Table 2: Spectral fit results.

Spectruma		 $N_{\rm H}$ $\Gamma$ $\chi^2$ (d.o.f.)/ $L_{1 - 10 {\rm ~keV}}$b
  (1022 cm-2)   C-stat (%)c (erg s-1)

001 (2006)		 $0.88_{\rm -0.62}^{+0.96}$ $\rm 1.89_{\rm -0.92}^{+1.07}$ 167.7 (65.8%) $2.35\times10^{-1}$
001-005 $2.28_{\rm -1.50}^{+2.21}$ $1.34_{\rm -0.96}^{+1.11}$ 225.9 (65.8%) $4.32\times10^{-2}$
006 $1.04_{\rm -0.20}^{+0.25}$ $1.00_{\rm -0.14}^{+0.16}$ 1.04 (83) 4.78
006 Flare 1 $0.85_{\rm -0.32}^{+0.46}$ $0.94_{\rm -0.28}^{+0.31}$ 0.66 (17) 8.68
006 Flare 2 $1.11_{\rm -0.49}^{+0.79}$ $0.91_{\rm -0.32}^{+0.42}$ 1.16 (25) 8.32
006 Flare 3 $0.83_{\rm -0.42}^{+0.62}$ $0.82_{\rm -0.40}^{+0.44}$ 0.93 (10) 11.1
006 Flare 4 $0.88_{\rm -0.31}^{+0.38}$ $1.03_{\rm -0.31}^{+0.32}$ 623.6 (39.0%) 4.86
006 Flare 5 $2.02_{\rm -0.79}^{+1.01}$ $1.51_{\rm -0.53}^{+0.58}$ 436.0 (54.6%) 2.75
007-008 $1.75_{\rm -0.83}^{+1.03}$ $1.94_{\rm -0.60}^{+0.64}$ 518.3 (66.0%) $2.22\times10^{-1}$
009-012 $1.04_{\rm -0.36}^{+0.47}$ $1.48_{\rm -0.35}^{+0.39}$ 576.9 (53.6%) $8.82\times10^{-2}$
007-012 $1.86_{\rm -0.44}^{+0.68}$ $1.92_{\rm -0.38}^{+0.43}$ 1.09 (18) $1.40\times10^{-1}$
007-018 $2.04_{\rm -0.50}^{+0.62}$ $2.08_{\rm -0.37}^{+0.41}$ 1.19 (19) $5.96\times10^{-2}$
a Last three digits of observation numbers, see Table 1, Col. 1.
b Luminosity in the 1-10 keV band in units of 1035 erg s-1 obtained from the spectral fits.
c Cash statistics (C-stat) and percentage of Monte Carlo realizations that had statistic <C-stat. We performed 104 simulations.

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