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We continue our study of the spectral energy distributions (SEDs) of 11 AGNat 1.5 < z < 2.2, with optical-NIR spectra, X-ray data and mid-IR photometry.In a previous paper we presented the observations and models; in this paper weexplore the parameter space of these models. We first quantify uncertainties onthe black hole masses (M$_{\rm BH}$) and degeneracies between SED parameters.The effect of BH spin is tested, and we find that while low to moderate spinvalues (a$_*$ $\leq$ 0.9) are compatible with the data in all cases, maximalspin (a$_*$ = 0.998) can only describe the data if the accretion disc isface-on. The outer accretion disc radii are well constrained in 8/11 objects,and are found to be a factor ~5 smaller than the self-gravity radii. We thenextend our modelling campaign into the mid-IR regime with WISE photometry,adding components for the host galaxy and dusty torus. Our estimates of thehost galaxy luminosities are consistent with the M$_{\rm BH}$-bulgerelationship, and the measured torus properties (covering factor andtemperatures) are in agreement with earlier work, suggesting a predominantlysilicate-based grain composition. Finally, we deconvolve the optical-NIRspectra using our SED continuum model. We claim that this is a more physicallymotivated approach than using empirical descriptions of the continuum such asbroken power-laws. For our small sample, we verify previously notedcorrelations between emission linewidths and luminosities commonly used forsingle-epoch M$_{\rm BH}$ estimates, and observe a statistically significantanti-correlation between [O III] equivalent width and AGN luminosity.

Reaching the Peak of the quasar spectral energy distribution - II. Exploring the accretion disc, dusty torus and host galaxy