Facial reconstruction

Search LJMU Research Online

Browse Repository | Browse E-Theses

Optical and near-infrared observations of SN 2013dx associated with GRB 130702A

Toy, VL, Cenko, SB, Silverman, JM, Butler, NR, Cucchiara, A, Watson, AM, Bersier, D, Perley, DA, Margutti, R, Bellm, E, Bloom, JS, Cao, Y, Capone, JI, Clubb, K, Corsi, A, Diego, JAD, Filippenko, AV, Fox, OD, Gal-Yam, A, Gehrels, N , Georgiev, L, González, JJ, Kasliwal, MM, Kelly, PL, Kulkarni, SR, Kutyrev, AS, Lee, WH, Prochaska, JX, Ramirez-Ruiz, E, Richer, MG, Román, C, Singer, L, Stern, D, Troja, E and Veilleux, S (2015) Optical and near-infrared observations of SN 2013dx associated with GRB 130702A. Astrophysical Journal. ISSN 1538-4357 (Submitted)

1508.00575v1.pdf - Submitted Version

Download (1MB) | Preview


We present optical and near-infrared light curves and optical spectra of SN 2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB 130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is measured to be $E_{\gamma,\mathrm{iso}} = 6.4_{-1.0}^{+1.3} \times 10^{50}$erg (1keV to 10MeV in the rest frame), placing it intermediate between low-luminosity GRBs like GRB 980425/SN 1998bw and the broader cosmological population. We compare the observed $g^{\prime}r^{\prime}i^{\prime}z^{\prime}$ light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves $\sim20$% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined Type Ic supernovae, both associated with (SN 2006aj and SN 1998bw) and lacking (SN 1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric velocities around peak of $\sim$21,000 km s$^{-1}$. We construct a quasi-bolometric ($g^{\prime}r^{\prime}i^{\prime}z^{\prime}yJH$) light curve for SN 2013dx, and, together with the photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a $^{56}$Ni mass of $M_{\mathrm{Ni}} = 0.38\pm 0.01$M$_{\odot}$, an ejecta mass of $M_{\mathrm{ej}} = 3.0 \pm 0.1$ M$_{\odot}$, and a kinetic energy of $E_{\mathrm{K}} = (8.2 \pm 0.40) \times 10^{51}$erg (statistical uncertainties only), consistent with previous GRB-associated SNe. When considering the ensemble population of GRB-associated SNe, we find no correlation between the mass of synthesized $^{56}$Ni and high-energy properties, despite clear predictions from numerical simulations that $M_{\mathrm{Ni}}$ should correlate with the degree of asymmetry. On the other hand, $M_{\mathrm{Ni}}$ clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.

Item Type: Article
Uncontrolled Keywords: astro-ph.HE; astro-ph.HE
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Publisher: American Astornomical Society and IOP Publishing
Related URLs:
Date Deposited: 13 Aug 2015 07:51
Last Modified: 04 Sep 2021 14:05
URI: https://researchonline.ljmu.ac.uk/id/eprint/1827
View Item View Item