al. 2006; Humphrey et al. 2006). In addition, observations by XMM-Newton have suggested similar metal abundance patterns to those in the centers of clusters or groups of galaxies (e.g., Matsushita et al. 2003; Matsushita et al. 2007b). The excellent energy resolution of XMM-Newton RGS has been used to precisely measure metal abundances (e.g., Xu et al. 2002; Tamura et al. 2003) and show that Si and Fe abundances in the central region are similar, while the O abundance is in general about half that of Fe. To understand metal enrichment processes, measurements of O, Ne, or Mg abundances in the outer regions are needed. To unambiguously constrain the O abundance in elliptical galaxies it is also necessary to have an accurate estimate of the foreground Galactic thermal emission. The best detector to satisfy these conditions is the Suzaku XIS which has a better energy resolution and a lower background than any previous X-ray CCD camera. The launch of the Suzaku XIS (Koyama et al. 2007) with high energy resolution in the lower energy X-ray band allows us to obtain O and Mg abundance distributions through accurate measurements of their emission lines. Past studies (e.g., NGC1399 ; Matsushita et al. 2007a, 