the NGC 4636 observations by assuming the same surface brightness and spectral parameters as those of the 3.2$^{\circ}$ offset region.

[ccccccc]{}\
& & &\
& 1.29 & & 40.0\
\
& & &\
& $kT$ (keV) & normalization$^{\S}$ & $kT$ (keV) & normalization$^{\S}$ & reduced-$\chi^2$ (d.o.f.)\
& 0.326$\pm$0.013 & 2.31$\pm$0.37 & 0.094$\pm$0.004 & 2.02$\pm$0.84 & 1.48 (206)\
\
\
\
\
\
\
\

[c]{}

Spectral Fitting
----------------

We fitted the spectra of each region of NGC 4636, based on the above estimation of the NXB, the CXB, and the GXE. The CXB and the GXE are included as models in the spectral fit with their spectral parameters fixed, and the NXB was subtracted. We applied a two-component model for the emission from NGC 4636 : a single-temperature vAPEC model for the ISM, and a BREMSS model with a temperature fixed to 7 keV (Matsushita et al. 1994) for the hard component due to low-mass X-ray binaries (LMXB). For the all regions, the fitting is performed in the energy range of 0.3–5 keV because the spectrum below 0.3 keV is difficult to analyze due to large systematic errors, and the NXB dominates above 5 keV. The energy range around the 