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dc.contributor.authorSingh, Avinash
dc.contributor.authorKumar, Brajesh
dc.contributor.authorMoriya, Takashi J.
dc.contributor.authorAnupama, G. C.
dc.contributor.authorSahu, D. K.
dc.contributor.authorBrown, Peter J.
dc.contributor.authorAndrews, Jennifer E.
dc.contributor.authorSMITH, NATHAN
dc.date.accessioned2019-10-09T17:27:30Z
dc.date.available2019-10-09T17:27:30Z
dc.date.issued2019-09-04
dc.identifier.citationAvinash Singh et al 2019 ApJ 882 68en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab3050
dc.identifier.urihttp://hdl.handle.net/10150/634700
dc.description.abstractThe optical and ultraviolet broadband photometric and spectroscopic observations of the Type II supernova (SN) 2016gfy are presented. The V-band light curve (LC) shows a distinct plateau phase with a slope of s(2) similar to 0.12 mag (100 day)(-1) and a duration of 90 +/- 5 days. Detailed analysis of SN 2016gfy provided a mean Ni-56 mass of 0.033 +/- 0.003 M-circle dot, a progenitor radius of similar to 350-700 R-circle dot, a progenitor mass of similar to 12-15 M-circle dot, and an explosion energy of (0.9-1.4) x 10(51) erg s(-1). The P-Cygni profile of H alpha in the early-phase spectra (similar to 11-21 days) shows a boxy emission. Assuming that this profile arises from the interaction of the SN ejecta with the pre-existing circumstellar material (CSM), it is inferred that the progenitor underwent a recent episode (30-80 yr prior to the explosion) of enhanced mass loss. Numerical modeling suggests that the early LC peak is reproduced better with an existing CSM of 0.15 M-circle dot spread out to similar to 70 au. A late-plateau bump is seen in the VRI LCs during similar to 50-95 days. This bump is explained as a result of the CSM interaction and/or partial mixing of radioactive Ni-56 in the SN ejecta. Using strong-line diagnostics, a subsolar oxygen abundance is estimated for the supernova H II region (12 + log(O/H) = 8.50 +/- 0.11), indicating an average metallicity for the host of an SN II. A star formation rate of similar to 8.5 M-circle dot yr(-1) is estimated for NGC 2276 using the archival GALEX FUV data.en_US
dc.description.sponsorshipScience and Engineering Research Board (SERB) under the Department of Science & Technology (DST), Govt. of India [PDF/2016/001563]; BRICS grant [DST/IMRCD/BRICS/PilotCall1/MuMeSTU/2017(G)]; DST/JSPS grant [DST/INT/JSPS/P/281/2018]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectgalaxies: individual (NGC 2276)en_US
dc.subjectsupernovae: generalen_US
dc.subjectsupernovae: individual (SN 2016gfy)en_US
dc.titleObservational Signature of Circumstellar Interaction and 56Ni-mixing in the Type II Supernova 2016gfyen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume882
dc.source.issue1
dc.source.beginpage68
refterms.dateFOA2019-10-09T17:27:31Z


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