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We studied the distributions of metal abundances and metal-mass-to-lightratios in the intracluster medium (ICM) of four galaxy groups, MKW 4, HCG 62,the NGC 1550 group, and the NGC 5044 group, out to 0.5 r180 observed withSuzaku. The Fe abundance decreases with radius, and about 0.2-0.4 solar beyond0.1 r180. At a given radius in units of r180, the Fe abundance in the ICM ofthe four galaxy groups were consistent or smaller than those of clusters ofgalaxies. The Mg/Fe and Si/Fe ratios in the ICM are nearly constant at thesolar ratio out to 0.5 r180. We also studied systematic uncertainties in thederived metal abundances comparing the results from two versions of atomic datafor astrophysicists (ATOMDB) and single- and two temperature model fits. Sincethe metals have been synthesized in galaxies, we collected K-band luminositiesof galaxies from Two Micron All Sky Survey catalogue (2MASS) and calculated theintegrated iron-mass-to-light-ratios (IMLR), or the ratios of the iron mass inthe ICM to light from stars in galaxies. The groups with smaller gas mass tolight ratios have smaller IMLR values and the IMLR inversely correlated withthe entropy excess. Based on these abundance features, we discussed the pasthistory of metal enrichment process in groups of galaxies.

Metal distributions out to 0.5 r180 in the intracluster medium of four galaxy groups observed with Suzaku