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|Title:||Multiwavelength analysis of three supernovae associated with gamma-ray bursts observed by GROND||Authors:||Olivares E., F.
Kann, D. A.
Afonso, P. M. J.
Nicuesa Guelbenzu, A.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||577||First Page:||A44||Abstract:||Context. After the discovery of the first connection between γ-ray bursts (GRBs) and supernovae (SNe) almost two decades ago, tens of SN-like rebrightenings have been discovered and about seven solid associations have been spectroscopically confirmed to date. Aims: We determine the luminosity, evolution, and origin of three SN rebrightenings in GRB afterglow light curves at z ~ 0.5 along with accurate determinations of the host-galaxy extinction. We estimate physical parameters of the SN explosions, such as synthesised <SUP>56</SUP>Ni mass, ejecta mass, and kinetic energy. Methods: We employ GROND optical/NIR data and Swift X-ray/UV data to estimate the host-galaxy extinction by modelling the afterglow spectral energy distribution, to determine the SN luminosity and evolution, and to construct quasi-bolometric light curves. The latter are corrected for the contribution of the NIR-bands using data available in the literature and black-body fits. We employ Arnett's analytic approach to obtain the physical parameters of the explosion. Results: The SNe 2008hw, 2009nz, and 2010ma observed by GROND exhibit 0.80, 1.15, and 1.78 times the optical (r'-band) luminosity of SN 1998bw, respectively. While SN 2009nz exhibits an evolution similar to SN 1998bw, SNe 2008hw and 2010ma show earlier peak times. The quasi-bolometric light curves (340-2200 nm) confirm the large luminosity of SN 2010ma (1.4 × 10<SUP>43</SUP> erg s<SUP>-1</SUP>), while SNe 2008hw and 2009nz reached a peak luminosity closer to that of SN 1998bw. The modelling indicates in <SUP>56</SUP>Ni masses of around 0.4-0.5 M<SUB>☉</SUB>. Conclusions: By means of a very comprehensive data set, we found that the luminosity and the <SUP>56</SUP>Ni mass of SNe 2008hw, 2009nz, and 2010ma resembles those of other known GRB-associated SNe. These findings strengthens previous claims of GRB-SNe being brighter than stripped-envelope SNe unaccompanied by GRBs. <P />Appendices are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201321936/olm">http://www.aanda.org</A>||Acknowledgments:||We acknowledge the referee for suggestions and corrections that helped improve the paper significantly. F.O.E. thanks F. Bufano for sanity checks on the bolometric LCs. The Ph.D. studies of F.O.E. were funded both by the Deutscher Akademischer Austausch Dienst (DAAD) and the Comisión Nacional de Investigación Científica y Tecnológica (CONICYT). F.O.E. acknowledges support from FONDECYT through postdoctoral grant 3140326. F.O.E. and G.P. acknowledge support from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Iniciativa Científica Milenio del Ministerio de Economía, Fomento y Turismo de Chile. Part of the GROND funding (both hardware and personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger, Deutsche Forschungsgemeinschaft (DFG) grant HA 1850/28–1. S.K., A.R., A.N., D.A.K. acknowledge support by DFG grant KL 766/16-1. S.S. acknowledges support by the Thüringer Ministerium für Bildung, Wissenschaft und Kultur under FKZ 12010-514. D.A.K. acknowledges financial support from MPE and TLS. A.R., A.N., D.A.K. are grateful for travel funding support through MPE. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester and data from the NASA’s Astrophysics Data System (NAS 5–26555). The Dark Cosmology Centre is funded by the Danish National Research Foundation.||URI:||http://hdl.handle.net/20.500.12386/23311||URL:||https://www.aanda.org/articles/aa/abs/2015/05/aa21936-13/aa21936-13.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201321936||Bibcode ADS:||2015A&A...577A..44O||Fulltext:||open|
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