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tokens: scaled-down AGN jet model based on equipartition assumptions and applied it to observationally well defined samples of galactic and extragalactic sources. They find that the jet powers of their studied sources were comparable to their accretion disk luminosities providing evidence for a disk-jet coupling holding from stellar mass BHs to low-luminosity AGN. Merloni Heinz (2008) present a synthesis model for the AGN evolution where they studied how SMBHs grow and evolve through the age of the Universe. In this model, AGN with high Eddington ratios may display either only radiative feedback (high-radiative mode, HR) or both radiative and kinetic feedback (high-kinetic mode, HK). In this context, HLAGN with low radio AGN fractions ( f AGN 0.5) would be those which display mostly radiative feedback, while those with high radio AGN fractions ( f AGN ≥ 0.5) also produce kinetic feedback in the form of radio-detectable features, such as cores, jets and lobes. Radiative feedback is expected to arise in galaxies hosting rapidly accreting SMBHs, where the energy released by the growth of the SMBH can influence the properties of the hosts (e.g., see a review by Fabian 2012 ). The models of galaxy evolution usually find the AGN bolometric luminosity density to increase from the local redshift out to a peak around z ∼ 2 − 3, followed by a decrease toward higher redshifts (e.g., Croton et al. 2006 ; Merloni Heinz 2008 ). For the ∼38% of HLAGN for which we estimated a radio luminosity arising from AGN emission (Sect. 3.2 ) we compare the radiative luminosity density to literature expectations (e.g., Croton et al. 2006 ; Merloni Heinz 2008 ). We binned the radiative luminosities derived from the SED-fitting decomposition (see Delvecchio et al. 2017 ) into nine redshift bins, finding typical values of bolometric luminosity density to be 1% of those found from the literature for all radiatively efficient AGN. This confirms that X-ray and MIR selected AGN detected in radio are not the dominant contribution to the total bolometric output expected for radiatively efficient AGN. In the following sections, we describe how the number and luminosity densities of HLAGN change through cosmic time. By scaling the 1.4 GHz AGN luminosity into kinetic luminosity, we calculate the kinetic luminosity density and compare it to semi-analytic model predictions. 6.2. Cosmic evolution of radio AGN To calculate the number and luminosity density, we use where Φ( L 1.4 GHz ) is the redshift evolved luminosity function, using both best-fit evolution parameters derived from the redshift binned and continuous fitting. Here we take the lower and upper limits of the integral to be L 1.4 GHz = 10 22 WHz −1 and L 1.4 GHz = 10 28 WHz −1 , respectively. The normalizations of the number and luminosity density evolution curves are affected by the chosen limits of integration. For example, a decrease of the lower limit to L 1.4 GHz = 10 21 WHz −1 would produce a number density higher by a factor