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

Lingzhi Wang, Carlos Contreras, Maokai Hu, Mario A. Hamuy, Eric Y. Hsiao, David J. Sand, Joseph P. Anderson, Chris Ashall, Christopher R. Burns, Juncheng Chen, Tiara R. Diamond, Scott Davis, Francisco Förster, Lluís Galbany, Santiago González-Gaitán, Mariusz Gromadzki, Peter Hoeflich, Wenxiong Li, G. H. Marion, Nidia MorrellGiuliano Pignata, Jose L. Prieto, Mark M. Phillips, Melissa Shahbandeh, Nicholas B. Suntzeff, Stefano Valenti, Lifan Wang, Xiaofeng Wang, D. R. Young, Lixin Yu, Jujia Zhang

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5 Scopus citations


Supernova (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.

Original languageEnglish (US)
Article numberabba82
JournalAstrophysical Journal
Issue number1
StatePublished - Nov 20 2020

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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  • Optical and NIR observation of SN (Ia) 2017cbv

    Wang, L. (Creator), Contreras, C. (Creator), Hu, M. (Creator), Hamuy, M. A. (Creator), Hsiao, E. Y. (Creator), Sand, D. J. (Creator), Anderson, J. P. (Creator), Ashall, C. (Creator), Burns, C. R. (Creator), Chen, J. (Creator), Diamond, T. R. (Creator), Davis, S. (Creator), Förster, F. (Contributor), Galbany, L. (Creator), González-Gaitán, S. (Contributor), Gromadzki, M. (Creator), Hoeflich, P. (Creator), Li, W. (Creator), Marion, G. H. (Creator), Morrell, N. (Creator), Pignata, G. (Creator), Prieto, J. L. (Creator), Phillips, M. M. (Creator), Shahbandeh, M. (Creator), Suntzeff, N. B. (Creator), Valenti, S. (Creator), Wang, L. (Creator), Wang, X. (Creator), Young, D. R. (Creator), Yu, L. (Creator), Zhang, J. (Creator), Hamuy, M. A. (Creator), Hsiao, E. Y. (Creator), Sand, D. J. (Creator), Burns, C. R. (Creator), Forster, F. (Creator), Prieto, J. L. (Creator) & Valenti, S. (Creator), Centre de Donnees Strasbourg (CDS), 2022


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