GRB161219B/SN2016jca: a powerful stellar collapse

被引：41

作者：

Ashall, C. ^{[1
,2
]}

Mazzali, P. A. ^{[2
,3
]}

Pian, E. ^{[4
]}

Woosley, S. E. ^{[5
]}

Palazzi, E. ^{[4
]}

Prentice, S. J. ^{[2
,6
]}

Kobayashi, S. ^{[2
]}

Holmbo, S. ^{[7
]}

Levan, A. ^{[8
]}

Perley, D. ^{[2
]}

Stritzinger, M. D. ^{[7
]}

Bufano, F. ^{[9
]}

Filippenko, A. V. ^{[10
,11
]}

Melandri, A. ^{[12
]}

Oates, S. ^{[8
]}

Rossi, A. ^{[4
]}

Selsing, J. ^{[13
]}

Zheng, W. ^{[10
]}

Castro-Tirado, A. J. ^{[14
]}

Chincarini, G. ^{[12
]}

D'Avanzo, P. ^{[12
]}

De Pasquale, M. ^{[15
]}

Emery, S. ^{[16
]}

Fruchter, A. S. ^{[17
]}

Hurley, K. ^{[18
]}

Moller, P. ^{[19
]}

Nomoto, K. ^{[20
]}

Tanaka, M. ^{[21
]}

Valeev, A. F. ^{[22
]}

机构：

[1] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[2] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[3] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany

[4] INAF OAS Bologna, Via P Gobetti 93-3, I-40129 Bologna, Italy

[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[6] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[7] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark

[8] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[9] Astron Observ Catania, INAF, Via Santa Sofia 78, I-95123 Catania, Italy

[10] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

[11] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA

[12] Brera Astron Observ, INAF, Via Santa Sofia 78, I-95123 Catania, Italy

[13] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark

[14] CSIC, Glorieta Astron, IAA, E-18008 Granada, Spain

[15] Istanbul Univ Beyazid, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey

[16] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[17] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 20218 USA

[18] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA

[19] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[20] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

[21] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[22] Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 487卷 / 04期

基金：

俄罗斯科学基金会; 英国科学技术设施理事会; 美国国家科学基金会;

关键词：

supernovae: general; supernovae: individual; GAMMA-RAY BURST; BOLOMETRIC LIGHT CURVES; OPTICAL AFTERGLOW; SUPERNOVA; SPECTRA; ULTRAVIOLET; EXPLOSIONS; MODEL; JETS; STAR;

D O I：

10.1093/mnras/stz1588

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report observations and analysis of the nearby gamma-ray burst GRB161219B (redshift z= 0.1475) and the associated Type Ic supernova (SN) 2016jca. GRB161219B had an isotropic gamma-ray energy of similar to 1.6x10(50)erg. Its afterglow is likely refreshed at an epoch preceding the first photometric points (0.6d), 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 similar to 42 degrees +/- 3 degrees). Our spectral series shows broad absorption lines typical of GRB supernovae (SNe), which testify to the presence of material with velocities up to similar to 0.25c. The spectrum at 3.73d allows for the very early identification of an SN associated with a GRB. Reproducing it requires a large photospheric velocity (kms(-1)). The kinetic energy of the SN is estimated through models to be E-kin approximate to 4x10(52)erg in spherical symmetry. The ejected mass in the explosion was M-ej approximate to 6.5 +/- 1.5M(circle dot), much less than that of other GRB-SNe, demonstrating diversity among these events. The total amount of Ni-56 in the explosion was 0.27 +/- 0.05M(circle dot). The observed spectra require the presence of freshly synthesized Ni-56 at the highest velocities, at least threetimes more than a standard GRB-SN. We also find evidence for a decreasing Ni-56 abundance as a function of decreasing velocity. This suggests that SN2016jca was a highly aspherical explosion viewed close to on-axis, powered by a compact remnant. Applying a typical correction for asymmetry, the energy of SN2016jca was similar to(1-3)x10(52)erg, confirming that most of the energy produced by GRB-SNe goes into the kinetic energy of the SN ejecta.

引用

页码：5824 / 5839

页数：16

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