Distribution and Evolution of Metals in the Magneticum simulations
  Metals are ideal tracers of the baryonic cycle within halos. Their
composition is a fossil record connecting the evolution of the various stellar
components of galaxies to the interaction with the environment by in- and
outflows. The Magneticum simulations allow to study halos across a large range
of masses and environments, from massive galaxy clusters containing hundreds of
galaxies down to isolated field galaxies. They include a detailed treatment of
the chemo-energetic feedback from the stellar component and its evolution as
well as feedback from the evolution of supermassive black holes. Following the
detailed evolution of various metal species and their relative composition due
to continuing enrichment of the IGM and ICM by SNIa, SNII and AGB winds of the
evolving stellar population reveals the complex interplay of local star
formation processes, mixing, global baryonic flows, secular galactic evolution
and environmental processes. We present results from the Magneticum simulations
on the chemical properties of simulated galaxies and galaxy clusters, carefully
comparing them to observations. We show that the simulations already reach a
very high level of realism within their complex descriptions of the
chemo-energetic feedback, successfully reproducing a large number of observed
properties and scaling relations. Our simulated galaxies clearly indicate that
there are no strong secondary parameters (like star formation rates at fixed
redshift) driving the scatter in these scaling relations. The remaining
differences clearly point to detailed physical processes which have to be
included into future simulations.
