2026ApJ..1000...32C

Understanding the dark matter (DM) halo environment in which galaxies that host active galactic nuclei (AGNs) reside is a window into the nature of supermassive black hole (SMBH) accretion. We apply halo occupation distribution (HOD) modeling tools to interpret the angular cross-correlation functions between 1.5 × 10⁶ luminous red galaxies and our ∼28,500 Hyper Suprime-Cam + Wide-field Infrared Survey Explorer-selected (and L_6μm-limited) AGNs to infer the halo properties of distinct quasar samples at physical scales s > 0.1 Mpc, for z ∈ 0.7-1.0. We find that Type I (unobscured) and Type II (obscured) AGNs cluster differently, both on small and large physical scales. The derived HODs imply that Type I AGNs reside, on average, in substantially (∼3×) more massive halos (M_h ∼ 10^13.4M_⊙) than Type II AGNs (M_h ∼ 10^12.9M_⊙) at >5σ significance. While Type II AGNs show one-halo correlations similar to that of galaxies of their average halo mass, the Type I AGN intra-halo clustering signal is significantly shallower. We interpret this observation with HOD methods and find Type I AGNs are significantly less likely (${f}_{{\rm{sat}}}\sim 0.0{5}_{-0.05}^{+1} \% $) to be found in satellite galaxies than Type II AGNs. We find reddened + obscured AGNs have typical satellite fractions for their halo mass (M_h ∼ 10¹³M_⊙), with ${f}_{{\rm{sat}}}\sim 2{0}_{-5}^{+10} \% $. Our results pose a significant challenge to the strict unified AGN morphological model, and instead suggest that a quasar's spectral class is strongly correlated with its host galaxy's DM halo environment. These intriguing results have provided a more complex picture of the SMBH-DM halo connection, and motivate future analyses of the intrinsic galaxy and accretion properties of AGNs.