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

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

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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: 13 Aug 2015 07:51
URI: http://researchonline.ljmu.ac.uk/id/eprint/1827

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