deletions | additions       diff --git a/section_Data_subsection_New_Observations__.tex b/section_Data_subsection_New_Observations__.tex  index 0d52b8f..2dceeee 100644  --- a/section_Data_subsection_New_Observations__.tex  +++ b/section_Data_subsection_New_Observations__.tex 
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\subsection{Archival Data}  We In addition to the new data taken with FLAMES, we  also use used  archival HI data from the GASS survey \cite{Kalberla_2010}  Here's \cite{Kalberla_2010}. GASS is  a spectrum, survey of Galactic HI taken  with GASS the Parkes antenna, with a beam size of 16$^\prime$, a spectral resolution of 1 km/s, and an rms noise of 57 mK. These  data overlaid.  Here's allow us to map out the structure of Complex WD on the sky, and compare the spectrum of the HI emission to Ca II H \& K absorption along the line of sight. We present in Figure \ref{fig:WD}  an image of complex Complex  WD from GASS GASS, along with the positions of clouds noted in the \cite{1991A&A...250..509W} catalog, and the line-of-sight toward USNO-A0600-15865535.