\begin{table}%t5
\caption{Total column density of \ion{Na}{i}, \ion{K}{i}, \ion{Ca}{ii}, \ion{Ti}{ii} and \ion{H}{i}
  (for the Milky Way (MW), intervening high velocity clouds (VC) and Large Magellanic Cloud (LMC) components) 
   derived from fitting the profiles with the splot task in IRAF.
   The column density of the individual components of the interstellar atomic line profile (as shown in
   Figs.~\ref{fig:IS-1} and~\ref{fig:IS-3}) is given in Tables~\ref{tb:IScomp_Sk69_243} to~\ref{tb:IScomp_Sk70_120}
   (on-line only). 
   For \object{Sk~--67 2} and \object{Sk~--68 135} the \ion{Na}{i}~D doublet is saturated and we used 
   the \ion{Na}{i} UV line at 3302~\AA\ instead.
   The error in column density log~N is about 0.02 to 0.05 dex for \ion{K}{i}, \ion{Ca}{ii}, \ion{Ti}{ii} and 
   about~0.03 and 0.08~dex for \ion{Na}{i}~D and \ion{Na}{i} (UV), respectively. 
   The apparent optical depth method picks up more unresolved structure and therefore gives slightly higher values of $N$
   than other methods (like Gaussian profile fitting).
   Nevertheless, the obtained column densities for \ion{Ca}{ii} and \ion{Na}{i} (from 3302.6~\AA\ line) agree well, 
   within the error bars, with preliminary results obtained by Welty (private communication) for the targets 
   \mbox{\object{Sk~--69 243}}, \mbox{\object{Sk~--68 135}} and \mbox{\object{Sk~--67 5}}.
\label{tb:NX}}
%\centerline
{\begin{tabular}{lllllll}\hline\hline
                   		  & \object{Sk~--69 223} & \object{Sk~--69 243} & \object{Sk~--67 2} & \object{Sk~--68 135} &  \object{Sk~--67 5} (STD) & \object{Sk~--70 120} (STD)\\
\Ebv$_{\rm, LMC}$ (mag)		  & 0.20	& 0.29         & 0.12	   & 0.14	 & 0.04 	 & 0.02         \\ \hline
\multicolumn{7}{c}{log $N$  (cm$^{-2}$)} \\ \hline
\multicolumn{3}{l}{\bf LMC: ${\bf 200} < \vec{v} < {\bf 330}$~km~s$^{-1}$}       &  	   &	    	 &               &		\\ 
\ion{Na}{i}	 	  	  &  12.59	& 12.84        & 13.49     & 13.25	 & 12.49	 & 11.30  	\\
\ion{K}{i}	        	  &  11.03$^b$ & 11.24        & 11.65     &  11.51	 & 11.09	 & 9.70$^b$    \\     
\ion{Ca}{ii}			  &  12.68	& 12.88        & 12.32     & 12.68	 & 12.26	 & 12.59        \\ 
\ion{Ti}{ii}		 	  &  12.77	& 12.76        & 12.16     & 12.73	 & 12.30	 & 12.63        \\    
$N$~(21~cm)$^a$      	  &  21.58	& 21.60        &  21.31    & 21.55	 & 21.21	 & 21.02        \\ 
\ion{H}{i}$^a$  		  & 21.46	& 21.47	       & 21.18	   & 21.42	 & 21.08	 & 20.89        \\ 
	                	  &		&	       & 21.00$^{3,4}$& 21.44$^1$  & 20.89$^1$	 &	        \\    
H$_{2}$                 	  &		&$\sim$19$^1$&	   & $19.87\pm0.07$$^{1}$& $19.44\pm0.05$$^{1,2}$ &      \\    
H$_{\rm tot}$  			  &		&              &	   & 21.50$^2$  & 21.49$^2$	 &	        \\    
\hline
\multicolumn{3}{l}{\bf Milky Way: $\vec{v} < {\bf 30}$~km~s$^{-1}$}        &  	   &	    	 &               &              \\ 
  \ion{Na}{i}                 	& 12.77$^c$ &  12.99$^c$   & 12.44     & 12.26       &   11.80       &   12.01      \\ 
  \ion{Ca}{ii}                	& 12.23	   &  12.05	   & 12.09     &  12.05      &   12.15       &   11.96      \\ 
  \ion{Ti}{ii}                	& 12.05	   &  11.97	   & 12.01     &  11.98      &   11.98       &   12.15      \\ 
\hline
\multicolumn{3}{l}{\bf Intermediate: ${\bf 30} < \vec{v} < {\bf 200}$~km~s$^{-1}$}&	   &             &		 &              \\ 
  \ion{Na}{i}  			  & --         & 11.48         & 10.89     & 10.75	 &    10.74	 &  11.12       \\ 
  \ion{Ca}{ii} 			  & 11.93      & 11.77         & 11.50     & 12.11	 &    11.45	 &  11.28       \\ 
  \ion{Ti}{ii}  		  & --         & --	       & 11.09     & 11.33	 &    --	 &  --          \\ 
\hline
\end{tabular}}
\par
\smallskip
\par
References:\\
  $^1$ \citet{2002ApJ...566..857T}; 
  $^2$ \citet{2004AetA...422..483A}; 
  $^3$ \citet{2005astro.ph..5416C}; 
  $^4$ \citet{2003ApJ...594..279G}. \\
Notes: $^a$  LMC 21~cm column density from \ion{H}{i} spectral line profiles provided by  \mbox{Staveley-Smith} (\citealt{2003MNRAS.339...87S,2003ApJS..148..473K}).\
	  This is converted to $N$(\ion{H}{i}) via 
	  $N$(\ion{H}{i})~=~($0.75\pm0.35$)~$\times$~$N$(21~cm). 
	  For these sightlines this results in typical log~$N$(\ion{H}{i}) errors 
	  of~$+0.17$ and $-0.27$~dex;  $^b$  no \ion{K}{i} data are available. \ion{K}{i} is derived from the relation with \ion{Na}{i} \citep{2001ApJ...554L..75W}; $^c$ due to the large amount of unresolved structure in the MW gas the doublet optical depth correction method is unreliable
	  for these targets. Using information contained in the unsaturated \ion{Na}{i}~3303~\AA\ line (low quality) 
	  we modelled the MW \ion{Na}{i} lines with VAPID, including a Monte-Carlo error analysis.
\end{table}