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Fig. 13


Mass outflow rate vs. nuclear SFR (left panel), outflow momentum rate vs. nuclear SFR (middle panel), and outflow kinetic luminosity vs. nuclear SFR (right panel). Red circles indicate nuclei with outflows launched by an AGN, green diamonds are objects hosting an AGN with molecular outflows of uncertain SF/AGN origin, and stars represent star-formation-dominated nuclei. The blue circles mark the ULIRGs presented in this work. The white stars are the lower luminosity starburts compiled by Cicone et al. (2014). The remaining points correspond to local U/ LIRGs from the literature: NGC 1614 and IRAS 17208–0014 (García-Burillo et al. 2015; Pereira-Santaella et al. 2015; Piqueras López et al. 2016); NGC 3256 N and S (Lira et al. 2002; Pereira-Santaella et al. 2011; Sakamoto et al. 2014; Emonts et al. 2014; Ohyama et al. 2015); ESO 320–G030 (Pereira-Santaella et al. 2016); Arp 220 W (Barcos-Muñoz et al. 2018); and NGC 6240 (Saito et al. 2018). The crosses at the lower right corners represent the typical error bars of the points. The black lines in the left panel correspond to mass loading factors, η = /SFR, of 1 and 10. The dashed orange line in the middle panel marks the total momentum injected by SNe as a function of the SFR. The dashed green lines indicate the L(SFR)/c ratio and ten times this value. The dashed orange lines in the right panel indicate the Lout = a × LSNe with a =1, 0.1, and 0.01 as function of the SFR. The solid red lines in the middle and right panels are the best linear fits to the star-formingobjects.

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