NGC 5044 ; Komiyama et al. 2008) have shown that the O to Fe abundance ratio, which can be used to estimate the number ratio of Ia to II supernovae, is about 0.6–0.8 solar in all regions. However, observations in the outer regions, where metals ejected from galaxies have remained, are still poor. So far, Suzaku measurements of abundance distribution have been reported for three elliptical galaxies. NGC 5044 and NGC 507 exhibit a steeper radial O abundance profile than NGC 1399 while there is a large scatter among their O mass-to-light ratios. (Matsushita et al. 2007a; Komiyama et al. 2009; Sato et al. 2009a). Studies of these properties in additional galaxies will thus aid understanding of metal enrichment processes.

In this paper, we report the results of spectral analysis of NGC 4636 observed by the XIS detector onboard Suzaku (Mitsuda et al. 2007). NGC 4636 (z = 0.00313; $\simeq$ 17 Mpc, Smith et al. 2000) is an X-ray bright elliptical galaxy belonging to the Virgo cluster. Metal-enriched hot gas is extended over the entire galaxy group (Matsushita et al. 1998). This galaxy is located at the south end of the cluster, where the X-ray emission from the Virgo center 