  We present a simple method for identifying candidate white dwarf systems with
dusty exoplanetary debris based on a single temperature blackbody model fit to
the infrared excess. We apply this technique to a sample of Southern Hemisphere
white dwarfs from the recently completed Edinburgh-Cape Blue Object Survey and
identify four new promising dusty debris disk candidates. We demonstrate the
efficacy of our selection method by recovering three of the four
$\textit{Spitzer}$ confirmed dusty debris disk systems in our sample. Further
investigation using archival high resolution imaging shows $\textit{Spitzer}$
data of the un-recovered fourth object is likely contaminated by a
line-of-sight object that either led to a mis-classification as a dusty disk in
the literature or is confounding our method. Finally, in our diagnostic plot we
show that dusty white dwarfs which also host gaseous debris lie along a
boundary of our dusty debris disk region, providing clues to the origin and
evolution of these especially interesting systems.
