Optical and near-infrared observations of the nearby SN Ia 2017cbv

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dc.contributor.authorWang L.
dc.contributor.authorContreras C.
dc.contributor.authorHu M.
dc.contributor.authorHamuy M.A.
dc.contributor.authorHsiao E.Y.
dc.contributor.authorSand D.J.
dc.contributor.authorAnderson J.P.
dc.contributor.authorAshall C.
dc.contributor.authorBurns C.R.
dc.contributor.authorChen J.
dc.contributor.authorDiamond T.R.
dc.contributor.authorDavis S.
dc.contributor.authorFörster F.
dc.contributor.authorGalbany L.
dc.contributor.authorGonzález-Gaitán S.
dc.contributor.authorGromadzki M.
dc.contributor.authorHoeflich P.
dc.contributor.authorLi W.
dc.contributor.authorMarion G.H.
dc.contributor.authorMorrell N.
dc.contributor.authorPignata G.
dc.contributor.authorPrieto J.L.
dc.contributor.authorPhillips M.M.
dc.contributor.authorShahbandeh M.
dc.contributor.authorSuntzeff N.B.
dc.contributor.authorValenti S.
dc.contributor.authorWang L.
dc.contributor.authorWang X.
dc.contributor.authorYoung D.R.
dc.contributor.authorYu L.
dc.contributor.authorZhang J.
dc.date.accessioned2021-10-19T18:36:30Z
dc.date.available2021-10-19T18:36:30Z
dc.date.issued2020-11
dc.descriptionIndexación Scopuses
dc.description.abstractSupernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 ± 0.006mag, with a postmaximum magnitude decline of Δm15(B) = 0.990 ± 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus μ = 30.58 ± 0.05 mag and assuming H0 = 72 km s-1 Mpc-1, we found that 0.73M⊙ 56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M⊙. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other wellobserved normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch delayed detonation models and sub-Mch double detonation models. © 2020. The American Astronomical Society.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.3847/1538-4357/abba82
dc.identifier.citationAstrophysical Journal, Volume 904, Issue 120 November 2020 Article number abba82es
dc.identifier.doi10.3847/1538-4357/abba82
dc.identifier.issn0004637X
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/20550
dc.language.isoenes
dc.publisherIOP Publishing Ltdes
dc.subjectSupernovaees
dc.subjectWhite Dwarfses
dc.subjectCompanion Starses
dc.titleOptical and near-infrared observations of the nearby SN Ia 2017cbves
dc.typeArtículoes
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