SN 2011fu: a type IIb supernova with a luminous double-peaked light curve
- Autores
- Morales Garoffolo, A.; Elias Rosa, N.; Bersten, Melina Cecilia; Jerkstrand, A.; Taubenberger, S.; Benetti, S.; Cappellaro, E.; Kotak, R.; Pastorello, A.; Bufano, F.; Domínguez, R. M.; Ergon, M.; Fraser, M.; Gao, X.; García, E.; Howell, D. A.; Isern, J.; Smartt, S. J.; Tomasella, L.; Valenti, S.
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present optical and near-infrared observations of the type IIb supernova (SN) 2011fu from a few days to ∼300 d after explosion. The SN presents a double-peaked light curve (LC) similar to that of SN 1993J, although more luminous and with a longer cooling phase after the primary peak. The spectral evolution is also similar to SN 1993J’s, with hydrogen dominating the spectra to ∼40 d, then helium gaining strength, and nebular emission lines appearing from ∼60 d post-explosion. The velocities derived from the P-Cygni absorptions are overall similar to those of other type IIb SNe. We have found a strong similarity between the oxygen and magnesium line profiles at late times, which suggests that these lines are forming at the same location within the ejecta. The hydrodynamical modelling of the pseudo-bolometric LC and the observed photospheric velocities suggest that SN 2011fu was the explosion of an extended star (R ∼ 450 R☉), in which 1.3 × 1051 erg of kinetic energy were released and 0.15 M of 56Ni were synthesized. In addition, a better reproduction of the observed early pseudo-bolometric LC is achieved if a more massive H-rich envelope than for other type IIb SNe is considered (0.3 M☉). The hydrodynamical modelling of the LC and the comparison of our late-time spectra with nebular spectral models for type IIb SNe, point to a progenitor for SN 2011fu with a Zero Age Main Sequence (ZAMS) mass of 13–18 M☉.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Astronomía
supernovae: general
supernovae: individual: SN 2011fu - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/93907
Ver los metadatos del registro completo
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SN 2011fu: a type IIb supernova with a luminous double-peaked light curveMorales Garoffolo, A.Elias Rosa, N.Bersten, Melina CeciliaJerkstrand, A.Taubenberger, S.Benetti, S.Cappellaro, E.Kotak, R.Pastorello, A.Bufano, F.Domínguez, R. M.Ergon, M.Fraser, M.Gao, X.García, E.Howell, D. A.Isern, J.Smartt, S. J.Tomasella, L.Valenti, S.Astronomíasupernovae: generalsupernovae: individual: SN 2011fuWe present optical and near-infrared observations of the type IIb supernova (SN) 2011fu from a few days to ∼300 d after explosion. The SN presents a double-peaked light curve (LC) similar to that of SN 1993J, although more luminous and with a longer cooling phase after the primary peak. The spectral evolution is also similar to SN 1993J’s, with hydrogen dominating the spectra to ∼40 d, then helium gaining strength, and nebular emission lines appearing from ∼60 d post-explosion. The velocities derived from the P-Cygni absorptions are overall similar to those of other type IIb SNe. We have found a strong similarity between the oxygen and magnesium line profiles at late times, which suggests that these lines are forming at the same location within the ejecta. The hydrodynamical modelling of the pseudo-bolometric LC and the observed photospheric velocities suggest that SN 2011fu was the explosion of an extended star (R ∼ 450 R☉), in which 1.3 × 10<sup>51</sup> erg of kinetic energy were released and 0.15 M of <sup>56</sup>Ni were synthesized. In addition, a better reproduction of the observed early pseudo-bolometric LC is achieved if a more massive H-rich envelope than for other type IIb SNe is considered (0.3 M☉). The hydrodynamical modelling of the LC and the comparison of our late-time spectra with nebular spectral models for type IIb SNe, point to a progenitor for SN 2011fu with a Zero Age Main Sequence (ZAMS) mass of 13–18 M☉.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2015-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf95–114http://sedici.unlp.edu.ar/handle/10915/93907enginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/454/1/95/1132801/SN-2011fu-a-type-IIb-supernova-with-a-luminous?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/url/https://ri.conicet.gov.ar/handle/11336/13949info:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1972info:eu-repo/semantics/altIdentifier/hdl/11336/13949info: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:UNLP2025-09-03T10:51:42Zoai:sedici.unlp.edu.ar:10915/93907Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-03 10:51:42.605SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| title |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| spellingShingle |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve Morales Garoffolo, A. Astronomía supernovae: general supernovae: individual: SN 2011fu |
| title_short |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| title_full |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| title_fullStr |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| title_full_unstemmed |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| title_sort |
SN 2011fu: a type IIb supernova with a luminous double-peaked light curve |
| dc.creator.none.fl_str_mv |
Morales Garoffolo, A. Elias Rosa, N. Bersten, Melina Cecilia Jerkstrand, A. Taubenberger, S. Benetti, S. Cappellaro, E. Kotak, R. Pastorello, A. Bufano, F. Domínguez, R. M. Ergon, M. Fraser, M. Gao, X. García, E. Howell, D. A. Isern, J. Smartt, S. J. Tomasella, L. Valenti, S. |
| author |
Morales Garoffolo, A. |
| author_facet |
Morales Garoffolo, A. Elias Rosa, N. Bersten, Melina Cecilia Jerkstrand, A. Taubenberger, S. Benetti, S. Cappellaro, E. Kotak, R. Pastorello, A. Bufano, F. Domínguez, R. M. Ergon, M. Fraser, M. Gao, X. García, E. Howell, D. A. Isern, J. Smartt, S. J. Tomasella, L. Valenti, S. |
| author_role |
author |
| author2 |
Elias Rosa, N. Bersten, Melina Cecilia Jerkstrand, A. Taubenberger, S. Benetti, S. Cappellaro, E. Kotak, R. Pastorello, A. Bufano, F. Domínguez, R. M. Ergon, M. Fraser, M. Gao, X. García, E. Howell, D. A. Isern, J. Smartt, S. J. Tomasella, L. Valenti, S. |
| author2_role |
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 |
Astronomía supernovae: general supernovae: individual: SN 2011fu |
| topic |
Astronomía supernovae: general supernovae: individual: SN 2011fu |
| dc.description.none.fl_txt_mv |
We present optical and near-infrared observations of the type IIb supernova (SN) 2011fu from a few days to ∼300 d after explosion. The SN presents a double-peaked light curve (LC) similar to that of SN 1993J, although more luminous and with a longer cooling phase after the primary peak. The spectral evolution is also similar to SN 1993J’s, with hydrogen dominating the spectra to ∼40 d, then helium gaining strength, and nebular emission lines appearing from ∼60 d post-explosion. The velocities derived from the P-Cygni absorptions are overall similar to those of other type IIb SNe. We have found a strong similarity between the oxygen and magnesium line profiles at late times, which suggests that these lines are forming at the same location within the ejecta. The hydrodynamical modelling of the pseudo-bolometric LC and the observed photospheric velocities suggest that SN 2011fu was the explosion of an extended star (R ∼ 450 R☉), in which 1.3 × 10<sup>51</sup> erg of kinetic energy were released and 0.15 M of <sup>56</sup>Ni were synthesized. In addition, a better reproduction of the observed early pseudo-bolometric LC is achieved if a more massive H-rich envelope than for other type IIb SNe is considered (0.3 M☉). The hydrodynamical modelling of the LC and the comparison of our late-time spectra with nebular spectral models for type IIb SNe, point to a progenitor for SN 2011fu with a Zero Age Main Sequence (ZAMS) mass of 13–18 M☉. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
We present optical and near-infrared observations of the type IIb supernova (SN) 2011fu from a few days to ∼300 d after explosion. The SN presents a double-peaked light curve (LC) similar to that of SN 1993J, although more luminous and with a longer cooling phase after the primary peak. The spectral evolution is also similar to SN 1993J’s, with hydrogen dominating the spectra to ∼40 d, then helium gaining strength, and nebular emission lines appearing from ∼60 d post-explosion. The velocities derived from the P-Cygni absorptions are overall similar to those of other type IIb SNe. We have found a strong similarity between the oxygen and magnesium line profiles at late times, which suggests that these lines are forming at the same location within the ejecta. The hydrodynamical modelling of the pseudo-bolometric LC and the observed photospheric velocities suggest that SN 2011fu was the explosion of an extended star (R ∼ 450 R☉), in which 1.3 × 10<sup>51</sup> erg of kinetic energy were released and 0.15 M of <sup>56</sup>Ni were synthesized. In addition, a better reproduction of the observed early pseudo-bolometric LC is achieved if a more massive H-rich envelope than for other type IIb SNe is considered (0.3 M☉). The hydrodynamical modelling of the LC and the comparison of our late-time spectra with nebular spectral models for type IIb SNe, point to a progenitor for SN 2011fu with a Zero Age Main Sequence (ZAMS) mass of 13–18 M☉. |
| publishDate |
2015 |
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2015-11 |
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eng |
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eng |
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