Supernova 2018cuf: A type iip supernova with a slow fall from plateau
- Autores
- Dong, Yize; Valenti, S.; Bostroem, K.A.; Sand, D.J.; Andrews, Jennifer E.; Galbany, L.; Jha, Saurabh W.; Eweis, Youssef; Kwok, Lindsey; Hsiao, E.Y.; Davis, Scott; Brown, Peter J.; Kuncarayakti, H.; Maeda, Keiichi; Rho, Jeonghee; Amaro, R.C.; Anderson, J.P.; Arcavi, Iair; Burke, Jamison; Dastidar, Raya; Folatelli, Gaston; Haislip, Joshua; Hiramatsu, Daichi; Hosseinzadeh, Griffin; Andrew Howell, D.; Jencson, J.; Kouprianov, Vladimir; Lundquist, M.; Lyman, J. D.; McCully, Curtis
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present multiband photometry and spectroscopy of SN 2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN 2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of −16.73 ± 0.32 at maximum and a decline rate of 0.21 ± 0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8 ± 5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN 2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN 2018cuf was most likely a red supergiant of about 14.5 Me that produced 0.04 ± 0.01 Me 56Ni during the explosion. We also found ∼0.07 Me of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ∼11,000 km s−1 were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN.
Fil: Dong, Yize. University of California at Davis; Estados Unidos
Fil: Valenti, S.. University of California at Davis; Estados Unidos
Fil: Bostroem, K.A.. University of California at Davis; Estados Unidos
Fil: Sand, D.J.. University of Arizona; Estados Unidos
Fil: Andrews, Jennifer E.. University of Arizona; Estados Unidos
Fil: Galbany, L.. Universidad de Granada; España
Fil: Jha, Saurabh W.. State University of New Jersey; Estados Unidos
Fil: Eweis, Youssef. State University of New Jersey; Estados Unidos. University of Iowa; Estados Unidos
Fil: Kwok, Lindsey. State University of New Jersey; Estados Unidos
Fil: Hsiao, E.Y.. Florida State University; Estados Unidos
Fil: Davis, Scott. University of California at Davis; Estados Unidos
Fil: Brown, Peter J.. Texas A&M University; Estados Unidos
Fil: Kuncarayakti, H.. University of Turku; Finlandia
Fil: Maeda, Keiichi. Kyoto University; Japón. University of Tokyo; Japón
Fil: Rho, Jeonghee. Seti Institute; Estados Unidos
Fil: Amaro, R.C.. University of Arizona; Estados Unidos
Fil: Anderson, J.P.. European Southern Observatory Chile; Chile
Fil: Arcavi, Iair. Universitat Tel Aviv; Israel. Canadian Institute for Advanced Research; Canadá
Fil: Burke, Jamison. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos
Fil: Dastidar, Raya. Aryabhatta Research Institute of Observational Sciences; India. University of Delhi; India
Fil: Folatelli, Gaston. University of Tokyo; Japón. 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: Haislip, Joshua. University of North Carolina; Estados Unidos
Fil: Hiramatsu, Daichi. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos
Fil: Hosseinzadeh, Griffin. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Andrew Howell, D.. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos
Fil: Jencson, J.. University of Arizona; Estados Unidos
Fil: Kouprianov, Vladimir. University of North Carolina; Estados Unidos
Fil: Lundquist, M.. University of Arizona; Estados Unidos
Fil: Lyman, J. D.. University of Warwick; Reino Unido
Fil: McCully, Curtis. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos - Materia
-
Core-collapse supernovae
Type II supernovae (1731) - 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:11336/145749
Ver los metadatos del registro completo
| id |
CONICETDig_47e041cbc39baa43c44f5e82fa696d77 |
|---|---|
| oai_identifier_str |
oai:ri.conicet.gov.ar:11336/145749 |
| network_acronym_str |
CONICETDig |
| repository_id_str |
3498 |
| network_name_str |
CONICET Digital (CONICET) |
| spelling |
Supernova 2018cuf: A type iip supernova with a slow fall from plateauDong, YizeValenti, S.Bostroem, K.A.Sand, D.J.Andrews, Jennifer E.Galbany, L.Jha, Saurabh W.Eweis, YoussefKwok, LindseyHsiao, E.Y.Davis, ScottBrown, Peter J.Kuncarayakti, H.Maeda, KeiichiRho, JeongheeAmaro, R.C.Anderson, J.P.Arcavi, IairBurke, JamisonDastidar, RayaFolatelli, GastonHaislip, JoshuaHiramatsu, DaichiHosseinzadeh, GriffinAndrew Howell, D.Jencson, J.Kouprianov, VladimirLundquist, M.Lyman, J. D.McCully, CurtisCore-collapse supernovaeType II supernovae (1731)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present multiband photometry and spectroscopy of SN 2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN 2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of −16.73 ± 0.32 at maximum and a decline rate of 0.21 ± 0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8 ± 5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN 2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN 2018cuf was most likely a red supergiant of about 14.5 Me that produced 0.04 ± 0.01 Me 56Ni during the explosion. We also found ∼0.07 Me of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ∼11,000 km s−1 were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN.Fil: Dong, Yize. University of California at Davis; Estados UnidosFil: Valenti, S.. University of California at Davis; Estados UnidosFil: Bostroem, K.A.. University of California at Davis; Estados UnidosFil: Sand, D.J.. University of Arizona; Estados UnidosFil: Andrews, Jennifer E.. University of Arizona; Estados UnidosFil: Galbany, L.. Universidad de Granada; EspañaFil: Jha, Saurabh W.. State University of New Jersey; Estados UnidosFil: Eweis, Youssef. State University of New Jersey; Estados Unidos. University of Iowa; Estados UnidosFil: Kwok, Lindsey. State University of New Jersey; Estados UnidosFil: Hsiao, E.Y.. Florida State University; Estados UnidosFil: Davis, Scott. University of California at Davis; Estados UnidosFil: Brown, Peter J.. Texas A&M University; Estados UnidosFil: Kuncarayakti, H.. University of Turku; FinlandiaFil: Maeda, Keiichi. Kyoto University; Japón. University of Tokyo; JapónFil: Rho, Jeonghee. Seti Institute; Estados UnidosFil: Amaro, R.C.. University of Arizona; Estados UnidosFil: Anderson, J.P.. European Southern Observatory Chile; ChileFil: Arcavi, Iair. Universitat Tel Aviv; Israel. Canadian Institute for Advanced Research; CanadáFil: Burke, Jamison. University of California; Estados Unidos. Las Cumbres Observatory; Estados UnidosFil: Dastidar, Raya. Aryabhatta Research Institute of Observational Sciences; India. University of Delhi; IndiaFil: Folatelli, Gaston. University of Tokyo; Japón. 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: Haislip, Joshua. University of North Carolina; Estados UnidosFil: Hiramatsu, Daichi. University of California; Estados Unidos. Las Cumbres Observatory; Estados UnidosFil: Hosseinzadeh, Griffin. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Andrew Howell, D.. University of California; Estados Unidos. Las Cumbres Observatory; Estados UnidosFil: Jencson, J.. University of Arizona; Estados UnidosFil: Kouprianov, Vladimir. University of North Carolina; Estados UnidosFil: Lundquist, M.. University of Arizona; Estados UnidosFil: Lyman, J. D.. University of Warwick; Reino UnidoFil: McCully, Curtis. University of California; Estados Unidos. Las Cumbres Observatory; Estados UnidosIOP Publishing2021-01info: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/11336/145749Dong, Yize; Valenti, S.; Bostroem, K.A.; Sand, D.J.; Andrews, Jennifer E.; et al.; Supernova 2018cuf: A type iip supernova with a slow fall from plateau; IOP Publishing; Astrophysical Journal; 906; 1; 1-2021; 1-150004-637X1538-4357CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abc417info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abc417info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:46:27Zoai:ri.conicet.gov.ar:11336/145749instacron: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 09:46:27.489CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| title |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| spellingShingle |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau Dong, Yize Core-collapse supernovae Type II supernovae (1731) |
| title_short |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| title_full |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| title_fullStr |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| title_full_unstemmed |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| title_sort |
Supernova 2018cuf: A type iip supernova with a slow fall from plateau |
| dc.creator.none.fl_str_mv |
Dong, Yize Valenti, S. Bostroem, K.A. Sand, D.J. Andrews, Jennifer E. Galbany, L. Jha, Saurabh W. Eweis, Youssef Kwok, Lindsey Hsiao, E.Y. Davis, Scott Brown, Peter J. Kuncarayakti, H. Maeda, Keiichi Rho, Jeonghee Amaro, R.C. Anderson, J.P. Arcavi, Iair Burke, Jamison Dastidar, Raya Folatelli, Gaston Haislip, Joshua Hiramatsu, Daichi Hosseinzadeh, Griffin Andrew Howell, D. Jencson, J. Kouprianov, Vladimir Lundquist, M. Lyman, J. D. McCully, Curtis |
| author |
Dong, Yize |
| author_facet |
Dong, Yize Valenti, S. Bostroem, K.A. Sand, D.J. Andrews, Jennifer E. Galbany, L. Jha, Saurabh W. Eweis, Youssef Kwok, Lindsey Hsiao, E.Y. Davis, Scott Brown, Peter J. Kuncarayakti, H. Maeda, Keiichi Rho, Jeonghee Amaro, R.C. Anderson, J.P. Arcavi, Iair Burke, Jamison Dastidar, Raya Folatelli, Gaston Haislip, Joshua Hiramatsu, Daichi Hosseinzadeh, Griffin Andrew Howell, D. Jencson, J. Kouprianov, Vladimir Lundquist, M. Lyman, J. D. McCully, Curtis |
| author_role |
author |
| author2 |
Valenti, S. Bostroem, K.A. Sand, D.J. Andrews, Jennifer E. Galbany, L. Jha, Saurabh W. Eweis, Youssef Kwok, Lindsey Hsiao, E.Y. Davis, Scott Brown, Peter J. Kuncarayakti, H. Maeda, Keiichi Rho, Jeonghee Amaro, R.C. Anderson, J.P. Arcavi, Iair Burke, Jamison Dastidar, Raya Folatelli, Gaston Haislip, Joshua Hiramatsu, Daichi Hosseinzadeh, Griffin Andrew Howell, D. Jencson, J. Kouprianov, Vladimir Lundquist, M. Lyman, J. D. McCully, Curtis |
| 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 |
Core-collapse supernovae Type II supernovae (1731) |
| topic |
Core-collapse supernovae Type II supernovae (1731) |
| 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 multiband photometry and spectroscopy of SN 2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN 2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of −16.73 ± 0.32 at maximum and a decline rate of 0.21 ± 0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8 ± 5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN 2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN 2018cuf was most likely a red supergiant of about 14.5 Me that produced 0.04 ± 0.01 Me 56Ni during the explosion. We also found ∼0.07 Me of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ∼11,000 km s−1 were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN. Fil: Dong, Yize. University of California at Davis; Estados Unidos Fil: Valenti, S.. University of California at Davis; Estados Unidos Fil: Bostroem, K.A.. University of California at Davis; Estados Unidos Fil: Sand, D.J.. University of Arizona; Estados Unidos Fil: Andrews, Jennifer E.. University of Arizona; Estados Unidos Fil: Galbany, L.. Universidad de Granada; España Fil: Jha, Saurabh W.. State University of New Jersey; Estados Unidos Fil: Eweis, Youssef. State University of New Jersey; Estados Unidos. University of Iowa; Estados Unidos Fil: Kwok, Lindsey. State University of New Jersey; Estados Unidos Fil: Hsiao, E.Y.. Florida State University; Estados Unidos Fil: Davis, Scott. University of California at Davis; Estados Unidos Fil: Brown, Peter J.. Texas A&M University; Estados Unidos Fil: Kuncarayakti, H.. University of Turku; Finlandia Fil: Maeda, Keiichi. Kyoto University; Japón. University of Tokyo; Japón Fil: Rho, Jeonghee. Seti Institute; Estados Unidos Fil: Amaro, R.C.. University of Arizona; Estados Unidos Fil: Anderson, J.P.. European Southern Observatory Chile; Chile Fil: Arcavi, Iair. Universitat Tel Aviv; Israel. Canadian Institute for Advanced Research; Canadá Fil: Burke, Jamison. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos Fil: Dastidar, Raya. Aryabhatta Research Institute of Observational Sciences; India. University of Delhi; India Fil: Folatelli, Gaston. University of Tokyo; Japón. 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: Haislip, Joshua. University of North Carolina; Estados Unidos Fil: Hiramatsu, Daichi. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos Fil: Hosseinzadeh, Griffin. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Andrew Howell, D.. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos Fil: Jencson, J.. University of Arizona; Estados Unidos Fil: Kouprianov, Vladimir. University of North Carolina; Estados Unidos Fil: Lundquist, M.. University of Arizona; Estados Unidos Fil: Lyman, J. D.. University of Warwick; Reino Unido Fil: McCully, Curtis. University of California; Estados Unidos. Las Cumbres Observatory; Estados Unidos |
| description |
We present multiband photometry and spectroscopy of SN 2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN 2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of −16.73 ± 0.32 at maximum and a decline rate of 0.21 ± 0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8 ± 5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN 2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN 2018cuf was most likely a red supergiant of about 14.5 Me that produced 0.04 ± 0.01 Me 56Ni during the explosion. We also found ∼0.07 Me of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ∼11,000 km s−1 were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN. |
| publishDate |
2021 |
| dc.date.none.fl_str_mv |
2021-01 |
| 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/11336/145749 Dong, Yize; Valenti, S.; Bostroem, K.A.; Sand, D.J.; Andrews, Jennifer E.; et al.; Supernova 2018cuf: A type iip supernova with a slow fall from plateau; IOP Publishing; Astrophysical Journal; 906; 1; 1-2021; 1-15 0004-637X 1538-4357 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/145749 |
| identifier_str_mv |
Dong, Yize; Valenti, S.; Bostroem, K.A.; Sand, D.J.; Andrews, Jennifer E.; et al.; Supernova 2018cuf: A type iip supernova with a slow fall from plateau; IOP Publishing; Astrophysical Journal; 906; 1; 1-2021; 1-15 0004-637X 1538-4357 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abc417 info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abc417 |
| 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 application/pdf |
| dc.publisher.none.fl_str_mv |
IOP Publishing |
| publisher.none.fl_str_mv |
IOP Publishing |
| dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
| reponame_str |
CONICET Digital (CONICET) |
| collection |
CONICET Digital (CONICET) |
| 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 |
| _version_ |
1844613450266836992 |
| score |
13.070432 |