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Quasar luminosity function (QLF) shows the active galactic nucleus (AGN)demography as a result of the combination of the growth and the evolution ofblack holes, galaxies, and dark matter halos along the cosmic time. The recentwide and deep surveys have improved the census of high-redshift quasars, makingit possible to construct reliable ultraviolet (UV) QLFs at $2\lesssimz\lesssim6$ down to $M_{1450}=-23$ mag. By parameterizing these up-to-dateobserved UV QLFs that are the most extensive in both luminosity and survey areacoverage at a given redshift, we show that the UV QLF has a universal shape,and their evolution can be approximated by a pure density evolution (PDE). Inorder to explain the observed QLF, we construct a model QLF employing the halomass function, a number of empirical scaling relations, and the Eddington ratiodistribution. We also include the outshining of AGN over its host galaxy, whichmade it possible to reproduce a moderately flat shape of the faint end of theobserved QLF (slope of $\sim-1.1$). This model successfully explains theobserved PDE behavior of UV QLF at $z>2$, meaning that the QLF evolution athigh redshift can be understood under the framework of halo mass functionevolution. The importance of the outshining effect in our model also impliesthat there could be a hidden population of faint AGNs ($M_{1450}\gtrsim-24$mag), which are buried under their host galaxy light.

Pure Density Evolution of the Ultraviolet Quasar Luminosity Function at $2\lesssim z \lesssim6$