Idiomas

Optical and Near-infrared Observations of SN 2013dx Associated with GRB 130702A

Toy, V. L.; Cenko, S. B.; Silverman, J. M.; Butler, N. R.; Cucchiara, A.; Watson, A. M.; Bersier, D.; Perley, D. A.; Margutti, R.; Bellm, E.; Bloom, J. S.; Cao, Y.; Capone, J. I.; Clubb, K.; Corsi, A.; De Cia, A.; de Diego, J. A.; Filippenko, A. V.; Fox, O. D.; Gal-Yam, A.; Gehrels, N.; Georgiev, L.; González, J. J.; Kasliwal, M. M.; Kelly, P. L.; Kulkarni, S. R.; Kutyrev, A. S.; Lee, W. H.; Prochaska, J. X.; Ramirez-Ruiz, E.; Richer, M. G.; Román-Zúñiga, C.; Singer, L.; Stern, D.; Troja, E.; Veilleux, S.
The Astrophysical Journal, Volume 818, Issue 1, article id. 79, 19 pp. (2016).
02/2016

ABSTRACT

We present optical and near-infrared (NIR) 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}γ ,{iso}={6.4}-1.0+1.3× {10}50 erg (1 keV to 10 MeV 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 ∼20% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined SNe Ic, 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 ∼ 21,000 km s‑1. We construct a quasi-bolometric ({g}\prime {r}\prime {i}\prime {z}\prime {yJ}) light curve for SN 2013dx, only the fifth GRB-associated SN with extensive NIR coverage and the third with a bolometric light curve extending beyond {{Δ }}t\gt 40 {{days}}. Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a 56Ni mass of {M}{Ni}=0.37+/- 0.01 {M}ȯ , an ejecta mass of {M}{ej}=3.1+/- 0.1 {M}ȯ , and a kinetic energy of {E}{{K}}=(8.2+/- 0.43)× {10}51 erg (statistical uncertainties only), consistent with previous GRB-associated supernovae. When considering the ensemble population of GRB-associated supernovae, we find no correlation between the mass of synthesized 56Ni and high-energy properties, despite clear predictions from numerical simulations that {M}{Ni} should correlate with the degree of asymmetry. On the other hand, {M}{Ni} clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.