XRF 100316D/SN 2010bh AND THE NATURE OF GAMMA-RAY BURST SUPERNOVAE

被引:82
作者
Cano, Z. [1 ]
Bersier, D. [1 ]
Guidorzi, C. [1 ,2 ]
Kobayashi, S. [1 ]
Levan, A. J. [3 ]
Tanvir, N. R. [4 ]
Wiersema, K. [4 ]
D'Avanzo, P. [5 ]
Fruchter, A. S. [6 ]
Garnavich, P. [7 ]
Gomboc, A. [8 ,9 ]
Gorosabel, J. [10 ]
Kasen, D. [11 ]
Kopac, D. [8 ]
Margutti, R. [5 ]
Mazzali, P. A. [12 ,13 ]
Melandri, A. [1 ,5 ]
Mundell, C. G. [1 ]
Nugent, P. E. [14 ]
Pian, E. [13 ,15 ]
Smith, R. J. [1 ]
Steele, I. [1 ]
Wijers, R. A. M. J. [16 ]
Woosley, S. E. [17 ]
机构
[1] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England
[2] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy
[3] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England
[4] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England
[5] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy
[6] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[7] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA
[8] Univ Ljubljana, Fac Math & Phys, Ljubljana, Slovenia
[9] Ctr Excellence SPACE SI, Ljubljana SI-1000, Slovenia
[10] Inst Astrofis Andalucia IAA CSIC, Granada, Spain
[11] Univ Calif Berkeley, Dept Astron & Astrophys, Berkeley, CA USA
[12] Max Planck Inst Astrophys, D-85741 Garching, Germany
[13] INAF Oss Astron Padova, Padua, Italy
[14] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
[15] Osserv Astron Trieste, I-34131 Trieste, Italy
[16] Univ Amsterdam, Astron Inst, Xh Amsterdam, Netherlands
[17] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA
基金
英国科学技术设施理事会;
关键词
gamma-ray burst: general; gamma-ray burst: individual (XRF 100316D); supernovae: general; supernovae: individual (SN 2010bh); 25; APRIL; 1998; SHOCK BREAKOUT; X-RAY; LIGHT CURVES; HOST GALAXY; SN; 1998BW; UBVRI PHOTOMETRY; IC SUPERNOVA; OPTICAL OBSERVATIONS; SPECTRAL MODELS;
D O I
10.1088/0004-637X/740/1/41
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present ground-based and Hubble Space Telescope optical and infrared observations of Swift XRF 100316D/SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype gamma-ray burst supernova (GRB-SN) 1998bw, but at a similar rate to SN 2006aj, an SN that was spectroscopically linked with XRF 060218, and at a similar rate to the non-GRB associated Type Ic SN 1994I. We estimate the rest-frame extinction of this event from our optical data to be E(B - V) = 0.18 +/- 0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M-V = -18.62 +/- 0.08, which is the faintest peak V-band magnitude observed to date for spectroscopically confirmed GRB-SNe. When we investigate the origin of the flux at t - t(0) = 0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the SN shock breakout. We then use our optical and infrared data to create a quasi-bolometric light curve of SN 2010bh, which we model with a simple analytical formula. The results of our modeling imply that SN 2010bh synthesized a nickel mass of M-Ni approximate to 0.1 M-circle dot, ejected M-ej approximate to 2.2 M-circle dot, and has an explosion energy of E-k approximate to 1.4 x 10(52) erg. Thus, while SN 2010bh is an energetic explosion, the amount of nickel created during the explosion is much less than that of SN 1998bw and only marginally more than SN 1994I. Finally, for a sample of 22 GRB-SNe we check for a correlation between the stretch factors and luminosity factors in the R band and conclude that no statistically significant correlation exists.
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页数:17
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