OPTICAL AND NEAR-INFRARED OBSERVATIONS OF SN 2013DX ASSOCIATED WITH GRB 130702A

被引:33
|
作者
Toy, V. L. [1 ]
Cenko, S. B. [2 ,3 ]
Silverman, J. M. [4 ]
Butler, N. R. [5 ]
Cucchiara, A. [2 ]
Watson, A. M. [6 ]
Bersier, D. [7 ]
Perley, D. A. [8 ]
Margutti, R. [9 ]
Bellm, E. [8 ]
Bloom, J. S. [10 ]
Cao, Y. [8 ]
Capone, J. I. [1 ]
Clubb, K. [10 ]
Corsi, A. [11 ]
De Cia, A. [12 ]
de Diego, J. A. [6 ]
Filippenko, A. V. [10 ]
Fox, O. D. [10 ]
Gal-Yam, A. [12 ]
Gehrels, N. [2 ]
Georgiev, L. [6 ]
Gonzalez, J. J. [6 ]
Kasliwal, M. M. [13 ]
Kelly, P. L. [10 ]
Kulkarni, S. R. [8 ]
Kutyrev, A. S. [2 ]
Lee, W. H. [6 ]
Prochaska, J. X. [14 ]
Ramirez-Ruiz, E. [14 ]
Richer, M. G. [6 ]
Roman-Zuniga, C. [6 ]
Singer, L. [2 ,15 ]
Stern, D. [16 ]
Troja, E. [1 ,2 ]
Veilleux, S. [1 ,3 ]
机构
[1] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[2] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[3] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA
[4] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA
[5] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA
[6] Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 106, Ensenada 22800, Baja California, Mexico
[7] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England
[8] CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA
[9] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[10] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA
[11] Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA
[12] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel
[13] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA
[14] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA
[15] CALTECH, LIGO Lab, Pasadena, CA 91125 USA
[16] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
来源
ASTROPHYSICAL JOURNAL | 2016年 / 818卷 / 01期
基金
美国国家科学基金会;
关键词
gamma-ray burst: individual (GRB 130702A); supernovae: individual (SN 2013dx); GAMMA-RAY BURST; LATE-TIME SPECTRA; LIGHT CURVES; RELATIVISTIC SUPERNOVAE; LOW-RESOLUTION; IC SUPERNOVAE; IBC SUPERNOVA; DATA RELEASE; OFF-AXIS; LONG;
D O I
10.3847/0004-637X/818/1/79
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 gamma,iso = 6.4(-1.0)(+1.3) x 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'r'i'z' light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves similar to 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 similar to 21,000 km s(-1). We construct a quasi-bolometric (g'r'i'z'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 Delta t > 40 days. Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a Ni-56 mass of M-Ni = 0.37 +/- 0.01 M-circle dot, an ejecta mass of M-ej = 3.1 +/- 0.1 M-circle dot, and a kinetic energy of E-K = (8.2 +/- 0.43) x 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 Ni-56 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.
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页数:19
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