2017/12/13 by D. K. Sahu, G. C. Anupama, N. K. Chakradhari +7
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Ejecta #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Light curve #Line (geometry) #Metallicity #Photometry (optics) #Physics #Pulsars and Gravitational Waves Research #Spectral line #Stars #Supernova #Type II supernova #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stx3212
15 pages, 17 figures and 4 tables. Accepted for publication in MNRAS main journal
openalex publication_date 2017/12/13 · arxiv created 2018/01/22 · arxiv updated 2018/02/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present optical and ultraviolet photometry and low-resolution optical spectroscopy of the broad-line Type Ic supernova SN 2014ad in the galaxy PGC 37625 (Mrk 1309), covering the evolution of the supernova during −5 to +87 d with respect to the date of maximum in the B band. A late-phase spectrum obtained at +340 d is also presented. With an absolute V-band magnitude at peak of MV = −18.86 ± 0.23 mag, SN 2014ad is fainter than supernovae associated with gamma ray bursts (GRBs), and brighter than most of the normal and broad-line Type Ic supernovae without an associated GRB. The spectral evolution indicates that the expansion velocity of the ejecta, as measured using the Si ii line, is as high as ∼33 500 km s−1 around maximum, while during the post-maximum phase it settles at ∼15 000 km s−1. The expansion velocity of SN 2014ad is higher than that of all other well-observed broad-line Type Ic supernovae except for the GRB-associated SN 2010bh. The explosion parameters, determined by applying Arnett's analytical light-curve model to the observed bolometric light-curve, indicate that it was an energetic explosion with a kinetic energy of ∼(1 ± 0.3) × 1052 erg and a total ejected mass of ∼(3.3 ± 0.8) M⊙, and that ∼0.24 M⊙ of 56Ni was synthesized in the explosion. The metallicity of the host galaxy near the supernova region is estimated to be ∼0.5 Z⊙.