| Abstract: | We identify and characterize a population of luminous dust-poor quasars at z<5, showing little IR emission from the dusty structure of active galactic nuclei (AGNs). This class of AGNs discovered at z>5, has been poorly understood in terms of number evolution or of any dependence on physical properties. In order to better understand the observational features of luminous dust-poor quasars, we searched for large area survey databases to compile a rest-frame UV to IR library of 41,000 optically selected type-1 quasars. After fitting the broad-band spectral energy distributions with accretion disk and dust model components, we find 0.6% of our sample to be hot dust-poor under the NIR-to-optical flux ratio selection compatible with Jiang et al. (2010). The blue UV-optical continuum slope of dust-poor quasars, together with the NIR-MIR luminosity correlations are presented. We provide the number evolution of the dust-poor fraction with redshift, for given bolometric luminosity. Also, we find the low BH mass and high Eddington ratio, to be connected with the dust poorness of AGNs. Finally, we provide models that explain the occurrence and physical properties of dust-poor quasars, which is best explained as in a rapidly growing evolutionary state. |