Spectrum fitted with three-component models (LHB+CGM+CXB) assuming different metal abundances. The red, blue, magenta, and black solid lines show the contribution from the local hot bubble, the circumgalactic medium, the cosmic X-ray background, and instrumental background, respectively. The dotted lines show the various contributions to the instrumental background. From top to bottom: Anders & Grevesse (1989); Wilms et al. (2000), and Lodders (2003) abundances are assumed. Assuming the Anders & Grevesse (1989) abundances, about half of the O VII line flux is due to the local hot bubble, while for later abundances the contribution to the O VII line drops significantly. Large residuals are present at the energy of the O VIII line and between ~ 0.7 and 1 keV.