Table 3: Afterglow model tests using X-ray data. The condition for closure depends on whether $\nu _{\rm c} > \nu _{\rm X}$ or $\nu _{\rm c} < \nu _{\rm X}$ (Col. 2). p is the power-law index of the emitting electron population.
Model $\nu_{\rm c}$ b, c Closure p

ISM > $\nu_{\rm X}$ (-3/2, 0) $0.76\pm0.06$ $1.94\pm0.02$

ISM > $\nu_{\rm X}$ (-3/2, 1/2) $1.26\pm0.05$ $0.94\pm0.02$

Wind > $\nu_{\rm X}$ (-3/2, -1/2) $0.26\pm0.05$ $1.94\pm0.02$

Wind > $\nu_{\rm X}$ (-3/2, 1/2) $1.26\pm0.05$ $0.94\pm0.02$

Jet > $\nu_{\rm X}$ (-2, -1) $-0.48\pm0.06$ $1.94\pm0.02$

Jet > $\nu_{\rm X}$ (-2, 0) $0.52\pm0.06$ $0.94\pm0.02$

**Table 3:** Afterglow model tests using X-ray data. The condition for closure depends on whether $\nu _{\rm c} > \nu _{\rm X}$ or $\nu _{\rm c} < \nu _{\rm X}$ (Col. 2). p is the power-law index of the emitting electron population.
Model	$\nu_{\rm c}$	b, c	Closure	p
ISM	> $\nu_{\rm X}$	(-3/2, 0)	$0.76\pm0.06$	$1.94\pm0.02$
ISM	> $\nu_{\rm X}$	(-3/2, 1/2)	$1.26\pm0.05$	$0.94\pm0.02$
Wind	> $\nu_{\rm X}$	(-3/2, -1/2)	$0.26\pm0.05$	$1.94\pm0.02$
Wind	> $\nu_{\rm X}$	(-3/2, 1/2)	$1.26\pm0.05$	$0.94\pm0.02$
Jet	> $\nu_{\rm X}$	(-2, -1)	$-0.48\pm0.06$	$1.94\pm0.02$
Jet	> $\nu_{\rm X}$	(-2, 0)	$0.52\pm0.06$	$0.94\pm0.02$

Source LaTeX | All tables | In the text

	1 Introduction
	2 INTEGRAL observations and results
	3 XMM-Newton
	4 Discussion
	5 Conclusion
	References