GRB 161219B/SN 2016jca: a powerful stellar collapse

DOI: 
10.1093/mnras/stz1588
Publication date: 
01/06/2019
Main author: 
Ashall, C.
IAA authors: 
Castro-Tirado, A. J.
Authors: 
Ashall, C.;Mazzali, P. A.;Pian, E.;Woosley, S. E.;Palazzi, E.;Prentice, S. J.;Kobayashi, S.;Holmbo, S.;Levan, A.;Perley, D.;Stritzinger, M. D.;Bufano, F.;Filippenko, A. V.;Melandri, A.;Oates, S.;Rossi, A.;Selsing, J.;Zheng, W.;Castro-Tirado, A. J.;Chincarini, G.;D'Avanzo, P.;De Pasquale, M.;Emery, S.;Fruchter, A. S.;Hurley, K.;Moller, P.;Nomoto, K.;Tanaka, M.;Valeev, A. F.
Journal: 
Monthly Notices of the Royal Astronomical Society
Refereed: 
Yes
Publication type: 
Article
Pages: 
5824-5839
Abstract: 
We report observations and analysis of the nearby gamma-ray burst GRB 161219B (redshift z = 0.1475) and the associated Type Ic supernova (SN) 2016jca. GRB 161219B had an isotropic gamma-ray energy of ̃1.6 × 10<SUP>50</SUP> erg. Its afterglow is likely refreshed at an epoch preceding the first photometric points (0.6 d), which slows down the decay rates. Combined analysis of the SN light curve and multiwavelength observations of the afterglow suggest that the GRB jet was broad during the afterglow phase (full opening angle ̃42<SUP>○</SUP> ± 3<SUP>○</SUP>). Our spectral series shows broad absorption lines typical of GRB supernovae (SNe), which testify to the presence of material with velocities up to ̃0.25c. The spectrum at 3.73 d allows for the very early identification of a SN associated with a GRB. Reproducing it requires a large photospheric velocity (35, 000 ± 7000 km s<SUP>-1</SUP>). The kinetic energy of the SN is estimated through models to be E<SUB>kin</SUB>≈4 × 10<SUP>52</SUP> erg in spherical symmetry. The ejected mass in the explosion was M<SUB>ej</SUB>≈6.5 ± 1.5 M<SUB>☉</SUB>, much less than that of other GRB-SNe, demonstrating diversity among these events. The total amount of <SUP>56</SUP>Ni in the explosion was 0.27 ± 0.05 M<SUB>☉</SUB>. The observed spectra require the presence of freshly synthesised <SUP>56</SUP>Ni at the highest velocities, at least 3 times more than a standard GRB-SN. We also find evidence for a decreasing <SUP>56</SUP>Ni abundance as a function of decreasing velocity. This suggests that SN 2016jca was a highly aspherical explosion viewed close to on-axis, powered by a compact remnant. Applying a typical correction for asymmetry, the energy of SN 2016jca was ̃ (1-3) × 10<SUP>52</SUP> erg, confirming that most of the energy produced by GRB-SNe goes into the kinetic energy of the SN ejecta.
Database: 
ADS
SCOPUS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85070095083&doi=10.1093%2fmnras%2fstz1588&partnerID=40&md5=56e7415b820813948b9d08df9717de04
ADS Bibcode: 
2019MNRAS.487.5824A
Keywords: 
gamma-ray burst;supernova