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dc.contributor.author
Dong, Yize
dc.contributor.author
Valenti, S.
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Bostroem, K. A.
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Sand, D. J.
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Andrews, Jennifer E.
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Galbany, Lluís
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Jha, Saurabh W.
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Eweis, Youssef
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Kwok, Lindsey
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Hsiao, Eric
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Davis, Scott
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Brown, Peter J.
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Kuncarayakti, H.
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Maeda, Keiichi
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Rho, Jeonghee
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Amaro, R. C.
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Anderson, J. P.
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Arcavi, Iair
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Burke, Jamison
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Dastidar, Raya
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Folatelli, Gaston
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Haislip, Joshua
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Hiramatsu, Daichi
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Hosseinzadeh, Griffin
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Howell, D. Andrew
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Jencson, J.
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Kouprianov, Vladimir
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Lundquist, M.
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Lyman, J. D.
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McCully, Curtis
dc.date.available
2022-02-24T14:12:46Z
dc.date.issued
2021-01
dc.identifier.citation
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; 1-22
dc.identifier.issn
0004-637X
dc.identifier.uri
http://hdl.handle.net/11336/152657
dc.description.abstract
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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
IOP Publishing
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Core-collapse supernovae
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Type II supernovae
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Astronomía
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dc.subject.classification
Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
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dc.title
Supernova 2018cuf : a type iip supernova with a slow fall from plateau
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2022-02-04T13:30:02Z
dc.journal.volume
906
dc.journal.number
1
dc.journal.pagination
1-22
dc.journal.pais
Reino Unido
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dc.description.fil
Fil: Dong, Yize. University of California at Davis; Estados Unidos
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Fil: Valenti, S.. University of California at Davis; Estados Unidos
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Fil: Bostroem, K. A.. University of California at Davis; Estados Unidos
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Fil: Sand, D. J.. University of Arizona; Estados Unidos
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Fil: Andrews, Jennifer E.. University of Arizona; Estados Unidos
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Fil: Galbany, Lluís. Universidad de Granada; España
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Fil: Jha, Saurabh W.. State University of New Jersey; Estados Unidos
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Fil: Eweis, Youssef. State University of New Jersey; Estados Unidos
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Fil: Kwok, Lindsey. State University of New Jersey; Estados Unidos
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Fil: Hsiao, Eric. Florida State University; Estados Unidos
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Fil: Davis, Scott. Florida State University; Estados Unidos
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Fil: Brown, Peter J.. Texas A&M University; Estados Unidos
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Fil: Kuncarayakti, H.. University of Turku; Finlandia
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Fil: Maeda, Keiichi. Kyoto University; Japón
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Fil: Rho, Jeonghee. SETI Institute; Estados Unidos
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Fil: Amaro, R. C.. University of Arizona; Estados Unidos
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Fil: Anderson, J. P.. European Southern Observatory Chile; Chile
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Fil: Arcavi, Iair. Universitat Tel Aviv; Israel
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Fil: Burke, Jamison. University of California; Estados Unidos
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Fil: Dastidar, Raya. Aryabhatta Research Institute of observational sciences; India
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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
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Fil: Haislip, Joshua. University of North Carolina at Chapel Hill; Estados Unidos
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Fil: Hiramatsu, Daichi. University of California; Estados Unidos
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Fil: Hosseinzadeh, Griffin. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Howell, D. Andrew. University of California; Estados Unidos
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Fil: Jencson, J.. University of Arizona; Estados Unidos
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Fil: Kouprianov, Vladimir. University of North Carolina at Chapel Hill; Estados Unidos
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Fil: Lundquist, M.. University of Arizona; Estados Unidos
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Fil: Lyman, J. D.. University of Warwick; Reino Unido
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Fil: McCully, Curtis. University of California; Estados Unidos
dc.journal.title
Astrophysical Journal
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.3847/1538-4357/abc417
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abc417
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