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High-velocity clouds (HVCs) provide a unique window into the coolest component of the circumgalactic medium and the processes of Galactic inflow and outflow. HVCs, and the complexes into which they are arranged, are found by their emission in HI or absorption in numerous metal lines, and have radial velocities inconsistent with Galactic rotation \cite{Wakker_1997}. HVCs with negative radial velocities, which are metal enriched in the range of 10\% to 30\% of the solar metallicity, are likely a tracer of the process by which material accretes onto the Galaxy, though the total rate of this accretion is very uncertain \cite{Putman_2012}. Less explored are the HVCs with positive radial velocities, most of which are in the inner two quadrants of the Galactic sky. These include the Wannier complexs WA, WB, WD, WE, and the Smith Cloud \cite{1991A&A...250..509W}. The Smith cloud has received significant attention of late, for its strongly cometary appearance which provides enough information to infer past trajectories, and make some inference as to its origin \cite{Lockman_2008, Fox_2015}.  Complex WD is the largest area (non-Magellanic) positive velocity HVC Complex covering 310 square degrees with a total HI flux of 1.2 $\times 10^7$ K km/s arcmin$^2$. It is by far the largest non-Magellanic complexes that exist in the inner two Galactic quadrants, where a very small fraction of HVC flux is detected. With a range of velocities of +90 to +130 km/s, it is consistent with cylindrically rotating on the far side of the inner Galaxy, 20 kpc from the sun with a mass of 6 $\times 10^7 M_\odot$. This would make it very similar in mass, Galactocentric radius, and height to Complex C C, the largest area non-magellanic complex  \cite{Thom_2008}. It is still unknown why there is a bias toward the outer disk in the HVC complexes, but determining the distance this outlier object should significantly improve our understanding of the MW's HVC system as a whole One major issue in gaining a better phsyical understanding these enigmatic clouds is their distance. Since there are no objects of standard luminosity in these clouds, there are effectively no distance constraints from HI emission or optical and UV absorption lines, which probe only the distance-independent column densities. Distance not only gives us a mass for these structures, but also a context; the relationship between the cloud and the disk gives us insight as to its origin.