\begin{table}%t1
\caption{Characteristics of the sources.\label{vela:table_objects}}
%\centerline
{\begin{tabular}[!ht]{llllllllll} 
\hline 
\hline
\noalign{\smallskip} 
& & \multicolumn{1}{c}{(1)}&\multicolumn{1}{c}{(2)}&\multicolumn{1}{c}{(3)}&\multicolumn{1}{c}{(4)}&\multicolumn{1}{c}{(5)}&\multicolumn{1}{c}{(6)}&\multicolumn{1}{c}{(7)}&\multicolumn{1}{c}{(8)}\\
\multicolumn{2}{c}{Source}&\multicolumn{1}{c}{$L_{{\rm NIR}}$}&\multicolumn{1}{c}{$L_{{\rm MIR}}$}&\multicolumn{1}{c}{$L_{{\rm IRAS}}$}&\multicolumn{1}{c}{$L_{{\rm submm}}$}
& \multicolumn{1}{c}{$L_{\rm bol}$} &\multicolumn{1}{c}{$M_{{\rm env}}$}&\multicolumn{1}{c}{$A_{{\rm V}}$}& \multicolumn{1}{c}{$N_*$}\\
&\multicolumn{1}{c}{}&\multicolumn{1}{c}{(\%)} &\multicolumn{1}{c}{(\%)} &\multicolumn{1}{c}{(\%)} &\multicolumn{1}{c}{(\%)} &\multicolumn{1}{c}{($L_{\odot}$)} &\multicolumn{1}{c}{($M_{\odot}$)}&\multicolumn{1}{c}{(Mag)}&\multicolumn{1}{c}{(pc$^{-2}$)}\\
\noalign{\smallskip} 
\hline
\noalign{\smallskip} 
\object{LLN 8}& \object{IRAS 08211--4158}   &  5.3 &  10.5 & 53.3 & 31.0  & 141$^{a}$ & \multicolumn{1}{c}{...}    &  \multicolumn{1}{c}{...}   &  \multicolumn{1}{c}{...} \\
\object{LLN 13}& \object{IRAS 08375--4109}  &  5.3 & \ 6.8 & 72.8 & 17.7  & 960$^{b}$ & 2.6$^{b}$ & $\geq$40$^{a}$ &800$^{b}$  \\
\object{LLN 17}& \object{IRAS 08448--4343}  &  1.3 & \ 4.0 & 60.8 & 33.9  & 3100$^{b}$ & 6.4$^{b}$ & $\sim$40$^{a}$&3400$^{b}$ \\
\object{LLN 19}& \object{IRAS 08470--4321}  &  4.8 &  20.3 & 65.8 & \ 9.1 & 1600$^{b}$ & 3.5$^{b}$ & $\sim$40$^{a}$&2400$^{b}$ \\
\object{LLN 41}& \object{IRAS 09017--4716}  &  ... &  ...  & 80.7 & 19.3      &  470              & ...    & ...   \\
\noalign{\smallskip} 
\hline
\noalign{\smallskip} 
\object{LLN 20}$^{c}$& \object{IRAS 08476--4306}   &  0.5     & 3.1      &  66.8    &  29.7  &  1600\ $^{b}$ & 2.2$^{b}$  &  &  3900$^{b}$\\
\object{LLN 33}$^{c}$& \object{IRAS 08576--4314}   &  2.6     & 12.6      & 80.6     & 4.2 & 91$^{a}$   & ...  & ...  & ... \\
\object{LLN 39}$^{c}$& \object{IRAS 09014--4736}   &  1.3      & 5.7      & 71.1     & 22.0  & 807$^{a}$  & ...  & ...  & ... \\
\object{LLN 47}$^{c}$& \object{IRAS 09094--4522}   &  3.4     & 13.3      & 74.4     & 8.9   &  21$^{a}$  & ...  & ...  & ... \\
\hline
\end{tabular}}
\par
\smallskip
  {Notes:} The dots refer to values which are not available in the literature.\\
    {Columns 1--4:} 
  The fractional luminosities are computed by
  \cite{Liseau1992AetA...265..577L}. The indices refer to the
  wavelength range 1--5~$\mu$m (Col.~1); 5--12~$\mu$m (Col.~2),
  12--100~$\mu$m (Col.~3) and 0.1--1 mm (Col.~4) for NIR, MIR, IRAS
  and submm, respectively. $L_{{\rm submm}}$ are estimated by
  \cite{Liseau1992AetA...265..577L} when the millimeter observations do
  not exist.  
  {Column 5:} bolometric luminosity.
    {Column 6:} the envelope masses ($M_{{\rm env}}$) are derived
  from 1~mm continuum flux by \cite{Massi1999AetAS..136..471M} for four
  of our sources. Envelope masses are only given for those sources for
  which millimeter observations have been carried out.    
  {Column 7:} extinction estimated by \citet{Liseau1992AetA...265..577L}.
    {Column 8:} $N_*$ refers to the maximum stellar surface
  densities measured.\\
    {Reference:} $^a$ \cite{Liseau1992AetA...265..577L};
  $^b$ \cite{Massi1999AetAS..136..471M}; $^c$ {VLT-ISAAC} data
  analyzed by \cite{Pontoppidan2003AetA...408..981P}.
\par
\end{table}