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We report results from deep Suzaku and mostly snapshot Chandra observationsof four nearby galaxy groups: MKW4, Antlia, RXJ1159+5531, and ESO3060170. Theirpeak temperatures vary over 2-3 keV, making them the smallest systems with gasproperties constrained to their viral radii. The average Fe abundance in theoutskirts (R $>$ 0.25R$_{200}$) of their intragroup medium (IGrM) is $Z_{\rmFe}=0.309\pm0.018$ $Z_\odot$ with $\chi^2$ = 14 for 12 degrees of freedom,which is remarkably uniform and strikingly similar to that of massive galaxyclusters, and is fully consistent with the numerical predictions from theIllustrisTNG cosmological simulation. Our results support an early-enrichmentscenario among galactic systems over an order of magnitude in mass, even beforetheir formation. When integrated out to R$_{200}$, we start to see a tensionbetween the measured Fe content in ICM and what is expected from supernovaeyields. We further constrain their O, Mg, Si, S, and Ni abundances. Theabundance ratios of those elements relative to Fe are consistent with thepredictions (if available) from IllustrisTNG. Their Type Ia supernovae fractionvaries between 14%-21%. A pure core collapsed supernovae enrichment at groupoutskirts can be ruled out. Their cumulative iron-mass-to-light ratios withinR$_{200}$ are half that of the Perseus cluster, which may imply that galaxygroups do not retain all of their enriched gas due to their shallowergravitational potential wells, or that groups and clusters may have differentstar formation histories.

Chemical abundances in the outskirts of nearby galaxy groups measured with joint Suzaku and Chandra observations