is negligible, so we can study the metal enrichment history of a giant elliptical galaxy (Matsushita et al. 1997). So far, observations by ASCA (Matsushita et al. 1997), Chandra (Ohto et al. 2003; Humphrey et al. 2006), and XMM-Newton (e.g. Xu et al. 2002) have been used to measure metal abundances. The temperature of hot gas in this galaxy is 0.6–0.7 keV, which is lower than the 1.0–1.5 keV of NGC 1399, NGC 507, and NGC 5044. Therefore, we can also discuss the temperature dependence of metal properties. In addition, NGC 4636 is quite isolated in comparison with the above 3 galaxies, and thus the comparison will aid investigations of environmental effects. We describe the observation and data reduction in section 2. Section 3 on the analysis and results describes the methods we used to estimate background and fit spectra as well as the resulting temperature and metallicity distributions. Additionally, we discuss the confirmation of resonance scattering in the Fe ${\rm_{XV\hspace{-.1em}I\hspace{-.1em}I}}$ line in the spectrum of the central region. In section 4, we discuss the O, Ne, Mg, Si abundance ratios to Fe, their distributions, the metal transport process, and resonance scattering of the Fe ${\rm_{XV\hspace{-.1em}I\hspace{-.1em}I}}$ line. A summary is 