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The orientation-based unification model of active galactic nuclei (AGNs)posits that the principle difference between obscured (Type 2) and unobscured(Type 1) AGNs is the line-of-sight into the central engine. If this model iscorrect than there should be no difference in many of the properties of AGNhost galaxies (e.g., the mass of the surrounding dark matter haloes). However,recent clustering analyses of Type 1 and Type 2 AGNs have provided someevidence for a difference in the halo mass, in conflict with theorientation-based unified model. In this work, a method to compute theConditional Luminosity Function (CLF) of Type 2 and Type 1 AGNs is presented.The CLF allows many fundamental halo properties to be computed as a function ofAGN luminosity, which we apply to the question of the host halo masses of Type1 and 2 AGNs. By making use of the total AGN CLF, the Type 1 X-ray luminosityfunction, and the luminosity-dependent Type 2 AGN fraction, the CLFs of Type 1and 2 AGNs are calculated at $z\approx 0$ and $0.9$. At both $z$, there is nostatistically significant difference in the mean halo mass of Type 2 and 1 AGNsat any luminosity. There is marginal evidence that Type 1 AGNs may have largerhalo masses than Type 2s, which would be consistent with an evolutionarypicture where quasars are initially obscured and then subsequently revealthemselves as Type 1s. As the Type 1 lifetime is longer, the host halo willincrease somewhat in mass during the Type 1 phase. The CLF technique will be apowerful way to study the properties of many AGNs subsets (e.g., radio-loud,Compton-thick) as future wide-area X-ray and optical surveys substantiallyincrease our ability to place AGNs in their cosmological context.

monthly notices of the royal astronomical society

Clustering, Cosmology and a New Era of Black Hole Demographics -- II.  The Conditional Luminosity Functions of Type 2 and Type 1 Active Galactic  Nuclei