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تسجيل مستخدم جديدGRB 161219B-SN 2016jca: a powerful stellar collapse
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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 $sim 1.6 times 10^{50}$,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 $sim 42^circ pm 3^circ$). Our spectral series shows broad absorption lines typical of GRB supernovae (SNe), which testify to the presence of material with velocities up to $sim 0.25$c. 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 ($35,000 pm 7000$,kms). The kinetic energy of the SN is estimated through models to be KE $approx 4 times 10^{52}$,erg in spherical symmetry. The ejected mass in the explosion was Mej $approx 6.5 pm 1.5$,Msun, much less than that of other GRB-SNe, demonstrating diversity among these events. The total amount of Nifs in the explosion was $0.27 pm 0.05$,Msun. The observed spectra require the presence of freshly synthesised Nifs at the highest velocities, at least 3 times more than a standard GRB-SN. We also find evidence for a decreasing Nifs 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 $sim$ (1--3) $times 10^{52}$,erg, confirming that most of the energy produced by GRB-SNe goes into the kinetic energy of the SN ejecta.
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Since the first discovery of a broad-lined type Ic supernova (SN) with a long-duration gamma-ray burst (GRB) in 1998, fewer than fifty gamma-ray burst supernovae (GRB-SNe) have been discovered. The intermediate-luminosity Swift GRB 161219B and its as
sociated supernova SN 2016jca, which occurred at a redshift of z=0.1475, represents only the seventh GRB-SN to have been discovered within 1 Gpc, and hence provides an excellent opportunity to investigate the observational and physical properties of these very elusive and rare type of SN. As such, we present optical to near-infrared photometry and optical spectroscopy of GRB 161219B and SN 2016jca, spanning the first three months since its discovery. GRB 161219B exploded in the disk of an edge-on spiral galaxy at a projected distance of 3.4 kpc from the galactic centre. GRB 161219B itself is an outlier of the Amati relation, while SN 2016jca had a rest-frame, peak absolute V-band magnitude of M_V = -19.0, which it reached after 12.5 rest-frame days. We find that the bolometric properties of SN 2016jca are inconsistent with being powered solely by a magnetar central engine, as proposed by other authors, and demonstrate that it was likely powered exclusively by energy deposited by the radioactive decay of nickel and cobalt into their daughter products, which were nucleosynthesized when its progenitor underwent core collapse. We find that 0.22 solar masses of nickel is required to reproduce the peak luminosity of SN 2016jca, and we constrain an ejecta mass of 5.8 solar masses and a kinetic energy of ~5 x 10^52 erg. Finally, we report on a chromatic, pre-maximum bump in the g-band light curve, and discuss its possible origin. [Abridged]
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