  We probe the role of the directional asymmetry between relativistic outflows
to kilo-parsec scale jets in the propagation and acceleration of cosmic rays.
Our sample contains powerful AGN hosting dense cluster environments. We attempt
a thorough description of where and when ultra high energy cosmic ray
production and acceleration takes place also using radio observations of the
large scale stucture of the AGNs and X-ray data of the hot dense gas in which
the AGNs are situated.
  As far as the cosmic ray primaries are concerned, the presence of
relativistic protons or mildly relativistic electrons/positrons contributes
substantially to the energy budget of the jets enabling them to heat
efficiently the intracluster gas.
