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It is widely reported, based on clustering measurements of observed activegalactic nuclei (AGN) samples, that AGN reside in similar mass host dark matterhalos across the bulk of cosmic time, with log $M/M_\odot$~12.5-13.0 to z~2.5.We show that this is due in part to the AGN fraction in galaxies rising withincreasing stellar mass, combined with AGN observational selection effects thatexacerbate this trend. Here, we use AGN specific accretion rate distributionfunctions determined as a function of stellar mass and redshift forstar-forming and quiescent galaxies separately, combined with the latestgalaxy-halo connection models, to determine the parent and sub-halo massdistribution function of AGN to various observational limits. We find thatwhile the median (sub-)halo mass of AGN, $\approx10^{12}M_\odot$, is fairlyconstant with luminosity, specific accretion rate, and redshift, the full halomass distribution function is broad, spanning several orders of magnitude. Weshow that widely used methods to infer a typical dark matter halo mass based onan observed AGN clustering amplitude can result in biased, systematically highhost halo masses. While the AGN satellite fraction rises with increasing parenthalo mass, we find that the central galaxy is often not an AGN. Our resultselucidate the physical causes for the apparent uniformity of AGN host halosacross cosmic time and underscore the importance of accounting for AGNselection biases when interpreting observational AGN clustering results. Wefurther show that AGN clustering is most easily interpreted in terms of therelative bias to galaxy samples, not from absolute bias measurements alone.

The AGN-galaxy-halo connection: The distribution of AGN host halo masses to z=2.5