Spectrum of a large region inside the NPS (red points) in comparison with the typical "Milky Way" spectrum well outside the NPS (black points). Contributions of the detector background and CXB have been subtracted. The blue and green lines illustrate a few characteristic models. The solid blue line shows the APEC spectrum with the temperature T_w = 0.16 keV and abundance Z/Z_⊙ = 0.05, using the abundance ratios from Asplund et al. (2009). The dashed blue line shows the same model with a three times larger abundance, i.e., Z/Z_⊙ = 0.15. The solid green line shows the APEC model with the temperature T_h = 0.5 keV, Z/Z_⊙ = 0.05, and the emission measure multiplied by a factor of (T_w/T_h)². The dashed green line shows the same model with Z/Z_⊙ = 0.7. A comparison of the histograms and the dashed lines shows that overabundances in the range 3-10 are needed to reproduce the enhanced brightness of the NPS compared to the Galaxy (assuming comparable pressures and linear sizes of the emitting regions).