  In order to test active galactic nucleus (AGN) unification and evolutionary
models, we measured the AGN clustering properties as a function of AGN
obscuration defined in terms of hydrogen column density, $N_{\rm H}$. In
addition to measuring the clustering of unobscured ($N_{\rm H} < 10^{22}\,{\rm
cm}^{-2}$) and moderately obscured ($10^{22} \leq N_{\rm H} < 10^{23.5}$) AGNs,
we also targeted highly obscured sources ($N_{\rm H}\geq 10^{23.5}$) up to
redshifts of $z=3$. We have compiled one of the largest samples of
X-ray-selected AGNs from a total of eight deep XMM/Chandra surveys. We measured
the clustering as a function of both AGN obscuration and redshift using the
projected two-point correlation function, $w_{\rm p}(r_{\rm p})$. We modeled
the large-scale clustering signal, measured the AGN bias, $b(z, N_{\rm H})$,
and interpreted it in terms of the typical AGN host dark matter halo, $M_{\rm
halo}(z, N_{\rm H}$). We find no significant dependence of AGN clustering on
obscuration, suggesting similar typical masses of the hosting halos as a
function of $N_{\rm H}$. This result matches expectations of AGN unification
models, in which AGN obscuration depends mainly on the viewing angle of the
obscuring torus. We measured, for the first time, the clustering of highly
obscured AGNs and find that these objects reside in halos with typical mass
$\log M_{\rm halo} = 12.98_{-0.22}^{+0.17} [h^{-1} M_\odot]$
($12.28_{-0.19}^{+0.13}$) at low $z \sim 0.7$ (high $z \sim 1.8$) redshifts. We
find that irrespective of obscuration, an increase in AGN bias with redshift is
slower than the expectation for a constant halo mass and instead follows the
growth rate of halos, known as the passive evolution track. This implies that
for those AGNs the clustering is mainly driven by the mass growth rate of the
hosting halos and galaxies across cosmic time.
