deletions | additions       diff --git a/section_Discussion_The_clear_detection__.tex b/section_Discussion_The_clear_detection__.tex  index b43d7f6..ebebb3f 100644  --- a/section_Discussion_The_clear_detection__.tex  +++ b/section_Discussion_The_clear_detection__.tex 
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The clear detection of Ca II H \& K absorption at +100 km/s in USNO-A0600-15865535, coincident with HI emission from Complex WD, indicates that the complex is closer than the star, at a distance 5.2 kpc. The column of Ca II measured is comparable between the cloud and the disk, even though they have wildly different HI columns. This is consistent with the weak \cite{Wakker_2000} or non-existent \cite{Bekhti_2012} correlation between HI and Ca II column density, which also explains the non-detection of the small intermediate velocity cloud along the line of sight at 60 km/s. Unfortunately, this lack of correlation makes it impossible to infer anything about the metallicity of the cloud from these metal absorption lines. Future metallicity measurements, perhaps toward USNO-A0600-15865535, will be critical in determining the origin of Complex WD.   The kinematics and location of complex WD do give us some clues as to its origin. 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 assumit it is at the maximal distnace of 5.2 kpc, decreasing to 0 km/s LSR as we assume a closer distance (see Figure \ref{fig:contour}. \ref{fig:contour}).  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}. One possibility is that Complex WD is simply a wayward accreting cloud. It could