lines considered here are listed in Table 4. Since the XIS cannot resolve individual lines, we summed the flux of neighboring lines within 30 eV in the RGS paper (Xu et al. 2002), and assumed the strength-weighted line energy. Furthermore, we refer to the ATOMDB line table [^2] for the energy and intensity of the 0.961 and 0.963 keV lines, which were not analyzed in the RGS spectrum, but are significant in the XIS spectra. The Ne lines around this energy range are not shown because their fluxes are not reliable due to the influence of Fe-L lines. The line width of all lines is fixed to 0 keV.

The line intensity ratio against the summed flux of the strongest line (0.737 and 0.728 keV ) of Fe ${\rm_{XV\hspace{-.1em}I\hspace{-.1em}I}}$ is summarized in Table 4 and Figure 8. In Figure 8, the predicted line intensity ratios are also shown. These were obtained by simulating spectra with the emission models and parameters from Table 3 and fitting them with the same model used for the data. The result indicates that the flux intensity of the Fe ${\rm_{XV\hspace{-.1em}I\hspace{-.1em}I}}$ line (0.825 keV), which was suggested to be affected by resonance scattering (Xu et al. 