deletions | additions       diff --git a/subsection_Line_fitting_We_perform__.tex b/subsection_Line_fitting_We_perform__.tex  index 085f16b..d288e05 100644  --- a/subsection_Line_fitting_We_perform__.tex  +++ b/subsection_Line_fitting_We_perform__.tex 
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\subsection{Line \subsection{ISM Absoption 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}}. For our Voigt profile fit analysis, the intrinsic model profiles are convolved with a Gaussian of FWHM 14 km/s to account for the instrument resolution. 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 1 km/s, respectively. The redshifted high-velocity absorption component is best fit with two Voigt profile components centered at $v_{LSR}\, \approx$ 942and 108 km/s, respectively. All four 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.