the gas mass distribution (Figure 10). The stellar light distribution is quoted from Fukazawa et al. (2006).

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Figure 11(a) shows that the O and Fe mass distributions are similar between the two galaxies and the metal mass of NGC 4636 is almost the same as that of NGC 1399 at all radii. Combining this with the difference of the gas mass, it can be understood that the abundance and the gas mass of NGC 4636 are about twice and half those of NGC 1399, respectively. As seen in Figure 11(b), MLR of NGC 4636 is also 2$\sim$3 times larger than that of NGC 1399 in all regions for both metals. This indicates that the metals in the ISM are distributed more compactly in NGC 4636; the metals in NGC 4636 do not diffuse so widely. This difference might be caused by environmental effects; galaxy interaction is frequent for NGC 1399 and thus metal-rich gas could be stirred by galaxy motions.

Finally, we compared the MLR of NGC 4636 with Suzaku results of other groups and clusters. These objects are galaxy groups centered on NGC 1399, NGC 5044, and NGC 507. They are X-ray bright elliptical galaxies like NGC 