“…Such obscured ("type 2") active galactic nuclei (AGNs) can be identified from narrow optical emission lines (Zakamska et al 2003(Zakamska et al , 2004(Zakamska et al , 2005Reyes et al 2008;Yuan et al 2016), radio luminosity (e.g., McCarthy 1993Martínez-Sansigre et al 2006;Seymour et al 2007;Wilkes et al 2013), or X-ray properties (e.g Alexander et al 2001;Stern et al 2002;Treister et al 2004;Vignali et al 2006Vignali et al , 2009Del Moro et al 2014). In addition, pioneering work with the Spitzer Space Telescope demonstrated that obscured quasars have similar mid-infrared (MIR) SEDs to their unobscured counterparts but are dominated by host galaxy light in the optical (Lacy et al 2004;Rowan-Robinson et al 2005;Stern et al 2005;Alonso-Herrero et al 2006;Martínez-Sansigre et al 2006;Polletta et al 2006;Hickox et al 2007;Donley et al 2008;Lacy et al 2013Lacy et al , 2015Dai et al 2014). Consequently, obscured quasars can be most efficiently selected in the MIR, as they appear very red in the IRAC [3.6] -[4.5] color, characteristic of the "hot" MIR SED that is evident in broadline quasars (e.g., Richards et al 2006;Assef et al 2010, hereafter R06 and A10, respectively).…”