2022/01/10 by Brajesh Kumar, Avinash Singh, D. K. Sahu +1
Mathematics · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #Geology #Mathematics #Neutrino Physics Research #Observational study #Paleontology #Physics #Statistics #Supernova #Type (biology) #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/ac4bb9
23 pages, 15 figures, 8 tables. Accepted for publication in ApJ
arxiv created 2022/01/10 · openalex publication_date 2022/03/01 · arxiv updated 2022/03/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report results of optical imaging and low-resolution spectroscopic monitoring of supernova (SN) 2017iro that occurred in the nearby (∼ 31 Mpc) galaxy NGC 5480. The \ionHe1 5876 Å feature present in the earliest spectrum (-- 7 d) classified it as a Type Ib SN. The follow-up observations span from -- 7 to + 266 d with respect to the B-band maximum. With a peak absolute magnitude in V-band, (MV) = -17.76±0.15 mag and bolometric luminosity (log10 L) = 42.39 ± 0.09 erg s-1, SN 2017iro is a moderately luminous Type Ib SN. The overall light curve evolution of SN 2017iro is similar to SN 2012au and SN 2009jf during the early (up to ∼100 d) and late phases (>150 d), respectively. The line velocities of both \ionFe2 5169 Å and \ionHe1 5876 Å are ∼ 9000 km s-1 near the peak. The analysis of the nebular phase spectrum (∼ +209 d) indicates an oxygen mass of ∼ 0.35 M\odot. The smaller [\ionO1]/[\ionCa2] flux ratio of ∼ 1 favours a progenitor with a zero-age main-sequence mass in the range ∼ 13--15 M\odot, most likely in a binary system, similar to the case of iPTF13bvn. The explosion parameters are estimated by applying different analytical models to the quasi-bolometric light curve of SN 2017iro. 56Ni mass synthesized in the explosion has a range of ∼ 0.05 -- 0.10 M\odot, the ejecta mass ∼1.4 -- 4.3 M\odot and the kinetic energy ∼ 0.8 -- 1.9 × 1051 erg.