\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}