GRB 161219B/SN 2016jca: a low-redshift gamma-ray burst supernova powered by radioactive heating
Author
dc.contributor.author
Cano, Z.
Author
dc.contributor.author
Izzo, L.
Author
dc.contributor.author
Ugarte Postigo, A. de
Author
dc.contributor.author
Fuentes González, Cesar
Admission date
dc.date.accessioned
2018-07-05T14:47:54Z
Available date
dc.date.available
2018-07-05T14:47:54Z
Publication date
dc.date.issued
2017
Cita de ítem
dc.identifier.citation
Astronomy & Astrophysics, 605, A107 (2017)
es_ES
Identifier
dc.identifier.other
10.1051/0004-6361/201731005
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/149531
Abstract
dc.description.abstract
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 GRB-supernovae (SNe) have been discovered. The intermediate-luminosity Swift GRB 161219B and its associated 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 in the E-p,E-i - E-gamma,E-iso plane, while SN 2016jca had a rest-frame, peak absolute V-band magnitude of M-V = -19.0 +/- 0.1, which it reached after 12.3 +/- 0.7 rest-frame days. We find that the bolometric properties of SN 2016jca are inconsistent with being powered solely by a magnetar central engine, 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 nucleosynthesised when its progenitor underwent core collapse. We find that 0.22 +/- 0.08 M-circle dot of nickel is required to reproduce the peak luminosity of SN 2016jca, and we constrain an ejecta mass of 5.8 +/- 0.3 M-circle dot and a kinetic energy of 5.1 +/- 0.8 x 10(52) erg. Finally, we report on a chromatic, pre-maximum bump in the g-band light curve, and discuss its possible origin.
es_ES
Patrocinador
dc.description.sponsorship
Spanish research project
AYA 2014-58381-P
Ramon y Cajal fellowships
RyC-2012-09984
RyC-2012-09975
Juan de la Cierva Incorporacion fellowships
IJCI-2015-26153
IJCI-2014-21669
BBVA Foundation Grant for Researchers and Cultural Creators
Sofia Kovalevskaja Award
Alexander von Humboldt Foundation of Germany
Instrument center for Danish Astrophysics (IDA)
European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme
098.A-0055A
European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO
Public ESO Spectroscopic Survey for Transient Objects Survey) ESO program
188.D-3003
191.D-0935
197.D-1075
University of Florida
National Science Foundation
AST-0352664
AST-1238877
Leibniz-Prize
HA 1850/28-1
National Aeronautics and Space Administration under Planetary Science Division of the NASA Science Mission Directorate
NNX08AR22G
Association of Universities for Research in Astronomy, Inc., under NASA
NAS 526555