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\section{Introduction}  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 in 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. Inflowing HVCs, 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). The Smith cloud has received significant attention of late... Complex WD is a large area complex covering X square degrees with a total HI flux of Y. 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. 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