/2003fg-like Type Ia supernovae (SNe Ia). Nine of these objects were observed by the Carnegie Supernova Project. The 2003fg-like SNe have slowly declining light curves (Δm 15(B) < 1.3 mag), and peak absolute B-band magnitudes of -19 < M B < -21 mag. Many of the 2003fg-like SNe are located in the same part of the luminosity-width relation as normal SNe Ia. In the optical B and V bands, the 2003fg-like SNe look like normal SNe Ia, but at redder wavelengths they diverge. Unlike other luminous SNe Ia, the 2003fg-like SNe generally have only one i-band maximum, which peaks after the epoch of the B-band maximum, while their near-IR (NIR) light-curve rise times can be ⪆40 days longer than those of normal SNe Ia. They are also at least 1 mag brighter in the NIR bands than normal SNe Ia, peaking above M H = -19 mag, and generally have negative Hubble residuals, which may be the cause of some systematics in dark-energy experiments. Spectroscopically, the 2003fg-like SNe exhibit peculiarities such as unburnt carbon well past maximum light, a large spread (8000-12,000 km s-1) in Si ii λ6355 velocities at maximum light with no rapid early velocity decline, and no clear H-band break at +10 days. We find that SNe with a larger pseudo-equivalent width of C ii at maximum light have lower Si ii λ6355 velocities and more slowly declining light curves. There are also multiple factors that contribute to the peak luminosity of 2003fg-like SNe. The explosion of a C-O degenerate core inside a carbon-rich envelope is consistent with these observations. Such a configuration may come from the core-degenerate scenario. Fil: Ashall, C.. University Hawaii Institute For Astronomy; Estados Unidos Fil: Lu, J.. Florida State University; Estados Unidos Fil: Hsiao, E. Y.. Florida State University; Estados Unidos Fil: Hoeflich, P.. Florida State University; Estados Unidos Fil: Phillips, M. M.. Las Campanas Observatory; Chile Fil: Galbany, Lluís. Instituto de Ciencias del Espacio; España Fil: Burns, C. R.. Las Campanas Observatory; Chile Fil: Contreras, C.. Las Campanas Observatory; Chile Fil: Krisciunas, K.. Texas A&M University; Estados Unidos Fil: Morrell, Nidia Irene. Las Campanas Observatory; Chile Fil: Stritzinger, M. D.. University Aarhus; Dinamarca Fil: Suntzeff, Nicholas B.. Texas A&M University; Estados Unidos Fil: Taddia, F.. University Aarhus; Dinamarca Fil: Anais, J.. Las Campanas Observatory; Chile Fil: Baron, E.. Oklahoma State University; Estados Unidos. Universitat Hamburg; Alemania Fil: Brown, P. J.. Texas A&M University; Estados Unidos Fil: Busta, L.. Las Campanas Observatory; Chile Fil: Campillay, A.. Universidad de La Serena; Chile Fil: Castellón, S.. Las Campanas Observatory; Chile Fil: Corco, C.. Las Campanas Observatory; Chile. Soar Telescope; Chile Fil: Davis, S.. University of California at Davis; Estados Unidos Fil: Folatelli, Gaston. 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: Förster, F.. Universidad de Chile; Chile. Instituto Milenio de Astrofísica; Chile Fil: Freedman, W. L.. University of Chicago; Estados Unidos Fil: Gonzaléz, C.. Las Campanas Observatory; Chile Fil: Hamuy, M.. Universidad de Chile; Chile Fil: Holmbo, S.. University Aarhus; Dinamarca Fil: Kirshner, R. P.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Kumar, S.. Florida State University; Estados Unidos Fil: Marion, G. H.. University of Texas at Austin; Estados Unidos Fil: Mazzali, P.. Liverpool John Moores University; Reino Unido Fil: Morokuma, T.. The University Of Tokyo; Japón Fil: Nugent, P. E.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos Fil: Persson, S. E.. Las Campanas Observatory; Chile Fil: Piro, A. L.. Las Campanas Observatory; Chile Fil: Roth, M.. Las Campanas Observatory; Chile Fil: Salgado, F.. Las Campanas Observatory; Chile Fil: Sand, D.J.. University of Arizona; Estados Unidos Fil: Seron, J.. Las Campanas Observatory; Chile Fil: Shahbandeh, M.. Florida State University; Estados Unidos Fil: Shappee, B. J.. University Hawaii Institute For Astronomy; Estados Unidos |
| description |
We present a multiwavelength photometric and spectroscopic analysis of 13 super-Chandrasekhar-mass/2003fg-like Type Ia supernovae (SNe Ia). Nine of these objects were observed by the Carnegie Supernova Project. The 2003fg-like SNe have slowly declining light curves (Δm 15(B) < 1.3 mag), and peak absolute B-band magnitudes of -19 < M B < -21 mag. Many of the 2003fg-like SNe are located in the same part of the luminosity-width relation as normal SNe Ia. In the optical B and V bands, the 2003fg-like SNe look like normal SNe Ia, but at redder wavelengths they diverge. Unlike other luminous SNe Ia, the 2003fg-like SNe generally have only one i-band maximum, which peaks after the epoch of the B-band maximum, while their near-IR (NIR) light-curve rise times can be ⪆40 days longer than those of normal SNe Ia. They are also at least 1 mag brighter in the NIR bands than normal SNe Ia, peaking above M H = -19 mag, and generally have negative Hubble residuals, which may be the cause of some systematics in dark-energy experiments. Spectroscopically, the 2003fg-like SNe exhibit peculiarities such as unburnt carbon well past maximum light, a large spread (8000-12,000 km s-1) in Si ii λ6355 velocities at maximum light with no rapid early velocity decline, and no clear H-band break at +10 days. We find that SNe with a larger pseudo-equivalent width of C ii at maximum light have lower Si ii λ6355 velocities and more slowly declining light curves. There are also multiple factors that contribute to the peak luminosity of 2003fg-like SNe. The explosion of a C-O degenerate core inside a carbon-rich envelope is consistent with these observations. Such a configuration may come from the core-degenerate scenario. |
| publishDate |
2021 |
| dc.date.none.fl_str_mv |
2021-12 |
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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/11336/169535 Ashall, C.; Lu, J.; Hsiao, E. Y.; Hoeflich, P.; Phillips, M. M.; et al.; Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae; IOP Publishing; Astrophysical Journal; 922; 2; 12-2021; 1-41 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/169535 |
| identifier_str_mv |
Ashall, C.; Lu, J.; Hsiao, E. Y.; Hoeflich, P.; Phillips, M. M.; et al.; Carnegie Supernova Project: The First Homogeneous Sample of Super-Chandrasekhar-mass/2003fg-like Type Ia Supernovae; IOP Publishing; Astrophysical Journal; 922; 2; 12-2021; 1-41 0004-637X CONICET Digital CONICET |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ac19ac info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ac19ac |
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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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