Non-thermal emission from galaxy clusters: feasibility study with SKA1
  Galaxy clusters are known to host a variety of extended radio sources: tailed
radio galaxies whose shape is modelled by the interaction with the
intra-cluster medium (ICM); radio bubbles filling cavities in the ICM
distribution and rising buoyantly through the thermal gas; diffuse giant radio
sources ("halos" and "relics") revealing the presence of relativistic electrons
and magnetic fields in the intra-cluster volume. It is currently the subject of
an active debate how the non-thermal components that we observe at radio
wavelengths affect the physical properties of the ICM and depend on the
dynamical state of galaxy clusters. In this work we start our SKA1 feasibility
study of the "radio cluster zoo" through simulations of a typical radio-loud
cluster, hosting several bright tailed radio galaxies and a diffuse radio halo.
Realistic simulations of SKA1 observations are obtained through the MeqTrees
software. A new deconvolution algorithm, based on sparse representations and
optimised for the detection of faint diffuse astronomical sources, is tested
and compared to the classical CLEAN method.
