Tools
Tools
Cano, Z, de Ugarte Postigo, A, Pozanenko, A, Butler, N, Thoene, CC, Guidorzi, C, Kruehler, T, Gorosabel, J, Jakobsson, P, Leloudas, G, Malesani, D, Hjorth, J, Melandri, A, Mundell, CG, Wiersema, K, D'Avanzo, P, Schulze, S, Gomboc, A, Johansson, A, Zheng, W , Kann, DA, Knust, F, Varela, K, Akerlof, CW, Bloom, J, Burkhonov, V, Cooke, E, de Diego, JA, Dhungana, G, Farina, C, Ferrante, FV, Flewelling, HA, Fox, OD, Fynbo, J, Gehrels, N, Georgiev, L, Gonzalez, JJ, Greiner, J, Guever, T, Hatch, N, Jelinek, M, Kehoe, R, Klose, S, Klunko, E, Kopae, D, Kutyrev, A, Krugly, Y, Lee, WH, Levan, A, Linkov, V, Matkin, A, Minikulov, N, Molotov, I, Prochaska, JX, Rieher, MG, Roman-Zuniga, CG, Rumyantsev, V, Sanchez-Ramirez, R, Steele, IA, Tanvir, NR, Volnova, A, Watson, AM, 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
|
Text
1405.3114v1.pdf - Accepted Version Download (851kB) | Preview |
Abstract
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: | 04 Sep 2021 12:05 |
| DOI or ID number: | 10.1051/0004-6361/201423920 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/5281 |
 |
View Item |