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Table 2:

Best fit spectral parameters for the persistent, the shallow-dipping, and the deep-dipping spectra fit simultaneously with the ionized absorber model.
Parameter Per. emission   Shallow dip   Deep dip
$N_{\rm H}^{\rm fore} ~(10^{22}$ cm-2) $0.410 \pm 0.007$   $0.420 \pm 0.009$   $0.45 \pm 0.03$
Significance   1.4$\sigma$   1.7$\sigma$  
Photon index     $1.98 \pm 0.01$    
Norm. (photons  keV-1 cm-2 s-1)     $0.0124 \pm 0.0002$    
$\log(\xi)$ (erg  s-1 cm) 5.0 Frozen   $\rm 2.52_{-0.07}^{+0.05}$   $2.29 \pm 0.02$
Significance       5$\sigma$  
$N_{\rm H}^{\xi} ~(10^{22}$ cm-2) 0.32 Frozen   $\rm 4.3_{-0.5}^{+0.4}$   $\rm 11.6_{-0.6}^{+0.4}$
Significance       >10$\sigma$  
Reduced $\chi^{2} = 1.42$ for 765 d.o.f.
The photon index and the normalization of the power law are linked between persistent, shallow and deep dipping. $N_{\rm H}^{\rm fore}$ is the foreground neutral hydrogen column density. $\xi$ is the ionization parameter. $N_{\rm H}^{\xi}$ is the warm absorber hydrogen column density. These parameters are allowed to vary to explain the spectral changes from persistent to deep dipping. Uncertainties are given at a 90% confidence level. We also indicate the significance of the change of $N_{\rm H}^{\rm fore}$ between the three spectra as well as the significance of the change of $\log(\xi)$ and $N_{\rm H}^{\xi}$ between shallow and deep-dipping spectra.

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