Broad-emission-line dominated hydrogen-rich luminous supernovae
- Autores
- Pessi, Priscila Jael; Anderson, J. P.; Folatelli, Gaston; Dessart, L.; González Gaitán, S.; Möller, A.; Gutiérrez, C. P.; Mattila, S.; Reynolds, T. M.; Charalampopoulos, P.; Filippenko, A.V.; Galbany, Lluís; Gal Yam, A.; Gromadzki, M.; Hiramatsu, D.; Howell, D. A.; Inserra, C.; Kankare, E.; Lunnan, R.; Martinez, Laureano; McCully, C.; Meza, N.; Müller Bravo, T. E.; Nicholl, M.; Pellegrino, C.; Pignata, G.; Sollerman, J.; Tucker, B. E.; Wang, X.; Young, D. R.
- Año de publicación
- 2023
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Hydrogen-rich Type II supernovae (SNe II) are the most frequently observed class of core-collapse SNe (CCSNe). However, most studies that analyse large samples of SNe II lack events with absolute peak magnitudes brighter than −18.5 mag at rest-frame optical wavelengths. Thanks to modern surveys, the detected number of such luminous SNe II (LSNe II) is growing. There exist several mechanisms that could produce luminous SNe II. The most popular propose either the presence of a central engine (a magnetar gradually spinning down or a black hole accreting fallback material) or the interaction of supernova ejecta with circumstellar material (CSM) that turns kinetic energy into radiation energy. In this work, we study the light curves and spectral series of a small sample of six LSNe II that show peculiarities in their H α profile, to attempt to understand the underlying powering mechanism. We favour an interaction scenario with CSM that is not dense enough to be optically thick to electron scattering on large scales – thus, no narrow emission lines are observed. This conclusion is based on the observed light curve (higher luminosity, fast decline, blue colours) and spectral features (lack of persistent narrow lines, broad H α emission, lack of H α absorption, weak, or non-existent metal lines) together with comparison to other luminous events available in the literature. We add to the growing evidence that transients powered by ejecta–CSM interaction do not necessarily display persistent narrow emission lines.
Fil: Pessi, Priscila Jael. Universidad Nacional de La Plata; Argentina. European Southern Observatory Chile; Chile
Fil: Anderson, J. P.. Instituto Milenio de Astrofísica; Chile. European Southern Observatory Chile; Chile
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: Dessart, L.. Institut D'astrophysique de Paris; Francia
Fil: González Gaitán, S.. Instituto Superior Tecnico; Portugal
Fil: Möller, A.. Swinburne University Of Technology; Australia
Fil: Gutiérrez, C. P.. University of Turku; Finlandia
Fil: Mattila, S.. University of Turku; Finlandia
Fil: Reynolds, T. M.. University of Turku; Finlandia
Fil: Charalampopoulos, P.. University of Turku; Finlandia
Fil: Filippenko, A.V.. University of California at Berkeley; Estados Unidos
Fil: Galbany, Lluís. Instituto de Ciencias del Espacio; España
Fil: Gal Yam, A.. Weizmann Institute Of Science Israel; Israel
Fil: Gromadzki, M.. University of Warsaw; Polonia
Fil: Hiramatsu, D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Howell, D. A.. University of California; Estados Unidos
Fil: Inserra, C.. Cardiff University; Reino Unido
Fil: Kankare, E.. University of Turku; Finlandia
Fil: Lunnan, R.. Stockholm Universit; Suecia
Fil: Martinez, Laureano. Universidad Nacional de Río Negro. Sede Andina; 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: McCully, C.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Meza, N.. University of California at Davis; Estados Unidos
Fil: Müller Bravo, T. E.. Instituto de Ciencias del Espacio; España
Fil: Nicholl, M.. The Queens University of Belfast; Irlanda
Fil: Pellegrino, C.. University of California; Estados Unidos
Fil: Pignata, G.. Universidad Andrés Bello; Chile
Fil: Sollerman, J.. Stockholm University; Suecia
Fil: Tucker, B. E.. Australian National University; Australia
Fil: Wang, X.. Beijing Academy of Science and Technology; China
Fil: Young, D. R.. The Queens University of Belfast; Irlanda - Materia
-
SN 2017GPP
SN 2017HBJ
SN 2017HXZ
SN 2018AQL
SN 2018EPH)
TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFO - 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:11336/234197
Ver los metadatos del registro completo
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Broad-emission-line dominated hydrogen-rich luminous supernovaePessi, Priscila JaelAnderson, J. P.Folatelli, GastonDessart, L.González Gaitán, S.Möller, A.Gutiérrez, C. P.Mattila, S.Reynolds, T. M.Charalampopoulos, P.Filippenko, A.V.Galbany, LluísGal Yam, A.Gromadzki, M.Hiramatsu, D.Howell, D. A.Inserra, C.Kankare, E.Lunnan, R.Martinez, LaureanoMcCully, C.Meza, N.Müller Bravo, T. E.Nicholl, M.Pellegrino, C.Pignata, G.Sollerman, J.Tucker, B. E.Wang, X.Young, D. R.SN 2017GPPSN 2017HBJSN 2017HXZSN 2018AQLSN 2018EPH)TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFOhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Hydrogen-rich Type II supernovae (SNe II) are the most frequently observed class of core-collapse SNe (CCSNe). However, most studies that analyse large samples of SNe II lack events with absolute peak magnitudes brighter than −18.5 mag at rest-frame optical wavelengths. Thanks to modern surveys, the detected number of such luminous SNe II (LSNe II) is growing. There exist several mechanisms that could produce luminous SNe II. The most popular propose either the presence of a central engine (a magnetar gradually spinning down or a black hole accreting fallback material) or the interaction of supernova ejecta with circumstellar material (CSM) that turns kinetic energy into radiation energy. In this work, we study the light curves and spectral series of a small sample of six LSNe II that show peculiarities in their H α profile, to attempt to understand the underlying powering mechanism. We favour an interaction scenario with CSM that is not dense enough to be optically thick to electron scattering on large scales – thus, no narrow emission lines are observed. This conclusion is based on the observed light curve (higher luminosity, fast decline, blue colours) and spectral features (lack of persistent narrow lines, broad H α emission, lack of H α absorption, weak, or non-existent metal lines) together with comparison to other luminous events available in the literature. We add to the growing evidence that transients powered by ejecta–CSM interaction do not necessarily display persistent narrow emission lines.Fil: Pessi, Priscila Jael. Universidad Nacional de La Plata; Argentina. European Southern Observatory Chile; ChileFil: Anderson, J. P.. Instituto Milenio de Astrofísica; Chile. European Southern Observatory Chile; ChileFil: 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: Dessart, L.. Institut D'astrophysique de Paris; FranciaFil: González Gaitán, S.. Instituto Superior Tecnico; PortugalFil: Möller, A.. Swinburne University Of Technology; AustraliaFil: Gutiérrez, C. P.. University of Turku; FinlandiaFil: Mattila, S.. University of Turku; FinlandiaFil: Reynolds, T. M.. University of Turku; FinlandiaFil: Charalampopoulos, P.. University of Turku; FinlandiaFil: Filippenko, A.V.. University of California at Berkeley; Estados UnidosFil: Galbany, Lluís. Instituto de Ciencias del Espacio; EspañaFil: Gal Yam, A.. Weizmann Institute Of Science Israel; IsraelFil: Gromadzki, M.. University of Warsaw; PoloniaFil: Hiramatsu, D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Howell, D. A.. University of California; Estados UnidosFil: Inserra, C.. Cardiff University; Reino UnidoFil: Kankare, E.. University of Turku; FinlandiaFil: Lunnan, R.. Stockholm Universit; SueciaFil: Martinez, Laureano. Universidad Nacional de Río Negro. Sede Andina; 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: McCully, C.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Meza, N.. University of California at Davis; Estados UnidosFil: Müller Bravo, T. E.. Instituto de Ciencias del Espacio; EspañaFil: Nicholl, M.. The Queens University of Belfast; IrlandaFil: Pellegrino, C.. University of California; Estados UnidosFil: Pignata, G.. Universidad Andrés Bello; ChileFil: Sollerman, J.. Stockholm University; SueciaFil: Tucker, B. E.. Australian National University; AustraliaFil: Wang, X.. Beijing Academy of Science and Technology; ChinaFil: Young, D. R.. The Queens University of Belfast; IrlandaWiley Blackwell Publishing, Inc2023-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/234197Pessi, Priscila Jael; Anderson, J. P.; Folatelli, Gaston; Dessart, L.; González Gaitán, S.; et al.; Broad-emission-line dominated hydrogen-rich luminous supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 523; 4; 8-2023; 5315-53400035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad1822info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/523/4/5315/7199790info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:01:52Zoai:ri.conicet.gov.ar:11336/234197instacron: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 10:01:52.896CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| title |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| spellingShingle |
Broad-emission-line dominated hydrogen-rich luminous supernovae Pessi, Priscila Jael SN 2017GPP SN 2017HBJ SN 2017HXZ SN 2018AQL SN 2018EPH) TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFO |
| title_short |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| title_full |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| title_fullStr |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| title_full_unstemmed |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| title_sort |
Broad-emission-line dominated hydrogen-rich luminous supernovae |
| dc.creator.none.fl_str_mv |
Pessi, Priscila Jael Anderson, J. P. Folatelli, Gaston Dessart, L. González Gaitán, S. Möller, A. Gutiérrez, C. P. Mattila, S. Reynolds, T. M. Charalampopoulos, P. Filippenko, A.V. Galbany, Lluís Gal Yam, A. Gromadzki, M. Hiramatsu, D. Howell, D. A. Inserra, C. Kankare, E. Lunnan, R. Martinez, Laureano McCully, C. Meza, N. Müller Bravo, T. E. Nicholl, M. Pellegrino, C. Pignata, G. Sollerman, J. Tucker, B. E. Wang, X. Young, D. R. |
| author |
Pessi, Priscila Jael |
| author_facet |
Pessi, Priscila Jael Anderson, J. P. Folatelli, Gaston Dessart, L. González Gaitán, S. Möller, A. Gutiérrez, C. P. Mattila, S. Reynolds, T. M. Charalampopoulos, P. Filippenko, A.V. Galbany, Lluís Gal Yam, A. Gromadzki, M. Hiramatsu, D. Howell, D. A. Inserra, C. Kankare, E. Lunnan, R. Martinez, Laureano McCully, C. Meza, N. Müller Bravo, T. E. Nicholl, M. Pellegrino, C. Pignata, G. Sollerman, J. Tucker, B. E. Wang, X. Young, D. R. |
| author_role |
author |
| author2 |
Anderson, J. P. Folatelli, Gaston Dessart, L. González Gaitán, S. Möller, A. Gutiérrez, C. P. Mattila, S. Reynolds, T. M. Charalampopoulos, P. Filippenko, A.V. Galbany, Lluís Gal Yam, A. Gromadzki, M. Hiramatsu, D. Howell, D. A. Inserra, C. Kankare, E. Lunnan, R. Martinez, Laureano McCully, C. Meza, N. Müller Bravo, T. E. Nicholl, M. Pellegrino, C. Pignata, G. Sollerman, J. Tucker, B. E. Wang, X. Young, D. R. |
| 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 |
| dc.subject.none.fl_str_mv |
SN 2017GPP SN 2017HBJ SN 2017HXZ SN 2018AQL SN 2018EPH) TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFO |
| topic |
SN 2017GPP SN 2017HBJ SN 2017HXZ SN 2018AQL SN 2018EPH) TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFO |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Hydrogen-rich Type II supernovae (SNe II) are the most frequently observed class of core-collapse SNe (CCSNe). However, most studies that analyse large samples of SNe II lack events with absolute peak magnitudes brighter than −18.5 mag at rest-frame optical wavelengths. Thanks to modern surveys, the detected number of such luminous SNe II (LSNe II) is growing. There exist several mechanisms that could produce luminous SNe II. The most popular propose either the presence of a central engine (a magnetar gradually spinning down or a black hole accreting fallback material) or the interaction of supernova ejecta with circumstellar material (CSM) that turns kinetic energy into radiation energy. In this work, we study the light curves and spectral series of a small sample of six LSNe II that show peculiarities in their H α profile, to attempt to understand the underlying powering mechanism. We favour an interaction scenario with CSM that is not dense enough to be optically thick to electron scattering on large scales – thus, no narrow emission lines are observed. This conclusion is based on the observed light curve (higher luminosity, fast decline, blue colours) and spectral features (lack of persistent narrow lines, broad H α emission, lack of H α absorption, weak, or non-existent metal lines) together with comparison to other luminous events available in the literature. We add to the growing evidence that transients powered by ejecta–CSM interaction do not necessarily display persistent narrow emission lines. Fil: Pessi, Priscila Jael. Universidad Nacional de La Plata; Argentina. European Southern Observatory Chile; Chile Fil: Anderson, J. P.. Instituto Milenio de Astrofísica; Chile. European Southern Observatory Chile; Chile 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: Dessart, L.. Institut D'astrophysique de Paris; Francia Fil: González Gaitán, S.. Instituto Superior Tecnico; Portugal Fil: Möller, A.. Swinburne University Of Technology; Australia Fil: Gutiérrez, C. P.. University of Turku; Finlandia Fil: Mattila, S.. University of Turku; Finlandia Fil: Reynolds, T. M.. University of Turku; Finlandia Fil: Charalampopoulos, P.. University of Turku; Finlandia Fil: Filippenko, A.V.. University of California at Berkeley; Estados Unidos Fil: Galbany, Lluís. Instituto de Ciencias del Espacio; España Fil: Gal Yam, A.. Weizmann Institute Of Science Israel; Israel Fil: Gromadzki, M.. University of Warsaw; Polonia Fil: Hiramatsu, D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Howell, D. A.. University of California; Estados Unidos Fil: Inserra, C.. Cardiff University; Reino Unido Fil: Kankare, E.. University of Turku; Finlandia Fil: Lunnan, R.. Stockholm Universit; Suecia Fil: Martinez, Laureano. Universidad Nacional de Río Negro. Sede Andina; 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: McCully, C.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Meza, N.. University of California at Davis; Estados Unidos Fil: Müller Bravo, T. E.. Instituto de Ciencias del Espacio; España Fil: Nicholl, M.. The Queens University of Belfast; Irlanda Fil: Pellegrino, C.. University of California; Estados Unidos Fil: Pignata, G.. Universidad Andrés Bello; Chile Fil: Sollerman, J.. Stockholm University; Suecia Fil: Tucker, B. E.. Australian National University; Australia Fil: Wang, X.. Beijing Academy of Science and Technology; China Fil: Young, D. R.. The Queens University of Belfast; Irlanda |
| description |
Hydrogen-rich Type II supernovae (SNe II) are the most frequently observed class of core-collapse SNe (CCSNe). However, most studies that analyse large samples of SNe II lack events with absolute peak magnitudes brighter than −18.5 mag at rest-frame optical wavelengths. Thanks to modern surveys, the detected number of such luminous SNe II (LSNe II) is growing. There exist several mechanisms that could produce luminous SNe II. The most popular propose either the presence of a central engine (a magnetar gradually spinning down or a black hole accreting fallback material) or the interaction of supernova ejecta with circumstellar material (CSM) that turns kinetic energy into radiation energy. In this work, we study the light curves and spectral series of a small sample of six LSNe II that show peculiarities in their H α profile, to attempt to understand the underlying powering mechanism. We favour an interaction scenario with CSM that is not dense enough to be optically thick to electron scattering on large scales – thus, no narrow emission lines are observed. This conclusion is based on the observed light curve (higher luminosity, fast decline, blue colours) and spectral features (lack of persistent narrow lines, broad H α emission, lack of H α absorption, weak, or non-existent metal lines) together with comparison to other luminous events available in the literature. We add to the growing evidence that transients powered by ejecta–CSM interaction do not necessarily display persistent narrow emission lines. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023-08 |
| 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 |
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http://hdl.handle.net/11336/234197 Pessi, Priscila Jael; Anderson, J. P.; Folatelli, Gaston; Dessart, L.; González Gaitán, S.; et al.; Broad-emission-line dominated hydrogen-rich luminous supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 523; 4; 8-2023; 5315-5340 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/234197 |
| identifier_str_mv |
Pessi, Priscila Jael; Anderson, J. P.; Folatelli, Gaston; Dessart, L.; González Gaitán, S.; et al.; Broad-emission-line dominated hydrogen-rich luminous supernovae; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 523; 4; 8-2023; 5315-5340 0035-8711 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad1822 info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/523/4/5315/7199790 |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf |
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Wiley Blackwell Publishing, Inc |
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Wiley Blackwell Publishing, Inc |
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