Introduction

The distribution of relativistic electrons as well as the morphology of uniform and random magnetic fields in galactic halos are strongly affected by dynamical processes in the underlying disk. During the evolution of a galaxy, ongoing star formation leads to subsequent supernova explosions and the creation of superbubbles. These processes may cause the transport of high-energetic particles and small-scale turbulences away from the star forming regions into the disk-halo interface and to high galactic latitudes. As a consequence, the magnetic field properties as well as the spectral distribution of the emission is expected to be different in galaxies of differing star forming activity.

Edge-on galaxies are ideal candidates for observing these effects using radio continuum and polarization measurements at cm-wavelengths, where the emission is mainly due to relativistic electrons gyrating around magnetic field lines. Especially the combination of observations at different wavelengths provide useful information necessary to understand the various relationships between star-formation in the disk and its consequences on the interstellar medium.