Observational Signature of Circumstellar Interaction and 56 Ni-mixing in the Type II Supernova 2016gfy

Abstract

The optical and ultraviolet broadband photometric and spectroscopic observations of the Type II supernova (SN) 2016gfy are presented. The V -band light curve (LC) shows a distinct plateau phase with a slope of s 2 ∼ 0.12 mag (100 day) −1 and a duration of 90 ± 5 days. Detailed analysis of SN 2016gfy provided a mean 56 Ni mass of 0.033 ± 0.003 M ⊙ , a progenitor radius of ∼350–700 R ⊙ , a progenitor mass of ∼12–15 M ⊙ , and an explosion energy of (0.9–1.4) × 10 51 erg s −1 . The P-Cygni profile of H α in the early-phase spectra (∼11–21 days) shows a boxy emission. Assuming that this profile arises from the interaction of the SN ejecta with the pre-existing circumstellar material (CSM), it is inferred that the progenitor underwent a recent episode (30–80 yr prior to the explosion) of enhanced mass loss. Numerical modeling suggests that the early LC peak is reproduced better with an existing CSM of 0.15 M ⊙ spread out to ∼70 au. A late-plateau bump is seen in the VRI LCs during ∼50–95 days. This bump is explained as a result of the CSM interaction and/or partial mixing of radioactive 56 Ni in the SN ejecta. Using strong-line diagnostics, a subsolar oxygen abundance is estimated for the supernova H ii region (12 + log(O/H) = 8.50 ± 0.11), indicating an average metallicity for the host of an SN II. A star formation rate of ∼8.5 M ⊙ yr −1 is estimated for NGC 2276 using the archival GALEX FUV data.