Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv

Abstract

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 BVRIYJHK s -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 ± 0.006 mag, with a postmaximum magnitude decline of Δ m 15 ( 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 H 0  = 72 km s −1 Mpc −1 , we found that 0.73 M ⊙ 56 Ni 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 Pa β 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 well-observed normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some M ch delayed detonation models and sub- M ch double detonation models.