  Aims. The goal of this work is to devise a description of the enrichment
process in large-scale structure that explains the available observations and
makes predictions for future measurements. Methods. We took a spartan approach
to this study, employing observational results and algebra to connect stellar
assembly in star-forming halos with metal enrichment of the intra-cluster and
group medium. Results. On one hand, our construct is the first to provide an
explanation for much of the phenomenology of metal enrichment in clusters and
groups. It sheds light on the lack of redshift evolution in metal abundance, as
well as the small scatter of metal abundance profiles, the entropy versus
abundance anti-correlation found in cool core clusters, and the so-called Fe
conundrum, along with several other aspects of cluster enrichment. On the other
hand, it also allows us to infer the properties of other constituents of
large-scale structure. We find that gas that is not bound to halos must have a
metal abundance similar to that of the ICM and only about one-seventh to
one-third of the Fe in the Universe is locked in stars. A comparable amount is
found in gas in groups and clusters and, lastly and most importantly, about
three-fifths of the total Fe is contained in a tenuous warm or hot gaseous
medium in or between galaxies. We point out that several of our results follow
from two critical but well motivated assumptions: 1) the stellar mass in
massive halos is currently underestimated and 2) the adopted Fe yield is only
marginally consistent with predictions from synthesis models and SN rates.
Conclusions. One of the most appealing features of the work presented here is
that it provides an observationally grounded construct where vital questions on
chemical enrichment in the large-scale structure can be addressed. We hope that
it may serve as a useful baseline for future works.
