Left: mass of the gas with a higher velocity dispersion ([OIII] W70 >  300 km s⁻¹) as a function of the jet kinetic power. The black dots mark the ionized mass measurements from Venturi et al. (2021) for local Seyfert galaxies, while the colored symbols are our estimates for the ionized mass of the ionized gas in our sample. The stars are used for targets in which the higher velocity dispersion perpendicular to the jet is clearly observed, and the less transparent triangles are used for target in which this phenomenon is unclear, as for J1100+0864, or in which it is not observed, such as J1010+0612. The quantities have been calculated consistently with Venturi et al. (2021). The purple squares mark the measurements from Peralta de Arriba et al. (2023), which represent a lower limit of our estimations. Right: kinetic energy of the high-velocity dispersion gas as a function of jet kinetic power.