The fast rise of the unusual type IIL/IIb SN 2018ivc
- Autores
- Reguitti, A.; Dastidar, R.; Pignata, G.; Maeda, K.; Moriya, T. J.; Kuncarayakti, H.; Rodríguez, Ó.; Bersten, Melina Cecilia; Anderson, J. P.; Charalampopoulos, P.; Fraser, M.; Gromadzki, M.; Young, D. R.; Benetti, S.; Cai, Y.-Z.; Elias Rosa, N.; Lundqvist, P.; Carini, R.; Cosentino, S. P.; Galbany, L.; González Bañuelos, M.; Gutiérrez, C. P.; Kopsacheili, M.; Pineda García, J. A.; Ramirez, M.
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present an analysis of the photometric and spectroscopic dataset of the type II supernova (SN) 2018ivc in the nearby (10 Mpc) galaxy Messier 77. Thanks to our high-cadence data, we observed the SN rising very rapidly by nearly three magnitudes in five hours (or 18 mag d‑1). The r-band light curve presents four distinct phases: the maximum light, which was reached in just one day, followed by a first, rapid linear decline and a short-duration plateau. Finally, the long, slower linear decline lasted for one year. Thanks to the ensuing radio re-brightening, we were able to detect SN 2018ivc four years after the explosion. The early spectra show a blue, nearly featureless continuum, but the spectra go on to evolve rapidly; after about ten days, a prominent Hα line starts to emerge, characterised by a peculiar profile. However, the spectra are heavily contaminated by emission lines from the host galaxy. The He I lines, namely λλ5876,7065, are also strong. In addition, strong absorption from the Na I doublet is evident and indicative of a non-negligible internal reddening. From its equivalent width, we derived a lower limit on the host reddening of AV ≃ 1.5 mag. From the Balmer decrement and a match of the B ‑ V colour curve of SN 2018ivc to that of the comparison objects, we obtained a host reddening of AV ≃ 3.0 mag. The spectra are similar to those of SNe II, but with strong He lines. Given the peculiar light curve and spectral features, we suggest SN 2018ivc could be a transitional object between the type IIL and type IIb SNe classes. In addition, we found signs of an interaction with the circum-stellar medium (CSM) in the light curve, also making SN 2018ivc an interacting event. Finally, we modelled the early multi-band light curves and photospheric velocity of SN 2018ivc to estimate the physical parameters of the explosion and CSM.
Fil: Reguitti, A.. Istituto Nazionale di Astrofisica; Italia
Fil: Dastidar, R.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics; Chile
Fil: Pignata, G.. Universidad de Tarapacá; Chile
Fil: Maeda, K.. Kyoto University; Japón
Fil: Moriya, T. J.. The Graduate University for Advanced Studies; Japón. Monash University; Australia
Fil: Kuncarayakti, H.. University of Turku; Finlandia
Fil: Rodríguez, Ó.. Millennium Institute of Astrophysics; Chile
Fil: Bersten, Melina Cecilia. 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. University of Tokyo; Japón
Fil: Anderson, J. P.. Millennium Institute of Astrophysics; Chile. European Southern Observatory; Chile
Fil: Charalampopoulos, P.. University of Turku; Finlandia
Fil: Fraser, M.. University College Dublin; Irlanda
Fil: Gromadzki, M.. Uniwersytet Warszawski; Argentina
Fil: Young, D. R.. The Queens University of Belfast; Irlanda
Fil: Benetti, S.. Istituto Nazionale di Astrofisica; Italia
Fil: Cai, Y.-Z.. Chinese Academy of Sciences; República de China. Yunnan Key Laboratory; China
Fil: Elias Rosa, N.. Istituto Nazionale di Astrofisica; Italia. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España
Fil: Lundqvist, P.. Stockholms Universitet; Suecia
Fil: Carini, R.. Istituto Nazionale di Astrofisica; Italia
Fil: Cosentino, S. P.. Università degli Studi di Catania; Italia. Istituto Nazionale di Astrofisica; Italia
Fil: Galbany, L.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; España
Fil: González Bañuelos, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; España
Fil: Gutiérrez, C. P.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; España
Fil: Kopsacheili, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; España
Fil: Pineda García, J. A.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; Chile
Fil: Ramirez, M.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; Chile - Materia
-
SUPERNOVAE
TRANSIENT
STELLAR EVOLUTION - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/257177
Ver los metadatos del registro completo
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The fast rise of the unusual type IIL/IIb SN 2018ivcReguitti, A.Dastidar, R.Pignata, G.Maeda, K.Moriya, T. J.Kuncarayakti, H.Rodríguez, Ó.Bersten, Melina CeciliaAnderson, J. P.Charalampopoulos, P.Fraser, M.Gromadzki, M.Young, D. R.Benetti, S.Cai, Y.-Z.Elias Rosa, N.Lundqvist, P.Carini, R.Cosentino, S. P.Galbany, L.González Bañuelos, M.Gutiérrez, C. P.Kopsacheili, M.Pineda García, J. A.Ramirez, M.SUPERNOVAETRANSIENTSTELLAR EVOLUTIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present an analysis of the photometric and spectroscopic dataset of the type II supernova (SN) 2018ivc in the nearby (10 Mpc) galaxy Messier 77. Thanks to our high-cadence data, we observed the SN rising very rapidly by nearly three magnitudes in five hours (or 18 mag d‑1). The r-band light curve presents four distinct phases: the maximum light, which was reached in just one day, followed by a first, rapid linear decline and a short-duration plateau. Finally, the long, slower linear decline lasted for one year. Thanks to the ensuing radio re-brightening, we were able to detect SN 2018ivc four years after the explosion. The early spectra show a blue, nearly featureless continuum, but the spectra go on to evolve rapidly; after about ten days, a prominent Hα line starts to emerge, characterised by a peculiar profile. However, the spectra are heavily contaminated by emission lines from the host galaxy. The He I lines, namely λλ5876,7065, are also strong. In addition, strong absorption from the Na I doublet is evident and indicative of a non-negligible internal reddening. From its equivalent width, we derived a lower limit on the host reddening of AV ≃ 1.5 mag. From the Balmer decrement and a match of the B ‑ V colour curve of SN 2018ivc to that of the comparison objects, we obtained a host reddening of AV ≃ 3.0 mag. The spectra are similar to those of SNe II, but with strong He lines. Given the peculiar light curve and spectral features, we suggest SN 2018ivc could be a transitional object between the type IIL and type IIb SNe classes. In addition, we found signs of an interaction with the circum-stellar medium (CSM) in the light curve, also making SN 2018ivc an interacting event. Finally, we modelled the early multi-band light curves and photospheric velocity of SN 2018ivc to estimate the physical parameters of the explosion and CSM.Fil: Reguitti, A.. Istituto Nazionale di Astrofisica; ItaliaFil: Dastidar, R.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics; ChileFil: Pignata, G.. Universidad de Tarapacá; ChileFil: Maeda, K.. Kyoto University; JapónFil: Moriya, T. J.. The Graduate University for Advanced Studies; Japón. Monash University; AustraliaFil: Kuncarayakti, H.. University of Turku; FinlandiaFil: Rodríguez, Ó.. Millennium Institute of Astrophysics; ChileFil: Bersten, Melina Cecilia. 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. University of Tokyo; JapónFil: Anderson, J. P.. Millennium Institute of Astrophysics; Chile. European Southern Observatory; ChileFil: Charalampopoulos, P.. University of Turku; FinlandiaFil: Fraser, M.. University College Dublin; IrlandaFil: Gromadzki, M.. Uniwersytet Warszawski; ArgentinaFil: Young, D. R.. The Queens University of Belfast; IrlandaFil: Benetti, S.. Istituto Nazionale di Astrofisica; ItaliaFil: Cai, Y.-Z.. Chinese Academy of Sciences; República de China. Yunnan Key Laboratory; ChinaFil: Elias Rosa, N.. Istituto Nazionale di Astrofisica; Italia. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; EspañaFil: Lundqvist, P.. Stockholms Universitet; SueciaFil: Carini, R.. Istituto Nazionale di Astrofisica; ItaliaFil: Cosentino, S. P.. Università degli Studi di Catania; Italia. Istituto Nazionale di Astrofisica; ItaliaFil: Galbany, L.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; EspañaFil: González Bañuelos, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; EspañaFil: Gutiérrez, C. P.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; EspañaFil: Kopsacheili, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; EspañaFil: Pineda García, J. A.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; ChileFil: Ramirez, M.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; ChileEDP Sciences2024-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/257177Reguitti, A.; Dastidar, R.; Pignata, G.; Maeda, K.; Moriya, T. J.; et al.; The fast rise of the unusual type IIL/IIb SN 2018ivc; EDP Sciences; Astronomy and Astrophysics; 692; 11-2024; 1-200004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202450805info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202450805info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:15:24Zoai:ri.conicet.gov.ar:11336/257177instacron: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 10:15:24.474CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| title |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| spellingShingle |
The fast rise of the unusual type IIL/IIb SN 2018ivc Reguitti, A. SUPERNOVAE TRANSIENT STELLAR EVOLUTION |
| title_short |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| title_full |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| title_fullStr |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| title_full_unstemmed |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| title_sort |
The fast rise of the unusual type IIL/IIb SN 2018ivc |
| dc.creator.none.fl_str_mv |
Reguitti, A. Dastidar, R. Pignata, G. Maeda, K. Moriya, T. J. Kuncarayakti, H. Rodríguez, Ó. Bersten, Melina Cecilia Anderson, J. P. Charalampopoulos, P. Fraser, M. Gromadzki, M. Young, D. R. Benetti, S. Cai, Y.-Z. Elias Rosa, N. Lundqvist, P. Carini, R. Cosentino, S. P. Galbany, L. González Bañuelos, M. Gutiérrez, C. P. Kopsacheili, M. Pineda García, J. A. Ramirez, M. |
| author |
Reguitti, A. |
| author_facet |
Reguitti, A. Dastidar, R. Pignata, G. Maeda, K. Moriya, T. J. Kuncarayakti, H. Rodríguez, Ó. Bersten, Melina Cecilia Anderson, J. P. Charalampopoulos, P. Fraser, M. Gromadzki, M. Young, D. R. Benetti, S. Cai, Y.-Z. Elias Rosa, N. Lundqvist, P. Carini, R. Cosentino, S. P. Galbany, L. González Bañuelos, M. Gutiérrez, C. P. Kopsacheili, M. Pineda García, J. A. Ramirez, M. |
| author_role |
author |
| author2 |
Dastidar, R. Pignata, G. Maeda, K. Moriya, T. J. Kuncarayakti, H. Rodríguez, Ó. Bersten, Melina Cecilia Anderson, J. P. Charalampopoulos, P. Fraser, M. Gromadzki, M. Young, D. R. Benetti, S. Cai, Y.-Z. Elias Rosa, N. Lundqvist, P. Carini, R. Cosentino, S. P. Galbany, L. González Bañuelos, M. Gutiérrez, C. P. Kopsacheili, M. Pineda García, J. A. Ramirez, M. |
| 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 |
| dc.subject.none.fl_str_mv |
SUPERNOVAE TRANSIENT STELLAR EVOLUTION |
| topic |
SUPERNOVAE TRANSIENT STELLAR EVOLUTION |
| 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 an analysis of the photometric and spectroscopic dataset of the type II supernova (SN) 2018ivc in the nearby (10 Mpc) galaxy Messier 77. Thanks to our high-cadence data, we observed the SN rising very rapidly by nearly three magnitudes in five hours (or 18 mag d‑1). The r-band light curve presents four distinct phases: the maximum light, which was reached in just one day, followed by a first, rapid linear decline and a short-duration plateau. Finally, the long, slower linear decline lasted for one year. Thanks to the ensuing radio re-brightening, we were able to detect SN 2018ivc four years after the explosion. The early spectra show a blue, nearly featureless continuum, but the spectra go on to evolve rapidly; after about ten days, a prominent Hα line starts to emerge, characterised by a peculiar profile. However, the spectra are heavily contaminated by emission lines from the host galaxy. The He I lines, namely λλ5876,7065, are also strong. In addition, strong absorption from the Na I doublet is evident and indicative of a non-negligible internal reddening. From its equivalent width, we derived a lower limit on the host reddening of AV ≃ 1.5 mag. From the Balmer decrement and a match of the B ‑ V colour curve of SN 2018ivc to that of the comparison objects, we obtained a host reddening of AV ≃ 3.0 mag. The spectra are similar to those of SNe II, but with strong He lines. Given the peculiar light curve and spectral features, we suggest SN 2018ivc could be a transitional object between the type IIL and type IIb SNe classes. In addition, we found signs of an interaction with the circum-stellar medium (CSM) in the light curve, also making SN 2018ivc an interacting event. Finally, we modelled the early multi-band light curves and photospheric velocity of SN 2018ivc to estimate the physical parameters of the explosion and CSM. Fil: Reguitti, A.. Istituto Nazionale di Astrofisica; Italia Fil: Dastidar, R.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics; Chile Fil: Pignata, G.. Universidad de Tarapacá; Chile Fil: Maeda, K.. Kyoto University; Japón Fil: Moriya, T. J.. The Graduate University for Advanced Studies; Japón. Monash University; Australia Fil: Kuncarayakti, H.. University of Turku; Finlandia Fil: Rodríguez, Ó.. Millennium Institute of Astrophysics; Chile Fil: Bersten, Melina Cecilia. 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. University of Tokyo; Japón Fil: Anderson, J. P.. Millennium Institute of Astrophysics; Chile. European Southern Observatory; Chile Fil: Charalampopoulos, P.. University of Turku; Finlandia Fil: Fraser, M.. University College Dublin; Irlanda Fil: Gromadzki, M.. Uniwersytet Warszawski; Argentina Fil: Young, D. R.. The Queens University of Belfast; Irlanda Fil: Benetti, S.. Istituto Nazionale di Astrofisica; Italia Fil: Cai, Y.-Z.. Chinese Academy of Sciences; República de China. Yunnan Key Laboratory; China Fil: Elias Rosa, N.. Istituto Nazionale di Astrofisica; Italia. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España Fil: Lundqvist, P.. Stockholms Universitet; Suecia Fil: Carini, R.. Istituto Nazionale di Astrofisica; Italia Fil: Cosentino, S. P.. Università degli Studi di Catania; Italia. Istituto Nazionale di Astrofisica; Italia Fil: Galbany, L.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; España Fil: González Bañuelos, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; España Fil: Gutiérrez, C. P.. Consejo Superior de Investigaciones Científicas; España. Instituto de Ciencias del Espacio; España. Institut d’Estudis Espacials de Catalunya; España Fil: Kopsacheili, M.. Consejo Superior de Investigaciones Científicas; España. Institut d’Estudis Espacials de Catalunya; España Fil: Pineda García, J. A.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; Chile Fil: Ramirez, M.. Universidad Andrés Bello; Chile. Millennium Institute of Astrophysics ; Chile |
| description |
We present an analysis of the photometric and spectroscopic dataset of the type II supernova (SN) 2018ivc in the nearby (10 Mpc) galaxy Messier 77. Thanks to our high-cadence data, we observed the SN rising very rapidly by nearly three magnitudes in five hours (or 18 mag d‑1). The r-band light curve presents four distinct phases: the maximum light, which was reached in just one day, followed by a first, rapid linear decline and a short-duration plateau. Finally, the long, slower linear decline lasted for one year. Thanks to the ensuing radio re-brightening, we were able to detect SN 2018ivc four years after the explosion. The early spectra show a blue, nearly featureless continuum, but the spectra go on to evolve rapidly; after about ten days, a prominent Hα line starts to emerge, characterised by a peculiar profile. However, the spectra are heavily contaminated by emission lines from the host galaxy. The He I lines, namely λλ5876,7065, are also strong. In addition, strong absorption from the Na I doublet is evident and indicative of a non-negligible internal reddening. From its equivalent width, we derived a lower limit on the host reddening of AV ≃ 1.5 mag. From the Balmer decrement and a match of the B ‑ V colour curve of SN 2018ivc to that of the comparison objects, we obtained a host reddening of AV ≃ 3.0 mag. The spectra are similar to those of SNe II, but with strong He lines. Given the peculiar light curve and spectral features, we suggest SN 2018ivc could be a transitional object between the type IIL and type IIb SNe classes. In addition, we found signs of an interaction with the circum-stellar medium (CSM) in the light curve, also making SN 2018ivc an interacting event. Finally, we modelled the early multi-band light curves and photospheric velocity of SN 2018ivc to estimate the physical parameters of the explosion and CSM. |
| publishDate |
2024 |
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2024-11 |
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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/11336/257177 Reguitti, A.; Dastidar, R.; Pignata, G.; Maeda, K.; Moriya, T. J.; et al.; The fast rise of the unusual type IIL/IIb SN 2018ivc; EDP Sciences; Astronomy and Astrophysics; 692; 11-2024; 1-20 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/257177 |
| identifier_str_mv |
Reguitti, A.; Dastidar, R.; Pignata, G.; Maeda, K.; Moriya, T. J.; et al.; The fast rise of the unusual type IIL/IIb SN 2018ivc; EDP Sciences; Astronomy and Astrophysics; 692; 11-2024; 1-20 0004-6361 CONICET Digital CONICET |
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eng |
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eng |
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