We present an analysis of the iron abundance in the hot gas surrounding galaxy groups and clusters .
To do this , we first compile and homogenise a large dataset of 79 low-redshift ( \left|z \right| = 0.03 ) systems ( 159 individual measurements ) from the literature .
Our analysis accounts for differences in aperture size , solar abundance , and cosmology , and scales all measurements using customised radial profiles for the temperature ( T ) , gas density ( \rho _ { \textnormal { gas } } ) , and iron abundance ( Z _ { \textnormal { Fe } } ) .
We then compare this dataset to groups and clusters in the L-Galaxies galaxy evolution model .

Our homogenised dataset reveals a tight T - Z _ { \textnormal { Fe } } relation for clusters , with a scatter in Z _ { \textnormal { Fe } } of only 0.10 dex and a slight negative gradient .
After examining potential measurement biases , we conclude that at least some of this negative gradient has a physical origin .
Our model suggests greater accretion of hydrogen in the hottest systems , via stripping of gas from infalling satellites , as a cause .
At lower temperatures , L-Galaxies over-estimates Z _ { \textnormal { Fe } } in groups , indicating that metal-rich gas removal ( via e.g . AGN feedback ) is required .

L-Galaxies provides a reasonable match to the observed Z _ { \textnormal { Fe } } in the intracluster medium ( ICM ) of the hottest clusters from at least z \sim 1.3 to 0.3 .
This is achieved without needing to modify any of the galactic chemical evolution ( GCE ) model parameters .
However , the Z _ { \textnormal { Fe } } in intermediate- T clusters appears to be under-estimated in our model at z = 0 .
The merits and problems with modifying the GCE modelling to correct this are discussed .