  Magnetized radio filaments are found in abundance in the inner few hundred pc
of our Galaxy. Progress in understanding this population of filaments has been
slow, in part due to a lack of detection elsewhere in the Galaxy or in external
galaxies. Recent highly sensitive radio continuum observations of radio
galaxies in galaxy clusters have revealed remarkable isolated filamentary
structures in the ICM that are linked to radio jets, tails and lobes. The
origin of this class of filaments is not understood either. Here, we argue that
the underlying physical mechanisms responsible for the creation of the two
populations are the same because of their similarity in morphology, spacing
between the filaments, aspect ratio, magnetic energy densities to thermal
pressure of the medium, and that both populations have undergone synchrotron
aging. These similarities provide an opportunity to investigate the physical
processes in the ISM and ICM for the first time. We consider that the origin of
the filaments in both the GC and ICM is a result of the interaction of a
large-scale wind with clouds, or the filaments arise through the stretching and
collection of field lines by turbulence in weakly magnetized medium. We examine
these ideas toward four radio galaxy filaments associated with four radio
galaxies IC 40B, IC 4496, J1333-3141, ESO137-006 and argue that much can be
understood in the future by comparing these two populations of filaments.
