  The morphology of tailed radio galaxies is an invaluable source of
environmental information, in which a history of the past interactions in the
intra-cluster medium, such as complex galaxy motions and cluster merger shocks,
are preserved. In recent years, the use of tailed radio galaxies as
environmental probes has gained momentum as a method for galaxy cluster
detection, examining the dynamics of individual clusters, measuring the density
and velocity flows in the intra-cluster medium, and for probing cluster
magnetic fields. To date instrumental limitations in terms of resolution and
sensitivity have confined this research to the local (z < 0.7) Universe. The
advent of SKA1 surveys however will allow detection of roughly 1,000,000 tailed
radio galaxies and their associated galaxy clusters out to redshifts of 2 or
more. This is in fact ten times more than the current number of known clusters
in the Universe. Additionally between 50,000 and 100,000 tailed radio galaxies
will be sufficiently polarized to allow characterization of the magnetic field
of their parent cluster. Such a substantial sample of tailed galaxies will
provide an invaluable tool not only for detecting clusters, but also for
characterizing their intra-cluster medium, magnetic fields and dynamical state
as a function of cosmic time. In this chapter we present an analysis of the
usability of tailed radio galaxies as tracers of dense environments
extrapolated from existing deep radio surveys.
