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dc.contributor.authorKilpatrick, Charles D.
dc.contributor.authorAndrews, Jennifer E.
dc.contributor.authorSmith, Nathan
dc.contributor.authorMilne, P. A.
dc.contributor.authorRieke, George H.
dc.contributor.authorZheng, WeiKang
dc.contributor.authorFilippenko, Alexei V.
dc.date.accessioned2017-01-23T23:28:21Z
dc.date.available2017-01-23T23:28:21Z
dc.date.issued2016-11-21
dc.identifier.citationAn optical and near-infrared study of the Type Ia/IIn Supernova PS15si 2016, 463 (1):1088 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stw2061
dc.identifier.urihttp://hdl.handle.net/10150/622110
dc.description.abstractWe present optical/near-infrared spectroscopy and photometry of the supernova (SN) PS15si. This object was originally identified as a Type IIn SN, but here we argue that it should be reclassified as a Type Ia SN with narrow hydrogen lines originating from interaction with circumstellar matter (CSM; i.e. SN Ia/IIn or SN Ia-CSM). Based on deep non-detections 27 d before discovery, we infer that this SN was discovered around or slightly before optical maximum, and we estimate the approximate time that it reached R-band maximum based on comparison with other SNe Ia/IIn. In terms of spectral morphology, we find that PS15si can be matched to a range of SN Ia spectral types, although SN 1991T-like SNe Ia provides the most self-consistent match. While this spectral classification agrees with analysis of most other SNe Ia/IIn, we find that the implied CSM-interaction luminosity is too low. We infer that the similarity between PS15si and the hot, overluminous, high-ionization spectrum of SN 1991T is a consequence of a spectrum that originates in ejecta layers that are heated by ultraviolet/X-ray radiation from CSM interaction. In addition, PS15si may have rebrightened over a short time-scale in the B and V bands around 85 d after discovery, perhaps indicating that the SN ejecta are interacting with a local enhancement in CSM produced by clumps or a shell at large radii.
dc.description.sponsorshipW. M. Keck Foundation; ESO programmes [188.D-3003, 191.D-0935]; NASA [NNX12AR65G, NNX14AM74G]; NASA by JPL/Caltech [1255094]; NSF [AST-1312221, AST-1515559, AST-1211916]; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundationen
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttps://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw2061en
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectcircumstellar matteren
dc.subjectsupernovae: generalen
dc.subjectsupernovae: individual: PS15sien
dc.titleAn optical and near-infrared study of the Type Ia/IIn Supernova PS15sien
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
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
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-24T11:40:39Z
html.description.abstractWe present optical/near-infrared spectroscopy and photometry of the supernova (SN) PS15si. This object was originally identified as a Type IIn SN, but here we argue that it should be reclassified as a Type Ia SN with narrow hydrogen lines originating from interaction with circumstellar matter (CSM; i.e. SN Ia/IIn or SN Ia-CSM). Based on deep non-detections 27 d before discovery, we infer that this SN was discovered around or slightly before optical maximum, and we estimate the approximate time that it reached R-band maximum based on comparison with other SNe Ia/IIn. In terms of spectral morphology, we find that PS15si can be matched to a range of SN Ia spectral types, although SN 1991T-like SNe Ia provides the most self-consistent match. While this spectral classification agrees with analysis of most other SNe Ia/IIn, we find that the implied CSM-interaction luminosity is too low. We infer that the similarity between PS15si and the hot, overluminous, high-ionization spectrum of SN 1991T is a consequence of a spectrum that originates in ejecta layers that are heated by ultraviolet/X-ray radiation from CSM interaction. In addition, PS15si may have rebrightened over a short time-scale in the B and V bands around 85 d after discovery, perhaps indicating that the SN ejecta are interacting with a local enhancement in CSM produced by clumps or a shell at large radii.


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