deletions | additions       diff --git a/section_Discussion_The_clear_detection__.tex b/section_Discussion_The_clear_detection__.tex  index 3a91741..183c997 100644  --- a/section_Discussion_The_clear_detection__.tex  +++ b/section_Discussion_The_clear_detection__.tex 
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The kinematics and location of Complex WD do give us some clues as to its origin. Originally \cite{1991A&A...250..509W} suggested that because complex WD is at positive velocity it is likely part of the structure of the Galaxy itself co-rotating with the disk. We call this the "far" scenario in Figure \ref{fig:contour}, and it is emphatically ruled out by our detection of absorption. The appeal of the scenario is quite clear from the Figure -- a distant cloud could easily be nicely corotating with the disk. We now know that Complex WD is mostly inside the solar circle toward the fourth quadrant. Along the line of sight to USNO-A0600-15865535, Complex WD sits above a portion of the disk moving at -30 km/s LSR if we assum it it is at the maximal distnace of 5.2 kpc, decreasing to 0 km/s LSR as we assume a closer distance. Complex WD is therefore strongly not in corotation with the disk. This is in rather stark contrast with other HVCs; a simplified model of HVCs with known distances found that they rotated with the disk at 77 km/s -- slower than Galactic rotation, but with the same sense \citep{Putman_2012}.   A number of scenarios could account for an overall difference in velocity between the cloud and the disk. An accreting cloud could easily have a much lower accretion velocity than the rotation speed of the disk, and the positive velocity observed could be an artifact of the solar motion. Similarly, it is possible that Complex WD is material ejected from star-forming regions closer to Galactic center \citep[e.g.][]{Ford_2010}, and thus the high positive velocity is an effect of the lower specific angular momemtum of that material. Both of these scenarios suffer from the fine tuning required to meet the very small LSR velocity gradient found in the Complex. A flux-weighted first-order polynomial fit to the velocity gradient in the Wakker \& van Woerden 1991 catalog of WD clouds find $-0.072 \pm 0.146$ km/s per degree of Galactic longitude. The reflex velocity of the solar motion represents 100 km/s across 40 degrees of Complex WD -- unless the Cloud is conspiring to thwart our detection of a velocity gradient, we should see some effect of the solar motion. While we cannot fully rule out the "intermediate" scenario, where the bulk of the cloud is at $\sim 5$ kpc, this velocity structure puts very tight constraints on any future model.  One possibility is that Finally we examine a "near" scenario, where  Complex WD is simply a wayward accreting cloud. It could   A distance of 5 only 1-3  kpc puts away. In  this part of scenario  the WD complex above cloud originated from an area near  the molecular ring, but with a significantly offset sun, and thus has inherited the overall solar motion, thus largely solving the fine-tuning of the LSR  velocity. Unlike complex C, it In the "near" scenario the cloud  is not ejected from the disk by some kind of impulsive event, perhaps connected to star formation  incorotation with  the disk, Gould Belt,  or part of a lagging halo.  Do we put together Saggitarus Arm, imparting  an argument overall 100 km/s bulk velocity. A cloud this far away would only be  about an outflow effect? 0.5 kpc above the disk, which is quite low for most known HVCs, and would make it distinct from all other known HVCs in it's origin. The somewhat symmetric Complex WE, with a similar velocity below the disk, could conceivably have been generated by the same event.