The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object

Autores: Gutiérrez, C. P.; Bersten, Melina Cecilia; Orellana, Mariana Dominga; Pastorello, A.; Ertini, Keila Yael; Folatelli, Gaston; Pignata, G.; Anderson, J. P.; Smartt, S.; Sullivan, M.; Pursiainen, M.; Inserra, C.; Elias Rosa, N.; Fraser, M.; Kankare, E.; Moran, S.; Reguitti, A.; Reynolds, T. M.; Stritzinger, M.; Burke, J.; Frohmaier, C.; Galbany, Lluís; Hiramatsu, D.; Howell, D. A.; Kuncarayakti, H.; Mattila, S.; Müller Bravo, T.; Pellegrino, C.; Smith, M.
Año de publicación: 2021
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: We present the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first ∼100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in ∼8 d, while the r-band peak occurred ∼15 d post-explosion. A second and more prominent peak is reached in all bands at ∼45 d past explosion, followed by a fast decline from ∼60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si ii λ6355 and C ii λ6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M?, and an explosion energy of 3.5 × 1051 erg. The light-curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M?, and an internal component of 0.3 M? or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible.
Fil: Gutiérrez, C. P.. University of Southampton; Reino Unido
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
Fil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; Argentina
Fil: Pastorello, A.. Osservatorio Astronomico Di Padova; Italia
Fil: Ertini, Keila Yael. 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: 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: Pignata, G.. Universidad Andrés Bello; Chile
Fil: Anderson, J. P.. European Southern Observatory Chile; Chile
Fil: Smartt, S.. The Queens University of Belfast; Irlanda
Fil: Sullivan, M.. University of Southampton; Reino Unido
Fil: Pursiainen, M.. University of Southampton; Reino Unido
Fil: Inserra, C.. Cardiff University; Reino Unido
Fil: Elias Rosa, N.. Osservatorio Astronomico Di Padova; Italia
Fil: Fraser, M.. University College Dublin; Irlanda
Fil: Kankare, E.. University of Turku; Finlandia
Fil: Moran, S.. University of Turku; Finlandia
Fil: Reguitti, A.. Universidad Andrés Bello; Chile
Fil: Reynolds, T. M.. University of Turku; Finlandia
Fil: Stritzinger, M.. University Aarhus; Dinamarca
Fil: Burke, J.. University of California; Estados Unidos
Fil: Frohmaier, C.. University of Portsmouth; Estados Unidos
Fil: Galbany, Lluís. Universidad de Granada; España
Fil: Hiramatsu, D.. University of California; Estados Unidos
Fil: Howell, D. A.. University of California; Estados Unidos
Fil: Kuncarayakti, H.. University of Turku; Finlandia
Fil: Mattila, S.. University of Turku; Finlandia
Fil: Müller Bravo, T.. University of Southampton; Reino Unido
Fil: Pellegrino, C.. University of California; Estados Unidos
Fil: Smith, M.. Université de Lyon; Francia
Materia: SUPERNOVAE: GENERAL
SUPERNOVAE: INDIVIDUAL: SN 2019CAD
Nivel de accesibilidad: acceso abierto
Condiciones de uso: https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
Institución: Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador: oai:ri.conicet.gov.ar:11336/152461

Acceder

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network_acronym_str	CONICETDig
repository_id_str	3498
network_name_str	CONICET Digital (CONICET)
spelling	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like objectGutiérrez, C. P.Bersten, Melina CeciliaOrellana, Mariana DomingaPastorello, A.Ertini, Keila YaelFolatelli, GastonPignata, G.Anderson, J. P.Smartt, S.Sullivan, M.Pursiainen, M.Inserra, C.Elias Rosa, N.Fraser, M.Kankare, E.Moran, S.Reguitti, A.Reynolds, T. M.Stritzinger, M.Burke, J.Frohmaier, C.Galbany, LluísHiramatsu, D.Howell, D. A.Kuncarayakti, H.Mattila, S.Müller Bravo, T.Pellegrino, C.Smith, M.SUPERNOVAE: GENERALSUPERNOVAE: INDIVIDUAL: SN 2019CADhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first ∼100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in ∼8 d, while the r-band peak occurred ∼15 d post-explosion. A second and more prominent peak is reached in all bands at ∼45 d past explosion, followed by a fast decline from ∼60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si ii λ6355 and C ii λ6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M?, and an explosion energy of 3.5 × 1051 erg. The light-curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M?, and an internal component of 0.3 M? or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible.Fil: Gutiérrez, C. P.. University of Southampton; Reino UnidoFil: 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; ArgentinaFil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; ArgentinaFil: Pastorello, A.. Osservatorio Astronomico Di Padova; ItaliaFil: Ertini, Keila Yael. 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: 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: Pignata, G.. Universidad Andrés Bello; ChileFil: Anderson, J. P.. European Southern Observatory Chile; ChileFil: Smartt, S.. The Queens University of Belfast; IrlandaFil: Sullivan, M.. University of Southampton; Reino UnidoFil: Pursiainen, M.. University of Southampton; Reino UnidoFil: Inserra, C.. Cardiff University; Reino UnidoFil: Elias Rosa, N.. Osservatorio Astronomico Di Padova; ItaliaFil: Fraser, M.. University College Dublin; IrlandaFil: Kankare, E.. University of Turku; FinlandiaFil: Moran, S.. University of Turku; FinlandiaFil: Reguitti, A.. Universidad Andrés Bello; ChileFil: Reynolds, T. M.. University of Turku; FinlandiaFil: Stritzinger, M.. University Aarhus; DinamarcaFil: Burke, J.. University of California; Estados UnidosFil: Frohmaier, C.. University of Portsmouth; Estados UnidosFil: Galbany, Lluís. Universidad de Granada; EspañaFil: Hiramatsu, D.. University of California; Estados UnidosFil: Howell, D. A.. University of California; Estados UnidosFil: Kuncarayakti, H.. University of Turku; FinlandiaFil: Mattila, S.. University of Turku; FinlandiaFil: Müller Bravo, T.. University of Southampton; Reino UnidoFil: Pellegrino, C.. University of California; Estados UnidosFil: Smith, M.. Université de Lyon; FranciaWiley Blackwell Publishing, Inc2021-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/152461Gutiérrez, C. P.; Bersten, Melina Cecilia; Orellana, Mariana Dominga; Pastorello, A.; Ertini, Keila Yael; et al.; The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 504; 4; 7-2021; 4907-49220035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab1009info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/504/4/4907/6224870info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:48:35Zoai:ri.conicet.gov.ar:11336/152461instacron: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:34982025-09-03 09:48:36.089CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
title	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
spellingShingle	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object Gutiérrez, C. P. SUPERNOVAE: GENERAL SUPERNOVAE: INDIVIDUAL: SN 2019CAD
title_short	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
title_full	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
title_fullStr	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
title_full_unstemmed	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
title_sort	The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
dc.creator.none.fl_str_mv	Gutiérrez, C. P. Bersten, Melina Cecilia Orellana, Mariana Dominga Pastorello, A. Ertini, Keila Yael Folatelli, Gaston Pignata, G. Anderson, J. P. Smartt, S. Sullivan, M. Pursiainen, M. Inserra, C. Elias Rosa, N. Fraser, M. Kankare, E. Moran, S. Reguitti, A. Reynolds, T. M. Stritzinger, M. Burke, J. Frohmaier, C. Galbany, Lluís Hiramatsu, D. Howell, D. A. Kuncarayakti, H. Mattila, S. Müller Bravo, T. Pellegrino, C. Smith, M.
author	Gutiérrez, C. P.
author_facet	Gutiérrez, C. P. Bersten, Melina Cecilia Orellana, Mariana Dominga Pastorello, A. Ertini, Keila Yael Folatelli, Gaston Pignata, G. Anderson, J. P. Smartt, S. Sullivan, M. Pursiainen, M. Inserra, C. Elias Rosa, N. Fraser, M. Kankare, E. Moran, S. Reguitti, A. Reynolds, T. M. Stritzinger, M. Burke, J. Frohmaier, C. Galbany, Lluís Hiramatsu, D. Howell, D. A. Kuncarayakti, H. Mattila, S. Müller Bravo, T. Pellegrino, C. Smith, M.
author_role	author
author2	Bersten, Melina Cecilia Orellana, Mariana Dominga Pastorello, A. Ertini, Keila Yael Folatelli, Gaston Pignata, G. Anderson, J. P. Smartt, S. Sullivan, M. Pursiainen, M. Inserra, C. Elias Rosa, N. Fraser, M. Kankare, E. Moran, S. Reguitti, A. Reynolds, T. M. Stritzinger, M. Burke, J. Frohmaier, C. Galbany, Lluís Hiramatsu, D. Howell, D. A. Kuncarayakti, H. Mattila, S. Müller Bravo, T. Pellegrino, C. Smith, 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 author author author author
dc.subject.none.fl_str_mv	SUPERNOVAE: GENERAL SUPERNOVAE: INDIVIDUAL: SN 2019CAD
topic	SUPERNOVAE: GENERAL SUPERNOVAE: INDIVIDUAL: SN 2019CAD
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 the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first ∼100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in ∼8 d, while the r-band peak occurred ∼15 d post-explosion. A second and more prominent peak is reached in all bands at ∼45 d past explosion, followed by a fast decline from ∼60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si ii λ6355 and C ii λ6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M?, and an explosion energy of 3.5 × 1051 erg. The light-curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M?, and an internal component of 0.3 M? or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible. Fil: Gutiérrez, C. P.. University of Southampton; Reino Unido 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 Fil: Orellana, Mariana Dominga. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Río Negro; Argentina Fil: Pastorello, A.. Osservatorio Astronomico Di Padova; Italia Fil: Ertini, Keila Yael. 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: 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: Pignata, G.. Universidad Andrés Bello; Chile Fil: Anderson, J. P.. European Southern Observatory Chile; Chile Fil: Smartt, S.. The Queens University of Belfast; Irlanda Fil: Sullivan, M.. University of Southampton; Reino Unido Fil: Pursiainen, M.. University of Southampton; Reino Unido Fil: Inserra, C.. Cardiff University; Reino Unido Fil: Elias Rosa, N.. Osservatorio Astronomico Di Padova; Italia Fil: Fraser, M.. University College Dublin; Irlanda Fil: Kankare, E.. University of Turku; Finlandia Fil: Moran, S.. University of Turku; Finlandia Fil: Reguitti, A.. Universidad Andrés Bello; Chile Fil: Reynolds, T. M.. University of Turku; Finlandia Fil: Stritzinger, M.. University Aarhus; Dinamarca Fil: Burke, J.. University of California; Estados Unidos Fil: Frohmaier, C.. University of Portsmouth; Estados Unidos Fil: Galbany, Lluís. Universidad de Granada; España Fil: Hiramatsu, D.. University of California; Estados Unidos Fil: Howell, D. A.. University of California; Estados Unidos Fil: Kuncarayakti, H.. University of Turku; Finlandia Fil: Mattila, S.. University of Turku; Finlandia Fil: Müller Bravo, T.. University of Southampton; Reino Unido Fil: Pellegrino, C.. University of California; Estados Unidos Fil: Smith, M.. Université de Lyon; Francia
description	We present the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first ∼100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in ∼8 d, while the r-band peak occurred ∼15 d post-explosion. A second and more prominent peak is reached in all bands at ∼45 d past explosion, followed by a fast decline from ∼60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si ii λ6355 and C ii λ6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M?, and an explosion energy of 3.5 × 1051 erg. The light-curve morphology can be reproduced either by a double-peaked 56Ni distribution with an external component of 0.041 M?, and an internal component of 0.3 M? or a double-peaked 56Ni distribution plus magnetar model (P ∼11 ms and B ∼26 × 1014 G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the 56Ni model would require extreme values, while the magnetar model would still be feasible.
publishDate	2021
dc.date.none.fl_str_mv	2021-07
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
format	article
status_str	publishedVersion
dc.identifier.none.fl_str_mv	http://hdl.handle.net/11336/152461 Gutiérrez, C. P.; Bersten, Melina Cecilia; Orellana, Mariana Dominga; Pastorello, A.; Ertini, Keila Yael; et al.; The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 504; 4; 7-2021; 4907-4922 0035-8711 CONICET Digital CONICET
url	http://hdl.handle.net/11336/152461
identifier_str_mv	Gutiérrez, C. P.; Bersten, Melina Cecilia; Orellana, Mariana Dominga; Pastorello, A.; Ertini, Keila Yael; et al.; The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 504; 4; 7-2021; 4907-4922 0035-8711 CONICET Digital CONICET
dc.language.none.fl_str_mv	eng
language	eng
dc.relation.none.fl_str_mv	info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab1009 info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/504/4/4907/6224870
dc.rights.none.fl_str_mv	info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv	openAccess
rights_invalid_str_mv	https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv	application/pdf application/pdf
dc.publisher.none.fl_str_mv	Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv	Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv	reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str	CONICET Digital (CONICET)
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instname_str	Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv	CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv	dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object

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