\begin{table}%t1 \caption{Cloud parameters derived from the molecular line measurements. \label{cloudlineparams}} %\centerline {\begin{tabular}{l|cc|l|ccl} \hline\hline\noalign{\smallskip} \multicolumn{1}{c|}{} & \multicolumn{1}{c}{$r_{\rm e}^1$} & \multicolumn{1}{c|}{$r_{\rm hp}^1$} & \multicolumn{1}{c|}{$\Delta V$} & \multicolumn{1}{c}{$M_{\rm CO}^2$} & \multicolumn{1}{c}{$M_{\rm lte}^3$} & \multicolumn{1}{c}{$M_{\rm vir}^4$} \\ \multicolumn{1}{c|}{} & \multicolumn{2}{c|}{pc} & \multicolumn{1}{c|}{km~s$^{-1}$} & \multicolumn{3}{c}{$10^3$~\Msol} \\ \hline\\[-3.2mm] $^{12}$CO, cloud & 5.3 & 1.6 & 2.77$^5$ & 4.5--6.6 & & 5.1 \\ & & & 2.69$^{5,6}$ & & & 4.8$^6$ \\ $^{12}$CO, core & 2.9 & 1.6 & 3.34$^5$ & 3.2--4.7 & & 4.1 \\ & & & 3.22$^{5,6}$ & & & 3.8$^6$ \\ $^{13}$CO, core & 2.7 & 1.1 & 2.14 & & 1.0--5.0 & 1.6 \\ C$^{18}$O, core & 1.6 & 0.9 & 1.72 & & 0.8--3.2 & 0.6 \\ CS, core & 1.1 & 0.7 & 2.07 & & & 0.4 \\ \hline \end{tabular} } \par \smallskip\noindent \\ 1.\ $r_{\rm e}$: equivalent radius, corrected for beam size, at the $2{-}3\sigma$-level; $r_{\rm hp}$: the radius at half-maximum intensity level, corrected for beam size. 2.\ Via $N$(H$_2$)~=~$X$ $\int T_{\rm mb}(CO){\rm d}v$. The indicated range of masses derives from using the inner Galaxy value $X=1.9 \times 10^{20}$~cm$^{-2}$(K~\kms)$^{-1}$ and allowing a possible~45\% increase at the edge of the Galaxy (see text). 3.\ Assuming LTE-conditions, and $T_{\rm ex}=20$~K. Smaller values are for local abundance ratios for [H$_2$]/[$^{13}$CO] and [H$_2$]/[C$^{18}$O], higher values are for abundances extrapolated to the FOG (see text). 4.\ $M_{\rm vir}=126$ $r$ ($\Delta V)^2$, for a density distribution $\propto$$r^{-2}$, and using $r_{\rm e}$. 5.\ Equivalent width, derived from the area under the emission line and the peak temperature. 6.\ Excluding the wing emission. \end{table}