  Angular momentum (AM) is a key parameter to understand galaxy formation and
evolution. AM originates in tidal torques between proto-structures at turn
around, and from this the specific AM is expected to scale as a power-law of
slope 2/3 with mass. However, subsequent evolution re-shuffles this through
matter accretion from filaments, mergers, star formation and feedback, secular
evolution and AM exchange between baryons and dark matter. Outer parts of
galaxies are essential to study since they retain most of the AM and the
diagnostics of the evolution. Galaxy IFU surveys have recently provided a
wealth of kinematical information in the local universe. In the future, we can
expect more statistics in the outer parts, and evolution at high z, including
atomic gas with SKA.
