AGN X-ray luminosity (3 <= z <= 6)

We derive the X-ray spectral properties for all sources via spectral fitting, using a consistent technique and model. For modeling the parametric form of the XLF and the absorption function, we use a Bayesian methodology allowing us to correctly propagate the uncertainties for the observed X-ray properties of our sources and also the absorption effects. The evolution of XLF is in agreement with a pure density evolution model similar to what is witnessed at optical wavelengths, although a luminosity dependent density evolution model cannot be securely ruled out.

A large fraction (~60%) of our sources are absorbed by column densities of N_H_>=10^23^cm^-2^, while ~17% of the sources are Compton-thick. Our results favor a scenario where both the interstellar medium of the host and the AGN torus contribute to the obscuration. The derived black hole accretion rate density is roughly in agreement with the large-scale cosmological hydro-dynamical simulations, if one takes into account the results that the X-ray AGN are hosted by massive galaxies, while it differs from the one derived using JWST data.

The latter could be due to the differences in the AGN and host-galaxy properties