\begin{table}%t4
\caption{\label{table:prop}Source properties derived from the gas and dust. The table has been rearranged compared with Table~\ref{label:source} to reflect the classification in Sect.~6.2 } \small%\centerline
 {
\begin{tabular}{l l l l l l r l l}
\hline \hline 
&&&&&&&& \\[-8pt]
Source  	& $\alpha_{\rm{IR}}$ & $N_{\rm{H}_2}^a$& $\Delta\alpha^b$ &Mass$^c$ & $L_{\rm{bol}}$ & $T_{\rm{bol}}$ & $C_{850}$$^d$ & $C_{\rm{HCO^+}}$$^d$ \\ 
	        &  &(10$^{22}$ cm$^{-2})$&  &(10$^{-2}$ $M_{{\odot}})$&(10$^{-1}$ $L_{\rm{\odot}}$) &(K) & &\\ 
\hline
\multicolumn{5}{c}{{\bf Embedded sources}}\\ 
%\hline
GSS 30$^e$               &1.46   &23.3/19.4*& 2.6 &  20.5  & 33  & 123 & 0.55& 0.69\\ 
LFAM 1$^e$               &0.73   &50*       & 2.6 &  17.1  & 8.3 & 86  & 0.59& 0.69\\ 
VLA 1623                 & no    &441*      & --   & 111    & 2.7 & 12  & 0.7 & 0.72 \\ 
WL 12	                 &2.49   &10.5/15.2*& 3.1 & 4.6    & 34  & 155 & 0.26& 0.81\\ 
LFAM 26                  &1.27   &14.0/18.5*& 4.4 & 4.5    & 0.44& 238 & 0.40& 0.69\\ 
WL 17	                 &0.61   &8.4*      &  1.0& 4.0    & 6.7 & 323 & 0.22& 0.71\\ 
Elias 29                 &1.69 &22.7/33.6*  & 1.5 &6.2     & 25  & 424 & 0.49& --$^f$ \\ 
IRS 37$^e$	         &0.25   &20.8      & 1.0 &1.2     &3.8  & 243 & 0.58    & 0.72\\ 
WL 3$^e$                 &--0.03  &19.2/9.7* & 2.3 &2.9     & 4.6 & 192 & 0.25    & 0.67\\ 
WL 6	                 &0.72   &11.4      & -- &$<$0.4    & 8.5 & 394 & U       & 0.77\\ 
IRS 43	                 &1.17   &14.2/20.7* & 2.3 &17.1   & 10  & 134 & 0.58& 0.79\\ 
IRS 44	                 &2.29   &12.6/30.2D* & 2.9 &8.0   & 11  & 140 & 0.33& 0.80\\ 
Elias 32                 &--0.03  &6.8/140*  & 3.7 &41.9    &5    & 321 & 0.37& 0.70\\ 
Elias 33                 &--0.12  &13.1/96* & 3.1 &28.2     &12   & 460 & 0.6 & 0.64\\ 
IRS 54	                 & 0.03  &7.4       & 1.2 &3.1     & 7.8 & 486 & 0.8  & 0.80\\ 
IRAS 16285-2355          & 1.23  &5.0/41.9D* & 3.1 &10.3   & 0.57& 77  & 0.45&0.80\\ 
IRS 63	                 & 0.14  &3.7/84.0D* & --  &16.4    & 13  & 363 & 0.75& 0.60\\ \hline
\multicolumn{5}{c}{{\bf Confused sources}}\\ %\hline
CRBR 2324.1-1619         &0.87   & 31.6/70.5*& 5.2 &39.3      & 0.44& 283 & U& U\\ 
GY51                     & 0.05  &27.7*     & 4.5 &11.1      & 2.3 & 706 & U&U\\ 
 WL19                    &--0.43  & 13.7/16.8*& 4.9 &5.5     & 1.5 & 730 & 0.15& 0.53\\ 
IRS 42	                 &--0.03  & 8.7/14.2* & 1.3 &4.7     &14   & 540 & 0.44& 0.60\\ 
GY 256	                 &--0.05  & 11.8& -- &$<$0.2 &1.1  & 104 & U& 0.70\\ 
\hline
\multicolumn{5}{c}{{\bf Disks}}\\ %\hline
C2D-162527.6             & 0.36  & --   &  -- &$<$0.4 & 0.16& 1051& U&U\\  
GSS 26	                 &--0.46  &24.3D*& 1.8  &10.2     & 3.2 & 877 & 0.65&U\\ 
CRBR 2315.8-1700         & 0.69  &17.6*& 1.0  &5.1     &0.93 & 456 & 0.38&0.74 \\ 
CRBR 2317.3-1925         &--0.56  &12.6*& 0.3  &1.1     &0.11 & 1105& 0.85 &S\\ 
VSSG 1	                 &-0.73  &20.1*& --  &2.0     &5.8  & 930 & 0.74&SU\\ 
CRBR 2339.1-2032         &0.45   &6.7* & --  &2.0     & 0.55& 426 & 0.55& 0.58\\     
WL 2                     &0.02   & --   & --  &1.0    & 0.88& 573 &0.3 & 0.58\\ 
GY 224	                 &--0.05  &10.9*& 1.0  &2.4     & 2.1 & 614 & 0.63&SU\\ 
 WL 20S	                 &2.75   &10.9/15.3D*& 1.0  &3.9     & 4.5 & 85  & 0.57&SU\\ 
IRS 48	                 &0.88   & 5.7/15.2D*& 2.1  &1.2     &81   & 238 &0.70&U\\ 
GY 312                   &0.64   & --  &  -- &$<$0.2 & 0.73&285  &U & 0.3\\  
IRS 51	                 &--0.15  & 4.4/18.4D*& 2.3  &5.0    & 8   & 548 & 0.27&0.59\\ 
C2D-162741.6             &0.32   & --   &  -- &2.3     & 0.28&279  & U&U\\ 
C2D-162748.2             &1.55   & --   &  -- &0.4     & 0.17&241  & U&SU\\ 
C2D-162857.9             & 0.67  & --    & --  &5.6    & 0.22& 402 & U&SU\\ 
Haro 1-4                 &--0.89 & --    & --  &0.45    & 5.6 &762  & U&SU\\ 
DoAR 25	                 &--1.12 &38.6*     & --  &3.4     & 4.7 &1422 & 0.90&SU\\ 
OphE MM3                 &--0.33 & 12.0/13.4*& 3.4  &2.3     & 0.17&45   & U& 0.68\\ 
SR 21                    &--0.79 &33.6*     &  -- &3.1     & 1.8 & 1070& 0.89&SU\\ 
CRBR 2422.8-3423         &1.01  &106.6*     & 2.3  &20.5      & 4.4 & 157 & U &--$^f$\\ 
IRS 46	                 &0.18  & 6.3/15.1* & 2.8  &3.3     & 1.9 & 684 & U &SU\\ 
SR 9                     &--1.07 & --     & --  &$<$0.4 & 8.7 & 1588& U&SU\\ 
2MASS 16282              &--1.55 & --     & --  &1.7     & 0.84& 66  & U&SU\\ 
\hline
\end{tabular}}
\medskip
$^a$ Column densities marked with * are calculated from the SCUBA dust maps. Embedded sources where a large disk contribution is likely are indicated with a~D. Note that no column densities could be calculated from the dust below 1~$\times$ $10^{23}$~cm$^{-2}$.   \\
$^b$ $\Delta \alpha$ is an {\it upper limit} to change in 2$-$24~$\mu$m spectral slope due to the reddening by foreground clouds at this source. This is derived by considering the mean column density at~45$''$ off the source position.   \\
$^c$ Upper limit derived from the 850~$\mu$m data using the relation from \citet{Shirley00}, with the assumption that all 850~$\mu$m emission originates within a protostellar envelope.  \\
$^d$ U~= Undetected or Unobserved, S~= single position spectrum available only.  \\
$^e$ Circumbinary envelope.  \\
$^f$ Although both Elias 29 and CRBR 2422.8-3423 were observed, these sources are located near the edge of a field and do not have sufficient coverage to obtain a concentration parameter for the~HCO$^+$. 
\end{table}