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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7399
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dc.contributor.authorGangopadhyay, A-
dc.contributor.authorMisra, K-
dc.contributor.authorHiramatsu, D-
dc.contributor.authorWang, Shan-Qin-
dc.contributor.authorHosseinzadeh, G-
dc.contributor.authorWang, Xiaofeng-
dc.contributor.authorValenti, Stefano-
dc.contributor.authorZhang, Jujia-
dc.contributor.authorHowel, D. A-
dc.contributor.authorArcavi, Iair-
dc.contributor.authorAnupama, G. C-
dc.contributor.authorBurke, Jamison-
dc.contributor.authorDastidar, Raya-
dc.contributor.authorKoichi Itagaki, Koichi-
dc.contributor.authorKumar, Brajesh-
dc.contributor.authorKumar, B-
dc.contributor.authorLi, Long-
dc.contributor.authorMcCully, Curtis-
dc.contributor.authorMo, Jun-
dc.contributor.authorPandey, S. B-
dc.contributor.authorPellegrino, Craig-
dc.contributor.authorSa, Hanna-
dc.contributor.authorSahu, D. K-
dc.contributor.authorPankaj Sanwal-
dc.contributor.authorSingh, A-
dc.contributor.authorSingh, M-
dc.contributor.authorZhang, Jicheng-
dc.contributor.authorZhang, Tianmeng-
dc.contributor.authorZhang, Xinhan-
dc.date.accessioned2020-11-26T15:25:55Z-
dc.date.available2020-11-26T15:25:55Z-
dc.date.issued2020-02-01-
dc.identifier.citationThe Astrophysical Journal, Vol. 889, No. 2, 170en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/7399-
dc.descriptionRestricted Accessen_US
dc.description.abstractWe present photometric and spectroscopic observations of the type Ibn supernova (SN) 2019uo, the second ever SN Ibn with flash ionization (He ii, C iii, N iii) features in its early spectra. SN 2019uo displays a rapid post-peak luminosity decline of 0.1 mag day−1 similar to most of the SNe Ibn, but is fainter(M max = - 18.30 + 0.24 mag) than a typical SN Ibn and shows a color evolution that places it between SNe Ib and the most extreme SNe Ibn. SN 2019uo shows P-cygni He i features in the early spectra which gradually evolve and become emission dominated post peak. It also shows faster evolution in line velocities as compared to most other members of the type Ibn subclass. The bolometric light curve is fairly well described by a 56Ni + circumstellar interaction model.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ab6328-
dc.rights© The American Astronomical Society-
dc.subjectCore-collapse supernovaeen_US
dc.subjectSupernovaeen_US
dc.subjectCCD photometryen_US
dc.subjectPhotometryen_US
dc.subjectSpectroscopyen_US
dc.subjectAstronomical techniquesen_US
dc.titleFlash Ionization Signatures in the Type Ibn Supernova SN 2019uoen_US
dc.typeArticleen_US
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