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Modern cosmological simulations rely heavily on feedback from active galacticnuclei (AGN) in order to stave off overcooling in massive galaxies and galaxygroups and clusters. An important independent test is whether or not thesimulations capture the broad demographics of the observed AGN population.Here, we have used the cosmo-OWLS suite of cosmological hydrodynamicalsimulations to produce realistic synthetic catalogs of X-ray AGN out to $z$=3,with the aim of comparing the catalogs to the observed X-ray AGN population inthe XXL survey and other recent surveys. We focused on the unabsorbed X-rayluminosity function (XLF), the Eddington ratio distribution, the black holemass function, and the projected clustering of X-ray AGN. To compute theunabsorbed XLF of the simulated AGN, we used recent empirically-determinedbolometric corrections. We show that the simulated AGN sample accuratelyreproduces the observed XLF over 3 orders of magnitude in X-ray luminosity inall redshift bins. To compare to the observed Eddington ratio distribution andthe clustering of AGN, we produced detailed 'XMM-Newton-detected' catalogs ofthe simulated AGN. This requires the production of synthetic X-ray imagesextracted from light cones of the simulations that fold in the relevantinstrumental effects of XMM-Newton. We apply a luminosity- andredshift-dependent obscuration function for the AGN and employ the same AGNdetection algorithm as used for the real XXL survey. We demonstrate that thedetected population of simulated AGN reproduces the observed Eddington ratiodistribution and projected clustering from XXL quite well. We conclude that thesimulations have a broadly realistic population of AGN and that our syntheticX-ray AGN catalogs should be useful for interpreting additional trends and as ahelpful tool for quantifying AGN contamination in galaxy group and clusterX-ray surveys.

The XXL Survey XIX. A realistic population of simulated X-ray AGN: Comparison of models with observations