\begin{table}%t2
\caption{\label{coldens}Parameters given by the HFS fit of each ND and NH transition.}
\small
%\centering
\par
\begin{tabular}{c c c c c c}
\hline\hline\noalign{\smallskip}
Molecule  & $\tau(J_{\nu}(T_{\rm ex}) - J_\nu(T_{\rm bg})-T_{c})$ & $\Delta \varv$ & $\tau$ & $T_{\rm ex}$ & $N$ \\ 
\& transition& K & km s$^{-1}$ & & K & cm$^{-2}$\\
\hline\noalign{\smallskip}
ND (0$_1$--1$_2$) & $-$2.57 $\pm$ 0.33 & 0.74 $\pm$ 0.14 & 28.8 $\pm$ 3.9 & 4.6 & $(1.7 \pm 0.6) \times 10^{14}$\\
ND (0$_1$--1$_1$) & $-$1.18 $\pm$ 0.13 & 0.82 $\pm$ 0.14 & 7.9 $\pm$ 2.1 & 4.5 & $(0.9 \pm 0.4) \times 10^{14}$\\
NH (0$_1$--1$_0$) & $-$3.78 $\pm$ 0.58 & 0.60 $\pm$ 0.08 & 8.4 $\pm$ 2.1 & 9.5 &  $(2.0 \pm 0.8) \times 10^{14}$\\
NH (0$_1$--1$_2$) & $-$27.3 $\pm$ 0.27 & 0.64 $\pm$ 0.08 & 34.9 $\pm$ 4.8 & 7.7 & $(1.8 \pm 0.4) \times 10^{14}$\\
NH (0$_1$--1$_1$) & $-$18.6 $\pm$ 0.75 & 0.63 $\pm$ 0.08 & 25.1 $\pm$ 1.6 & 8.8 & $(2.2 \pm 0.4) \times 10^{14}$\\
\hline
\end{tabular}
\tablefoot{$\tau$ is the total optical depth, $T_{\rm ex}$ the excitation temperature, $J_{\nu}(T_{\rm ex})$ the radiation temperature at the frequency of the transition, $J_\nu(T_{\rm bg})$ the radiation temperature of the cosmological background at $T_{\rm bg}=2.7$~K, $T_{\rm c}$ the brightness temperature of the continuum,  $\Delta \varv$ the linewidth (full width at half maximum), and $N$ the total measured column density in the given species. $T_{\rm ex}$ was deduced from Col.~(2). Because of uncertainties in some stages of the data reduction process, we estimate that the linewidths are not known to better than about 0.25~MHz. It is this uncertainty that we quote here in Col.~(3). }
\end{table}