Notes.For the SINS galaxies studied in Shapiro et al. (2009) and Newman et al. (2012), the SFRs (i.e., ~100 M_⊙ yr^-1) are somewhat larger than our sample (~90 and 21 M_⊙ yr^-1, as derived from the infrared and Hα luminosities, respectively; though see effects due to reddening corrections in Sect. 2). The Harrison et al. (2012) sample is formed by ULIRGs with SFRs in the range ~300–1400 M_⊙ yr^-1 and therefore, significantly higher than local U/LIRGs. Similarly for Swinbank et al. (2004), who study a sample with average L_IR of ~10¹³ L_⊙, implying ~1000 M_⊙ yr^-1. Therefore, for these two works the comparison with local samples is less meaningful. Notes column: (1) Based on stacked integrated Hα spectra, (2) The values for the table are obtained by averaging of their high- and low-SFR bins. (3) Swinbank et al. 2004 only consider two components for Hα, not for the [NII] lines. (4) Based on integrated [OIII] lines. (5) For sake of homogeneity we compare with the galaxy integrated data (four sources), though Harrison et al. also provide IFU results.The smearing of the velocity field is not removed. The mean values have been obtained from Table 3 in Harrison et al., excluding a third redshifted component by +1350 km s^-1 detected in one of their sources.