Table 5: Total column density of Na I, K I, Ca II, Ti II and 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. 4 and 6) is given in Tables 11 to 15 (on-line only). For Sk -67 2 and Sk -68 135 the Na I D doublet is saturated and we used the Na I UV line at 3302 Å instead. The error in column density log N is about 0.02 to 0.05 dex for K I, Ca II, Ti II and about 0.03 and 0.08 dex for Na I D and 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 Ca II and Na I (from 3302.6 Å line) agree well, within the error bars, with preliminary results obtained by Welty (private communication) for the targets Sk -69 243, Sk -68 135 and Sk -67 5.
  Sk -69 223 Sk -69 243 Sk -67 2 Sk -68 135 Sk -67 5 (STD) Sk -70 120 (STD)
\ensuremath {E_{B-V}} $_{\rm , LMC}$ (mag) 0.20 0.29 0.12 0.14 0.04 0.02
log N (cm-2)
LMC: ${\bf 200} < \vec{v} < {\bf 330}$ km s-1        
Na I 12.59 12.84 13.49 13.25 12.49 11.30
K I 11.03b 11.24 11.65 11.51 11.09 9.70b
Ca II 12.68 12.88 12.32 12.68 12.26 12.59
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
H Ia 21.46 21.47 21.18 21.42 21.08 20.89
      21.003,4 21.441 20.891  
H2   $\sim $191   $19.87\pm0.07$1 $19.44\pm0.05$1,2  
H $_{\rm tot}$       21.502 21.492  
Milky Way: $\vec{v} < {\bf 30}$ km s-1        
Na I 12.77c 12.99c 12.44 12.26 11.80 12.01
Ca II 12.23 12.05 12.09 12.05 12.15 11.96
Ti II 12.05 11.97 12.01 11.98 11.98 12.15
Intermediate: ${\bf 30} < \vec{v} < {\bf 200}$ km s-1        
Na I - 11.48 10.89 10.75 10.74 11.12
Ca II 11.93 11.77 11.50 12.11 11.45 11.28
Ti II - - 11.09 11.33 - -
References:
1 Tumlinson et al. (2002); 2 André et al. (2004); 3 Cartledge et al. (2005); 4 Gordon et al. (2003).
Notes: a LMC 21 cm column density from H I spectral line profiles provided by Staveley-Smith (Kim et al. 2003; Staveley-Smith et al. 2003). This is converted to N(H I) via N(H I) = ( $0.75\pm0.35$) $\times $ N(21 cm). For these sightlines this results in typical log N(H I) errors of +0.17 and -0.27 dex; b no K I data are available. K I is derived from the relation with Na I (Welty et al. 2001); 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 Na I 3303 Å line (low quality) we modelled the MW Na I lines with VAPID, including a Monte-Carlo error analysis.

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