\begin{table}%T4
\caption{
The ISO/LWS high-$J$ CO and atomic FIR lines at 80$''$ resolution.
The transformation between flux densities and surface brightnesses was made using the 
beam sizes  given in Table 5.10 of the ISO-LWS Handbook v. 2.1.
The beam solid angle varies between $8\times10^{-8}$~sr and $1.4\times 10^{-7}$~sr.
Because the lines are unresolved, the line widths were held to the instrumental line width: 0.29 or 0.60~$\mu$m
for detectors $0{-}4$ and $5{-}9$, respectively.
Correction factors between 0.37 to 0.85 for extended sources have been applied.
% i.e. $0.8\times$10$^{-7}$ sr 
%for CO~15\TO14 and 14\TO13, 0.85$\times$10$^{-7}$ sr for CO~$17\TO1$6 and 
%16\TO15 and [CII] 158~$\mu$m,  0.90 (1.24)$\times$10$^{-7}$ sr for [OI] 63(145)~$\mu$m.
We assume a 30\% absolute photometry uncertainty for LWS.
%{\bf CHECK: Determine masses from C+/H ratio? e.g. Israel et al. 1996 what is $x_{C+}$}
}\label{tab-iso-pdr-lines}
%\centerline
 {\small
\begin{tabular}{lllllllrrrr}
%\noalign{\smallskip} 
\hline \hline %\noalign{\smallskip}
Position&CO&CO&CO&CO&\CII&\OI&\OI&\OIII&\OIII&\NII$\NOTE{a}$\\
in [$10^{-4}$ erg~s$^{-1}$~cm$^{-2}$ sr$^{-1}$]&$14\TO13$&$15\TO14$&$16\TO15$&$17\TO16$&158~\micron&63~\micron&145~\micron&52~\micron&88~\micron&122~\micron{}\\
%\noalign{\smallskip} 
\hline% \noalign{\smallskip}
DR21 E{}           & 0.25 & 0.72 & 0.51   & 0.33 & 8.2 & 48.2 & 2.9  &3.53&3.08&0.435\\
DR21 C{}           & 1.75 & 2.46 & 0.99   & 0.63 & 8.1 & 49.4 & 6.15 &11.5&4.64&${<}0.75$\\
DR21 W{}           & 0.44 & 0.69 & 0.42   & 0.29 & 4.7 & 10.1 & 1.136&1.78&2.52&0.306\\
DR21 (OH)$\NOTE{b}$& (0.45)& (0.99)&(0.40)&(0.50)& 2.3 & 2.94 & 0.845&(1.27)&1.56&${<}2.7$\\
DR21 FIR1$\NOTE{c}$&${<}0.28$&${<}0.3 $&${<}0.28$&${<}0.25$&3.6&1.78& 0.45 &0.54&1.66&${<}0.6$\\
\hline
\end{tabular}}
\par
\medskip
$\NOTE{a}$
\NII{} was clearly found only toward the outflow positions E{} and W{}. At the other positions, we give $3\sigma$ upper limits.
$\NOTE{b}$
For DR21~(OH), numbers in parentheses are more uncertain ({\it S/N} between $1{-}3$) due to a poorer frequency resolution.
$\NOTE{c}$
At DR21~FIR1, no detection of CO was possible, so we give $3\sigma$ upper limits.
\end{table}