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Table 4

Spectral analysis of GRB 120711A per segment and instrument.

Segment Inst.a Time interval Model N H,intr z Γ kT / E break b χ2/d.o.f. F-testc
(ks since trigger) (1022 cm-2) (keV)
I IBIS 0.115–0.13 PL − − 1.69 ± 0.06 − 35/28 −
BBPL − − 1.36 ± 0.12 4.8 ± 0.9 19/26 4 × 10-4
BKNPL − − 1.38 ± 0.10 44 ± 6 18/26 2 × 10-4
2.24 ± 0.18
II IBIS 0.13–0.28 PL − − 2.22 ± 0.05 − 60/28 −
BBPL − − 1.93 ± 0.15 3.6 ± 1.3 47/26 4 × 10-2
BKNPL − − 1.0 ± 0.5 86 45/26 2 × 10-2
2.35 ± 0.08
III IBIS 0.28–2.5 PL − − 2.02 ± 0.06 − 27/25 −
Fermi/LAT 0.3–1.05 PL − − 2.00 ± 0.3 − 0.17/1 −
IBIS 2.5-10 PL − − 2.5 ± 0.5 − 1.43/5 −
JEM-X 7–20 PL − − 1.77 ± 0.27 − 7/5 −
Swift/XRT-wt 8.3–9 PL 1.79 ± 0.22 1.405d 1.99 ± 0.06 − 111/93 −
Swift/XRT-pc 14.7–239 PL 1.17 ± 0.11 1.405d 1.87 ± 0.04 − 153/152 −
XMM/pn 90–130 PL 0.87 ± 0.03 1.405d 1.950 ± 0.014 − 163/156 −
IV Chandra e 1126–1136 PL − − 1.7 ± 0.4 − 11/9 −
PL 1.17d 1.405d 1.84 ± 0.22 − 12/9 −
XMM/pne 1530–1560 PL − − 2.16 ± 0.13 − 16/16 −
PL 1.17d 1.405d 2.81 ± 0.20 − 27/16 −
Chandra e 1755–1775 PL − − 2.41 ± 0.23 − 5/9 −
PL 1.17d 1.405d 2.8 ± 0.3 − 8/9 −
XMM/pne 3040–3080 PL − − 2.5 ± 0.5 − 11/10 −
PL 1.17d 1.405d 4.4 ± 0.5 − 16/10 −
Chandra e 6600–6640 PL − − 2.8 ± 0.8 − 4/5 −
PL 1.17d 1.405d 3.7 ± 0.8 − 2/5 −
Chandra e 7100–7140 PL − − 2.7 ± 0.6 − 3/3 −
PL 1.17d 1.405d 3.3 ± 0.8 − 3/3 −

Notes. The models considered are power-law (PL), blackbody+powerlaw (BBPL), and broken power-law (BKNPL).

(a)

The energy range of the instruments is 20−200 keV for IBIS, 0.1−10 GeV for Fermi/LAT, 3−35 keV for JEM-X, and 0.3−10 keV for Swift/XRT, XMM-Newton-pn and Chandra/ACIS-S.

(b)

The parameter kT corresponds to the temperature of the BBPL model and Ebreak to the break energy of the BKNPL.

(c)

Throughout, the F-test probability corresponds to the improvement with respect to the simplest model (PL).

(d)

Parameter fixed in the spectral model.

(e)

Only the Galactic absorption component is included in these observations.

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