Wang L.Contreras C.Hu M.Hamuy M.A.Hsiao E.Y.Sand D.J.Anderson J.P.Ashall C.Burns C.R.Chen J.Diamond T.R.Davis S.Förster F.Galbany L.González-Gaitán S.Gromadzki M.Hoeflich P.Li W.Marion G.H.Morrell N.Pignata G.Prieto J.L.Phillips M.M.Shahbandeh M.Suntzeff N.B.Valenti S.Wang L.Wang X.Young D.R.Yu L.Zhang J.2021-10-192021-10-192020-11Astrophysical Journal, Volume 904, Issue 120 November 2020 Article number abba820004637Xhttp://repositorio.unab.cl/xmlui/handle/ria/20550Indexación ScopusSupernova (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.enSupernovaeWhite DwarfsCompanion StarsArtículo10.3847/1538-4357/abba82