Table 1: Results of spectral analysis.
Power law (PL) with cutoff IBIS
$\Gamma$ $2.1\pm0.1$
$E_{\rm cut}$, keV >110 ($2\sigma$)
Flux (18-200 keV)a $1.65\pm0.2$
Flux (2-10 keV)b 1.3
$\chi^2/{\rm d.o.f}$ 7.6/10
Absorbed PL GIS
$N_{\rm H}$, 1022 cm-2 $1.5\pm0.2$
$\Gamma$ $1.48\pm0.15$
Flux (2-10 keV) 0.35
$\chi^2/{\rm d.o.f}$ 17.0/15
Absorbed PL with cutoff IBIS+GIS+ART-P
$N_{\rm H}$, 1022 cm-2 $2.0\pm0.3$
$\Gamma$ $1.7\pm0.2$
$E_{\rm cut}$ $156^{+\infty}_{-55}$
Flux (2-200 keV, IBIS)c 2.1
Flux (2-200 keV, GIS)c 1.3
Flux (2-200 keV, ART-P)c 2.1
$\chi^2/{\rm d.o.f}$ 34.1/34
Absorbed PL with cutoff+reflection IBIS+GIS+ART-P
$N_{\rm H}$, 1022 cm-2 $2.2\pm0.2$
$\Gamma$ $1.9\pm0.2$
$E_{\rm cut}$ >120 ($2\sigma$)
$R\equiv\Omega/2\pi$ 1.0 (fixed)
Flux (2-200 keV, IBIS)c 2.2
Flux (2-200 keV, GIS)c 1.8
Flux (2-200 keV, ART-P)c 2.8
$\chi^2/{\rm d.o.f}$ 34.4/34
    a All quoted fluxes are observed (uncorrected for absorption) ones and are given in units of 10-10 erg s-1 cm-2.
    b Flux in the 2-10 keV band computed from the model assuming interstellar absorption with $N_{\rm H}=1.5\times 10^{22}$ cm-2.
    c Model flux in the 2-200 keV band scaled to match the IBIS, GIS or ART-P data.


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