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Table 4:

HI, H2 and total hydrogen column densities.
  $\upsilon_0$ $\Delta \upsilon$ N(H)a $N({\rm H}_2)^{c}$ $N_{\rm H}^{d}$
Source (km s-1) (km s-1) (cm-2) (cm-2) (cm-2)
      $\times 10^{21}$ $\times 10^{21}$ $\times 10^{21}$
W51 $\left. \begin{array}{r r r} 6.2 \\ 11.8 \end{array} \right. $ $\left. \begin{array}{r r r} 5.6 \\ 6.0 \end{array} \right. $ $\left. \begin{array}{r r r} 1.27 \\ 0.58 \end{array} \right. $ 0.47 2.3
  $\upsilon_{\rm min}$ $\upsilon_{\rm max}$ N(H)b $N({\rm H}_2)^{c}$ $N_{\rm H}^{d}$
Source (km s-1) (km s-1) (cm-2) (cm-2) (cm-2)
      $\times 10^{21}$ $\times 10^{21}$ $\times 10^{21}$

G05.88-0.39 		$\left. \begin{array}{r r r} -31.3 \\ -10.0 \\ 4.0 \\ 20.0 \end{array} \right. $ $\left. \begin{array}{r r r} -10.0 \\ 4.0 \\ 20.0 \\ 29.3 \end{array} \right. $ $\left. \begin{array}{r r r} 1.59 \\ {>}6.68 \\ 5.87 \\ {>}3.86 \end{array} \right. $   16
G08.67-0.36 $\left. \begin{array}{r r r} -1.7 \\ 11.3 \\ 25.7 \end{array} \right. $ $\left. \begin{array}{r r r} 11.3 \\ 25.7 \\ 45.3 \end{array} \right. $ $\left. \begin{array}{r r r} 4.80 \\ 5.32 \\ {>}9.62 \end{array} \right. $   14
G10.62-0.38 $\left. \begin{array}{r r r} 11.3 \\ 25.0 \\ 30.6 \end{array} \right. $ $\left. \begin{array}{r r r} 25.0 \\ 30.6 \\ 47.3 \end{array} \right. $ $\left. \begin{array}{r r r} 3.53 \\ 2.61 \\ 5.54 \end{array} \right. $ 15.8 17
G34.3+0.1 $\left. \begin{array}{r r r} -2.5 \\ 7.1 \\ 20.0 \end{array} \right. $ $\left. \begin{array}{r r r} 7.1 \\ 20.0 \\ 34.1 \end{array} \right. $ $\left. \begin{array}{r r r} 0.54 \\ 2.01 \\ 4.42 \end{array} \right. $   9
W49N $\left. \begin{array}{r r r} 30.0 \\ 50.0 \end{array} \right. $ $\left. \begin{array}{r r r} 50.0 \\ 78.2 \end{array} \right. $ $\left. \begin{array}{r r r} 6.95 \\ 7.23 \end{array} \right. $ $\left. \begin{array}{r r r} 1.6 \\ 4.0 \end{array} \right. $ 23

Notes. (a) Gaussian decomposition from Koo (1997). The column densities have been scaled to a spin temperature of 100 K. (b) Inferred from the absorption profiles observed by Fish et al. (2003) with the VLA interferometer. A spin temperature of 100 K is assumed. (c) Estimation from the CH emission lines observed by Rydbeck et al. (1976) toward W51 and W49N, the CH absorption lines observed by Gerin et al. (in prep.) toward G10.62-0.38, and the correlation between CH and H2, $N({\rm CH})/N({\rm H}_2) = 4.3 \times 10^{-8}$ (Liszt & Lucas 2002). (d) From models of the extinction at 2 $\mu$m by Marshall et al. (2006).


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