  Many years ago we have introduced into general relativity, {\bf GR}, the
canonical superenergy tensors, $S_i^{~k}$, and the canonical angular
supermomentum tensors, $S^{ikl}=(-)S^{kil}$, matter and gravitation. We have
obtained these tensors by special averaging of the differences of the canonical
energy-momentum and canonical angular momentum. The averaging was performed in
Riemann normal coordinates, {\bf RNC(P)}; {\bf P} is beginning of these
coordinates. About four years ago we have observed that these tensors can also
be obtained in other, simpler way, by using the canonical superenergy and
angular super momentum complexes, $_K S_i^{~k}$, and, $_K S~^{ikl}=(-)_K
S^{kil}$, respectively. Such complexes can be introduced into {\bf GR} in a
natural way starting from canonical energy-momentum and angular momentum
complexes.
  In this paper, at first, we define the canonical superenergy and angular
supermomentum complexes in {\bf GR} and then, we apply them to analyze of a
closed system, {\bf CS}, Trautman's radiative spacetimes, {\bf TRS}, and
Friedman universes, {\bf FU}. Finally, we compare these complexes and the
results obtained with their help with the canonical superenergy and angular
supermomentum tensors and results obtained with them in past. In Appendix, for
convenience, we summarize our old approach to canonical superenergy and angular
supermomentum tensors.
