deletions | additions       diff --git a/subsection_Line_fitting_We_perform__.tex b/subsection_Line_fitting_We_perform__.tex  index 7500f90..8bcd8bc 100644  --- a/subsection_Line_fitting_We_perform__.tex  +++ b/subsection_Line_fitting_We_perform__.tex 
...
\subsection{Line fitting}  We perform Voigt profile fitting of the calcium II H \& K lines after dividing out the continuum spectrum and, in the case of the calcium II H lines, dividing out the Sersi\'c fit to the strong H$\epsilon$ line, which is centered at 230 km/s LSR in the calcium II H frame. The column densities were determined by simultaneously fitting Voigt profiles to both lines of the Ca II doublet with the \texttt{VPFIT} software \footnote{Available at \href{http://www.ast.cam.ac.uk/~rfc/vpfit.html}{http://www.ast.cam.ac.uk/$\sim$rfc/vpfit.html}}. The Ca II line close to the  Milky Way rest frame is best fit with two Voigt profile components centered at $v_{LSR} \,\approx$ -6  and 8 km/s, respectively. The redshifted  high-velocity lines are each absorption component is  best fit with two Voigt profile  components in each of the the two Ca II lines. centered at $v_{LSR}\, \approx$ 94 and 100 km/s, respectively.  All four fits individual Voigt profile compoents  to Ca II K components agree with the equivalent Ca II H parameters to within errors. The individual Voigt profile fits are reported in Table \ref{Table:Voigt_Fit} and are shown in Figure 3.  \begin{table}[ht]  \centering 
...
Ca II H & 11.8693 $\pm$ 2.1294 & 108.2863 $\pm$ 3.0378 & 12.1557 $\pm$ 0.1443\\  \hline  \end{tabular}  \lable{Table:Voigt_Fit}  \end{table}