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A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu

Cano, Z and de Ugarte Postigo, A and Pozanenko, A and Butler, N and Thoene, CC and Guidorzi, C and Kruehler, T and Gorosabel, J and Jakobsson, P and Leloudas, G and Malesani, D and Hjorth, J and Melandri, A and Mundell, CG and Wiersema, K and D'Avanzo, P and Schulze, S and Gomboc, A and Johansson, A and Zheng, W and Kann, DA and Knust, F and Varela, K and Akerlof, CW and Bloom, J and Burkhonov, V and Cooke, E and de Diego, JA and Dhungana, G and Farina, C and Ferrante, FV and Flewelling, HA and Fox, OD and Fynbo, J and Gehrels, N and Georgiev, L and Gonzalez, JJ and Greiner, J and Guever, T and Hatch, N and Jelinek, M and Kehoe, R and Klose, S and Klunko, E and Kopae, D and Kutyrev, A and Krugly, Y and Lee, WH and Levan, A and Linkov, V and Matkin, A and Minikulov, N and Molotov, I and Prochaska, JX and Rieher, MG and Roman-Zuniga, CG and Rumyantsev, V and Sanchez-Ramirez, R and Steele, IA and Tanvir, NR and Volnova, A and Watson, AM and Xu, D and Yuan, F (2014) A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. Astronomy and Astrophysics, 568. ISSN 0004-6361

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We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t − t0 = 16.1 d, which covers rest-frame 3000–6250 Å. Based on Fe ii λ5169 and Si ii λ6355, our spectrum indicates an unusually low expansion velocity of ~4000–6350 km s-1, the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Mészáros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 × 1015 G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Q Science > QD Chemistry
Divisions: Astrophysics Research Institute
Publisher: EDP Sciences
Related URLs:
Date Deposited: 18 Jan 2017 09:47
Last Modified: 06 Sep 2017 17:09
DOI or Identification number: 10.1051/0004-6361/201423920
URI: http://researchonline.ljmu.ac.uk/id/eprint/5281

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