@article{bc1b45a154c840f3a8d04e26e85bea5a,
title = "GRB 161219B/SN 2016jca: a powerful stellar collapse",
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 × 1050 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° ± 3°). 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 an SN associated with a GRB. Reproducing it requires a large photospheric velocity (35000 ± 7000 km s-1). The kinetic energy of the SN is estimated through models to be Ekin≈4 × 1052 erg in spherical symmetry. The ejected mass in the explosion was Mej≈6.5 ± 1.5 M⊙, much less than that of other GRB-SNe, demonstrating diversity among these events. The total amount of 56Ni in the explosion was 0.27 ± 0.05 M⊙. The observed spectra require the presence of freshly synthesized 56Ni at the highest velocities, at least three times more than a standard GRB-SN. We also find evidence for a decreasing 56Ni 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) × 1052 erg, confirming that most of the energy produced by GRB-SNe goes into the kinetic energy of the SN ejecta.",
keywords = "supernovae: general, supernovae: individual",
author = "C. Ashall and Mazzali, {P. A.} and E. Pian and Woosley, {S. E.} and E. Palazzi and Prentice, {S. J.} and S. Kobayashi and S. Holmbo and A. Levan and D. Perley and Stritzinger, {M. D.} and F. Bufano and Filippenko, {A. V.} and A. Melandri and S. Oates and A. Rossi and J. Selsing and W. Zheng and Castro-Tirado, {A. J.} and G. Chincarini and P. D'avanzo and {De Pasquale}, M. and S. Emery and Fruchter, {A. S.} and K. Hurley and P. Moller and K. Nomoto and M. Tanaka and Valeev, {A. F.}",
note = "Funding Information: The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and theMax Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University,DurhamUniversity, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, NASA grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, NSF grant AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Funding Information: The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen{\textquoteright}s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, NASA grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, NSF grant AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Funding Information: CA acknowledges support provided by the National Science Foundation (NSF) under grant AST–1613472. Work in this paper was based on observations made with ESO telescopes at the Paranal Observatory under programmes ID 098.D-0055(A), 098.D-0218(A), 298.D-5022(A), and 0100.D-0504(A). MS and SH are supported by a generous grant (13261) from VILLUM FONDEN. MS is also supported by a project grant from the IRFD (Independent Research Fund Denmark). A portion of this work was supported by a grant fron IDA (Danish Instrument Center for Danish Astrophysics). The work of AVF and WZ has been supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and the Miller Institute for Basic Research in Science (U.C. Berkeley). SRO acknowledges the support of the Leverhulme Trust. EP acknowledges Scuola Normale Superiore and INAF for support. AFV thanks the Russian Science Foundation for grant 14-50-00043. AM acknowledges support from the ASI INAF grant I/004/11/1. AJCT acknowledges support from the Spanish Ministry Project AYA2015-71718-R. Funding Information: SW at UCSC was supported by the NASA Theory Program (NNX14AH34G) Both the Liverpool Telescope and the GTC are operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Based on observations made with the TNG, operated on the island of La Palma by the Fundaci{\'o}n Galileo Galilei of the Instituto Nazionale di Astrofisica (INAF) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias under programme A32TAC5. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the Paranal Director for allocating Discretionary Time to this programme, the Paranal Science Operations team for their assistance, and T. Kr{\"u}hler for assistance with X-Shooter data reduction. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. IRAF is the Image Reduction and Analysis Facility made available to the astronomical community by the National Optical Astronomy Observatories, which are operated by AURA, Inc., under contract with the US National Science Foundation. It is available at http://iraf.noao.edu. Publisher Copyright: {\textcopyright} 2019 The Author(s).",
year = "2019",
month = jun,
day = "25",
doi = "10.1093/mnras/stz1588",
language = "English",
volume = "487",
pages = "5824--5839",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",
}