| Abstract
| - We study the kinematic properties of the ionised gas outflows and ambient interstellar medium (ISM) in a large and representative sample of local luminous and ultra-luminous infrared galaxies (U/LIRGs) (58 systems, 75 galaxies) at galactic and sub-galactic (i.e., star-forming clumps) scales, thanks to integral field spectroscopy (IFS)-based high signal-to-noise integrated spectra. The velocity dispersion of the ionized ISM in U/LIRGs ( ⟨ σ ⟩ ~ 70 km s -1) is larger than in lower luminosity local star-forming galaxies ( ⟨ σ ⟩ ~ 2 5 km s -1). While for isolated disc LIRGs star formation appears to sustain turbulence, gravitational energy release associated with interactions and mergers plays an important role in driving σ in the U/LIRG range. We find that σ has a dependency on the star formation rate density ( Σ SFR), which is weaker than expected if it were driven by the energy released by the starburst. The relatively small role of star formation (SF) driving the σ in U/LIRGs is reinforced by the lack of an increase in σ associated with high luminosity SF clumps. We also find that the impact of an active galactic nucleus (AGN) in ULIRGs is strong, increasing on average σ by a factor 1.5. Low- z U/LIRGs cover a range of velocity dispersion ( σ ~ 30 to 100 km s -1) and star formation rate density ( Σ SFR ~ 0. 1 to 20 M⊙ yr -1 kpc -2) similar to those of high- z SFGs. Moreover, the observed weak dependency of σ on Σ SFR for local U/LIRGs (σ ∝ Σ SFR+0.06) is in very good agreement with that measured in some high- z samples. The presence of ionized gas outflows in U/LIRGs seems universal based on the detection of a broad, usually blueshifted, H α line. The observed dependency of the maximum velocity of the outflow ( Vmax) on the star formation rate (SFR) is of the type Vmax( non − AGN) ∝ SFR( LIR) + 0.24. We find that AGNs in U/LIRGs are able to generate faster ( ~×2) and more massive ( ~× 1.4) ionized gas outflows than pure starbursts. The derived ionized mass loading factors ( η) are in general below 1, with only a few AGNs above this limit. The escaping gas fraction is low with only less massive (log( Mdyn/ M⊙) < 10.4 ) U/LIRGs having outflowing terminal velocities higher than their escape velocities, and more massive galaxies retaining the gas, even if they host an AGN. The observed average outflow properties in U/LIRGs are similar to high- z galaxies of comparable SFR. However, while high- z galaxies seem to require Σ SFR> 1 M⊙ yr -1 kpc -2 for launching strong outflows, this threshold is not observed in low- z U/LIRGs even after correcting for the differential fraction of the gas content. In the bright SF clumps found in LIRGs, ionized gas outflows appear to be very common (detection rate over 80%). Their observed properties are less extreme than those associated with the entire galaxy. The clumps in LIRGs follow the general size-L- σ scaling relations found for low- and high- z clumps, though they are in general smaller, less luminous, and are characterized by lower σ than at high- z. For a given observed (no internal extinction correction applied) star formation surface density, outflows in LIRG clumps would be about one to two orders of magnitude less energetic than the outflows launched by clumps in high- z SF galaxies.
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