given in section 5.

Throughout this paper, we use a Hubble constant value of $H_{0}$ = 70 km s$^{-1}$Mpc$^{-1}$ or $h_{100}$ = 0.7 (1 arcmin $\simeq$ 5 kpc), and a virial radius of [*r*]{}$_{180}$ = 1.95$h^{-1}_{100}$ $\sqrt[]{\mathstrut k{\langle T\rangle}/10{\rm keV}}$ Mpc (Markevitch et al. 1998) where $kT$ is the gas temperature. The Galactic hydrogen column density is $N_{\rm H}$ = 1.8$\times$10$^{20}$ cm$^{-2}$ in the direction of NGC 4636 (Stark et al. 1992). We use the Anders and Grevesse (1989) definition of Solar abundance ratios for easier comparison with other Suzaku papers which use this definition. Other recent papers often use instead Grevesse and Sauval (1998). The former has 26% and 48% higher abundances for O and Fe, respectively. All errors are given as a 90% confidence range.

Observation and Data Reduction
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A pointing observation of NGC 4636 by Suzaku was carried out on December 6–7, 2005 for about 70 ks. In order to measure metal abundances in the outer region of NGC 4636, a 10’ north offset observation was carried out on December 7–9, 2007. Another north-west offset observation at 3.2$^{\circ}$ away from the NGC 4636 center was also carried out on June 17–18, 2007 to estimate the foreground 