Table 2: Best-fitting parameters for the spectral fits of the core emission.
Model(a) $N^{{(b)}}_{\rm H(gal.)}$ kT Z(c) $N^{{(d)}}_{\rm H(torus)}$ $\Gamma^{{(e)}}$ $F_{\rm abs}^{{(f)}}$ $F_{\rm unabs}^{{(g)}}$ $\chi^2_{\rm red}$ ($\chi^2$/d.o.f.)
  [1022 cm-2] [keV]   [1022 cm-2]   [erg s-1 cm-2] [erg s-1 cm-2]  
Ia $\rm0.66^{+0.07}_{-0.07}$ $\rm0.44^{+0.07}_{-0.06}$ 1* $\rm0.74^{+0.56}_{-0.39}$ $\rm0.30^{+0.10}_{-0.08}$ $2.3\times 10^{-12}$ $3.3\times 10^{-12}$ 0.84 (15.9/19)
Ib 0.49* 0.48* 1* $\rm0.54^{+0.46}_{-0.34}$ $\rm0.20^{+0.10}_{-0.08}$ $2.3\times 10^{-12}$ $ 2.9\times 10^{-12}$ 0.76 (16.0/21)
Ic 0.49* 0.48* 0.25* $\rm0.84^{+0.55}_{-0.39}$ $\rm0.28^{+0.09}_{-0.09}$ $2.3\times 10^{-12}$ $3.0\times 10^{-12}$ 0.74 (15.8/21)

IIa		 $\rm0.51^{+0.09}_{-0.04}$ $\rm0.28^{+0.03}_{-0.04}$ 1* $\rm0.45^{+0.59}_{-0.21}$ $\rm0.22^{+0.13}_{-0.05}$ $2.5\times 10^{-12}$ $3.4\times 10^{-12}$ 0.89 (16.8/19)
IIb 0.41* 0.41* 1* $\rm0.62^{+0.46}_{-0.37}$ $\rm0.23^{+0.06}_{-0.09}$ $2.3\times 10^{-12}$ $2.8\times 10^{-12}$ 0.77 (16.1/21)
IIc 0.41* 0.41* 0.25* $\rm0.82^{+0.42}_{-0.42}$ $\rm0.27^{+0.07}_{-0.11}$ $2.2\times 10^{-12}$ $2.8\times 10^{-12}$ 0.78 (16.4/21)
* Fixed value; a I: (R&S + PL $^{\rm abs}$) $^{\rm abs}$, II: (M&K + PL $^{\rm abs}$) $^{\rm abs}$, (R&S $^{\rm abs}$: absorbed Raymond/Smith plasma, M&K $^{\rm abs}$: absorbed Mewe/Kaastra plasma, PL $^{(\rm abs)}$: (absorbed) power-law; b column density of the diffuse absorber; c metallicity (referring to the solar value); d column density of the compact absorber; e photon index; f absorbed X-ray flux between 0.2 keV and 8.0 keV; g unabsorbed X-ray flux between 0.2 keV and 8.0 keV, i.e., $N^{{(b)}}_{\rm H(gal.)}$ and  $N^{{(d)}}_{\rm H(torus)}$ are set to 0.


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