assumes that the emission is uniform within 20’. Finally, we estimated the GXE, using the 3.2$^{\circ}$ offset observation by extracting spectra within 8’ ($\simeq$ 40 kpc) of the center of the field of view. We used a uniform-sky ARF as for the CXB estimation. The GXE consists of a Local Hot Bubble (LHB) component and a Milky Way Halo (MWH) component. These have temperatures of approximately $\sim$0.08 keV and $\sim$0.2–0.3 keV, respectively (e.g., Lumb et al. 2002). We fitted the GXE spectrum with a two-temperature APEC model, where temperatures are set to be free and metal abundances are fixed to one solar. At these temperatures, the continuum emission is vanishingly small compared to the line emission. Therefore, even if this assumption for metal abundance is not completely correct, the estimation of the GXE will not change significantly. The results of the fit are shown in table 2, along with the fixed parameter values used for the CXB model. Figure 2 shows the best fit model and spectra. The temperatures obtained are consistent within errors with the results from the ROSAT-PSPC all-sky survey (Kuntz & Snowden 2000). Using the best-fit parameters, we modeled the Galactic emission in each spectral region of 