Dispersal of Galactic Magnetic Fields into Intracluster Space
  Little is known about the origin and basic properties of magnetic fields in
clusters of galaxies. High conductivity in magnetized interstellar plasma
suggests that galactic magnetic fields are (at least partly) ejected into
intracluster (IC) space by the same processes that enrich IC gas with metals.
We explore the dispersal of galactic fields by hydrodynamical simulations with
our new {\em Enzo-Galcon} code, which is capable of tracking a large number
galaxies during cluster assembly, and modeling the processes that disperse
their interstellar media. Doing so we are able to describe the evolution of the
mean strength of the field and its profile across the cluster. With the known
density profile of dispersed gas and an estimated range of coherence scales, we
predict the spatial distribution of Faraday rotation measure and find it to be
consistent with observational data.
