0.861 & 4.98$\pm$0.23 & 1.03$\pm$0.07\
Fe ${\rm_{XX}}$ & 0.961 & - & & & & &\
Fe ${\rm_{XX}}$ & 0.963 & - & - & - & 0.962 & 1.73$\pm$0.15 & 0.36$\pm$0.04\
Mg ${\rm_{XI}}$ & 1.35 & 0.59 & 0.59 & 0.070 & 1.35 & 0.61$\pm$0.04 & 0.13$\pm$0.01\
\

[c]{}

Discussion
==========

We measured the temperature and metal abundance distributions of NGC 4636 out to 28’ and confirmed the resonance scattering in the central region. In this section we compare the Suzaku results with those for other X-ray bright elliptical galaxies (NGC 1399, NGC 507, and NGC 5044), and discuss the metal enrichment process in elliptical galaxies.

Metallicity Distribution
------------------------

In Figures 4 and 5, observational results by the Suzaku XIS for NGC 1399 (Matsushita et al. 2007a) are also shown. These are the results with a two-temperature model within 4’ and one-temperature model beyond 4’. The temperature of NGC 1399 is about twice as high as that of NGC 4636, indicating that the gravitational potential of NGC 1399 is deeper. In Figure 5, the Ne abundance of NGC 1399 was not measured because its line was polluted by Fe-L lines. The radial distributions of the O, Mg, Si and 