the hard X-ray component of the BREMSS model is 1.5$\times$10$^{40}$ erg s$^{-1}$ over 2–10 keV within 6’ of NGC 4636. This is consistent with the ASCA results (Matsushita et al. 1994), indicating that the hard X-ray component is due to LMXB. We also confirmed that the abundance results are almost the same when we fit the hard component with a power-law of index 1.5, which was used for the LMXB estimation in Loewenstein et al. (2001). In the central region, the reduced-$\chi^2$ is a little larger than that in the outer region. This might be due to temperature structure in the center region (Ohto et al. 2003) so we tried fitting with a two-temperature model only in the 0–2’ region. We assumed that the metal abundances are the same for both temperature components. Comparing the result with that of the single-temperature model, the metal abundances do not greatly change and the temperature of the hot component in the two-temperature model is almost the same as that in the single-temperature. The F-test probability is 0.097% and thus the improvement is marginal. Therefore, hereafter we focus on the results with the single-temperature model. A fit residual around 0.7 keV in the 0–2’ 