  We study the kinematic properties of the ambient ionized ISM and ionized gas
outflows in a large and representative sample of local luminous and
ultraluminous infrared galaxies (U/LIRGs) (58 systems, 75 galaxies), on the
basis of integral field spectroscopy (IFS)-based high S/N integrated spectra at
galactic and sub-galactic, i.e. star forming (SF) clumps, scales.
  Ambient ionized gas. The velocity dispersion of the ionized ISM in U/LIRGs
(<sigma> ~ 70 kms-1) is larger than in lower luminosity local star forming
galaxies (<sigma> ~ 25 kms-1). While for isolated disc LIRGs star formation
appears to sustain turbulence, gravitational energy release associated to
interactions and mergers plays an important role driving sigma in the U/LIRG
range. We also find that the impact of an AGN in ULIRGs is strong, increasing
sigma by a factor 1.5 on average. The observed weak dependency of sigma with
SFR surface density for local U/LIRGs is in very good agreement with that
measured in some high-z samples.
  Ionized outflows. The presence of ionized gas outflows in U/LIRGs seems
universal based on the detection of a broad, usually blueshifted, Halpha line.
AGNs in U/LIRGs are able to generate faster (x2) and more massive (x1.4)
ionized gas outflows than pure starbursts. The derived ionized mass loading
factors are in general below one, with only a few AGNs above this limit. Only a
small fraction of the ionized material from low mass LIRGs (log(Mdyn/Msun) <
10.4) could reach the intergalactic medium, with more massive galaxies
retaining the gas. The observed average outflow properties in U/LIRGs are
similar to high-z galaxies of comparable SFR. In the bright SF clumps found in
LIRGs, ionized gas outflows appear to be very common. For a given SFR surface
density, outflows in LIRG clumps would be about one to two orders of magnitude
less energetic than those launched by clumps in high-z SF galaxies.
