\[hubble-space-telescope-data-and-observing-strategy\]–\[source-modeling-and-point-source-subtraction\]) are identical for all sources. Relevant properties of each of the six targets are summarized in Table \[tab\_targets\].

UV-faint FIR-luminous Quasars
-----------------------------

Guided by our initial experience with [@Mechtley2012], we determined that high-redshift quasars with weaker UV emission ($M_{1450\textrm{\AA}}>-26.5$ mag), but secure sub-mm detections, i.e., with large rest-frame FIR to UV flux ratios ($F_{\rm FIR}/F_{\rm UV}\gtrsim100$), are the best candidates for successful detection of host emission.

The rationale behind this selection is that a high FIR luminosity—and associated high star formation rate—coupled with a lower nuclear UV luminosity results in a less extreme nuclear-to-host contrast ratio, and thus improved detectability of host UV emission. At the time of selection (February 2012), there were only five such quasars known that met these criteria: , , , , and [SDSS]{} (see Figure \[fig:submm\_selection\]). We note that, while these quasars are UV-‘faint’ relative to the observed high-redshift quasar sample, they are still very luminous in the UV with $-26.5<M_{1450\textrm{\AA}}<-23.9$ mag.

![Selection of ultraviolet-faint, far infrared-luminous quasars based on absolute magnitude (rest-frame 1450Å) and observed sub-mm to near-infrared flux ratio. Our sample of six quasars is denoted by magenta circles, with detections for the five IR-luminous quasars, and an upper limit for the 