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NGC 4636, an X-ray bright elliptical galaxy, was observed for 70 ks withSuzaku. The low background and good energy resolution of the XIS enable us toestimate the foreground Galactic emission accurately and hence measure, for thefirst time, the O, Mg, Si and Fe abundances out to a radius of ~28 arcmin($\simeq$ 140 kpc). These metal abundances are as high as $>$1 solar within thecentral 4' and decrease by ~50% towards the outer regions. Further, the O to Feabundance ratio is about 0.60--1.0 solar in all regions analyzed, indicatingthat the products of both SNe II and SNe Ia have mixed and diffused to theouter regions of the galaxy. The O and Fe metal mass-to-light-ratios (MLR) ofNGC 4636 are 2--3 times larger than those of NGC 1399 implying that metaldistributions in NGC 4636 are less extended than those in NGC 1399, possiblydue to environmental factors, such as frequency of galaxy interaction. We alsofound that the MLRs of NGC 4636 at 0.1 $r_{180}$ are $\sim$5 times smaller thanthose of clusters of galaxies, possibly consistent with the correlation betweentemperature and MLR of other spherically symmetric groups of galaxies. We alsoconfirmed a resonant scattering signature in the Fe$_{XV II}}$ line in thecentral region, as previously reported using the XMM-Newton RGS.

Suzaku Observation of the Metallicity Distribution in the Elliptical Galaxy NGC 4636