\begin{table}%t3
\caption{Ice column densities. The errors are at 3$\sigma$ level and are dominated by systematics. \label{Vela:table_water_results}}
%\centerline
{\begin{tabular}[!ht]{lllllll}
\hline
\hline
\noalign{\smallskip} 
\multicolumn{2}{c}{Source} & \multicolumn{1}{c}{$\tau$(H$_2$O$_{{\rm ice}}$)}&\multicolumn{1}{c}{$N_{{\rm ice}}$(H$_2$O)}&\multicolumn{1}{c}{$T_{{\rm ice}}$(H$_2$O)}&\multicolumn{1}{c}{$N_{{\rm ice}}$(OCN$^{-}$)$^a$}&\multicolumn{1}{c}{$N_{{\rm ice}}$(CH$_3$OH)$^b$}\\
 & & &\multicolumn{1}{c}{(10$^{18}$ cm$^{-2}$)} &\multicolumn{1}{c}{(K)}&\multicolumn{1}{c}{(10$^{16}$ cm$^{-2}$)}&\multicolumn{1}{c}{(10$^{17}$ cm$^{-2}$)}\\
\noalign{\smallskip} 
\hline
\noalign{\smallskip} 
\object{LLN 8}  &\object{IRAS 08211--4158}  & 0.55 $\pm$ 0.10 & 0.80 $\pm$ 0.15 & 10--40 & $<$1.5& $<$1.0\\
\object{LLN 8b}  &\object{IRAS 08211--4158b} & 1.2\phantom{0} $\pm$ 0.3\phantom{0}  & 1.7\phantom{0} $\pm$ 0.4& 10--40 & ... & ... \\
\object{LLN 13}  &\object{IRAS 08375--4109}  & 1.4\phantom{0} $\pm$ 0.3\phantom{0} & 2.2\phantom{0} $\pm$ 0.4 & 10--40 & $<$0.5& $<$1.0 \\
\object{LLN 13b}  &\object{IRAS 08375--4109b} & 1.1\phantom{0} $\pm$ 0.3\phantom{0} &  1.7\phantom{0} $\pm$ 0.4& 10--40 & ... &...  \\
\object{LLN 17}  &\object{IRAS 08448--4343}  & 2.46 $\pm$ 0.50 & 3.61 $\pm$ 0.70 & 10--40 & \phantom{$<$}4.3 $\pm$ 0.5&\phantom{$<$}2.5 $\pm$ 1.0 \\
\object{LLN 17b}  &\object{IRAS 08448--4343b} & 1.4\phantom{0} $\pm$ 0.3 &  2.2\phantom{0} $\pm$ 0.2& 10--40 & $<$1.5& ...  \\
\object{LLN 19}  &\object{IRAS 08470--4321}  & 0.72 $\pm$ 0.10\phantom{0} & 1.05 $\pm$ 0.2 & 10--40 & $<$0.5& $<$1.0 \\
\object{LLN 41}  &\object{IRAS 09017-4716}  & 1.26 $\pm$ 0.20\phantom{0} & 1.85 $\pm$ 0.4 & 10--40 & $<$1.5&$<$1.0 \\ 
\object{LLN 41b}  &\object{IRAS 09017-4716b} & 0.8\phantom{0} $\pm$ 0.3\phantom{0} &  1.2\phantom{0} $\pm$ 0.4& 10--40 & $<$1.5& ...  \\
\hline
\end{tabular}}
\par
\smallskip
{Notes:}\\ 
$^a$ The 3$\sigma$ upper limits are derived assuming $\Delta \nu=25$ cm$^{-1}$ and 
$A=1.0  \times 10^{-16}$~cm$^{-1}$ molec$^{-1}$. Upper limits derived from low resolution spectra are higher than that from medium resolution because of the possible contamination by CO gas phase lines.
$^b$ The 3$\sigma$ upper limits are derived assuming $\Delta \nu=14$~cm$^{-1}$ and 
$A =2.8 \times 10^{-18}$~cm$^{-1}$~molec$^{-1}$. No upper limits are given for the companion objects because the signal-to-noise ratios are too low to provide scientifically meaningful upper limits.
\end{table}