We examine metal and entropy content in galaxy groups having T _ { X } \approx 0.5 - 2 keV in cosmological hydrodynamic simulations .
Our simulations include a well-constrained prescription for galactic outflows following momentum-driven wind scalings , and a sophisticated chemical evolution model .
Our simulation with no outflows reproduces observed iron abundances in X-ray emitting gas , but the oxygen abundance is too low ; including outflows yields iron and oxygen abundances in good agreement with data .
X-ray measures of [ O/Fe ] primarily reflect metal distribution mechanisms into hot gas , not the ratio of Type Ia to Type II supernovae within the group .
Iron abundance increases by \sim \times 2 from z \sim 1 \rightarrow 0 independent of group size , consistent with that seen in clusters , while [ O/Fe ] drops by \sim 30 % .
Core entropy versus temperature is elevated over self-similar predictions regardless of outflows due to radiative cooling removing low-entropy gas , but outflows provide an additional entropy contribution below 1 keV .
This results in a noticeable break in the L _ { X } - T _ { X } relation below \sim 1 keV , as observed .
Entropy at R _ { 500 } is also in good agreement with data , and is unaffected by outflows .
Importantly , outflows serve to reduce the stellar content of groups to observed levels .
Specific energy injection from outflows drops with group mass , and exceeds the thermal energy for \la 0.5 keV systems .
Radial profiles from simulations are in broad agreement with observations , but there remain non-trivial discrepancies that may reflect an excess of late-time star formation in central group galaxies in our simulations .
Our model with outflows suggests a connection between physical processes of galaxy formation and both pre-heating and enrichment in intragroup gas , though more definitive conclusions must await a model that simultaneously suppresses cooling flows as observed .