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Table 7:

Best-fit decay indexes of the early optical emission for all GRBs with well monitored optical counterpart that shows a steep-to-shallow behavior (Fig. 10).
GRB Filter $\alpha_1$ $\alpha_2$ $t_{{\rm break}}$ z
990123(1) V $\sim$2.5 $\sim$1.5 700 1.60
021211(2) R $1.97\pm0.05$ $1.01\pm0.02$ 300 1.0
060117(3) R $2.49\pm0.05$ $1.47\pm0.03$ 300 1a
061126(4) R $2.0\pm0.3$ $0.76\pm0.06$ 780 1.1588
060111B R $2.4\pm0.2$ $1.18\pm0.05$ 75 2
080319B(5) R $2.49\pm0.09$ $1.25\pm0.02$ 900 0.937
090102(6) R $1.83\pm0.13$ $1.1\pm0.3$ 400 1.547
For GRB 060117 since the redshift is not known, we imposed z=1.
References. (1) Akerlof et al. (1999); (2) Holland et al. (2004); (3) Jelínek et al. (2006); (4) Perley et al. (2008); (5) Racusin et al. (2008a); (6) Klotz et al. (2009).

Source LaTeX | All tables | In the text

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