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Table 2

Prompt emission time resolved spectral analysis.

Dataa # Startb Stopb Modelc Γ Epeak Ad kT ABB χ2(d.o.f.)
[s] [s] [keV] [ph cm-2 s-1] [keV] [ph cm-2 s-1]

B+G 1 0.256 1.792 CPL 0.92 207 2.93 164(244)
... 2 1.792 6.912 CPL 1.29 69 6.09 192(272)
... 3 17.152 23.296 PL 1.82 9.43 168(286)

X+B+G 4 90 100 CPL+BB 1.26 218 0.71 1.23 0.041 211(256) 3.8 × 10-7
... 5 100 110 CPL+BB 1.06 316 0.89 3.02 0.17 279(301) 8.0 × 10-13
... 6 110 120 CPL+BB 1.18 209 2.08 2.01 0.55 257(296) 6.3 × 10-35
... 7 120 130 CPL+BB 1.50 76 2.71 1.12 0.51 284(293) 8.7 × 10-45

X 8 130 140 BB 39(34)
... 9 140 150 PL+BB 30(26) 2.3 × 10-6
... 10 150 160 PL+BB 36(46) 4.6 × 10-10
... 11 160 170 PL 53(45) (0.02)e
... 12 170 180 PL 50(40) (0.01)e
... 13 180 190 PL 16(30)
... 14 190 200 PL 25(22)

XMM 7.8 × 105 1.3 × 106 PL+BB 398(345) 5.8 × 10-7

Notes.

(a)

Spectral data used in the fit: B = Swift/BAT, G = Fermi/GBM and X = Swift/XRT.

(b)

Times refer to the trigger time of the burst.

(c)

Models adopted in the fit: CPL = powerlaw with exponential cutoff, PL = powerlaw, BB = blackbody; galactic (NH,gal = 3.7 × 1020 cm-2) and intrinsic (NH = 4.4 × 1021 cm-2) absorption is present in all models (using Tuebingen–Boulder ISM absorption model, Wilms et al. 2000).

(d)

Spectral normalization is computed at 1 keV.

(e)

In this case the addition of a BB component is not statistically significant, as suggested by the value of the null hypothesis probability associated with the F-test. The horizontal lines correspond to the differently shaded regions in Fig. 1.

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