\begin{table}%t1
\par
\caption{\label{sample}Sample of embedded protostars.}
%\centerline
 {
\begin{tabular}{llllll}
\hline\hline
Source              & RA [J2000] & Dec [J2000] & $T_{\rm bol}$ [K] & $L_{\rm bol}$ [$L_\odot$]& $d$ [pc] \\ \hline
\multicolumn{6}{c}{{\it Class 0}}\\[1.0ex]
L1448-mm            &  03 25 38.9  & $+$30 44 05.4  &   77  & 5.3    & 220 \\[1.0ex]
\multicolumn{5}{l}{NGC~1333:} \\
\phantom{xx}-IRAS2A             &  03 28 55.6  & $+$31 14 37.1  &   57  & 20$^{a}$    & 220 \\
\phantom{xx}-IRAS4A-SE          &  03 29 10.5  & $+$31 13 31.0  &   43  & 5.8     & 220 \\
\phantom{xx}-IRAS4A-NW          &  03 29 10.4  & $+$31 13 32.3  &   --  & --      & 220 \\
\phantom{xx}-IRAS4B             &  03 29 12.0  & $+$31 13 08.1  &   55  & 3.8$^{b}$ & 220\\
\phantom{xx}-IRAS4B$'$          &  03 29 12.8  & $+$31 13 07.0  &   --  & --      & 220 \\[1.0ex]
L1527               &  04 39 53.9  & $+$26 03 09.8  &   59  & 2.0     & 140 \\
L483                &  18 17 29.9  & $-$04 39 39.6  &   60  & 9.0     & 200 \\
B335                &  19 37 00.9  & $+$07 34 09.7  &   60  & 3.0     & 250 \\
L1157               &  20 39 06.3  & $+$68 02 16.0  &   42  & 6.0     & 325 \\[1.0ex]
\multicolumn{6}{c}{\emph{Class I}}\\[1.0ex]
L1489-IRS           &  04 04 42.9  & $+$26 18 56.3  &  238  & 3.7     & 140 \\
TMR1                &  04 39 13.9  & $+$25 53 20.6  &  144  & 3.7     & 140 \\
TMC1A               &  04 39 35.2  & $+$25 41 44.4  &  172  & 2.2     & 140 \\
GSS30-IRS3          &  16 26 21.7  & $-$24 22 50.6  &  300  & 14$^{c}$ & 125 \\
GSS30-IRS1          &  16 26 22.2  & $-$24 23 01.9  &  --   & --      & 125 \\
WL~12                &  16 26 44.2  & $-$24 34 48.7  &  440  & 2.6     & 125 \\
Elias 29            &  16 27 09.4  & $-$24 37 20.0  &  350  & 41    & 125 \\
IRS~43               &  16 27 26.9  & $-$24 40 50.6  &  310  & 6.0     & 125 \\
IRS~54               &  16 27 51.8  & $-$24 31 45.4  &  740  & 2.5     & 125 \\
IRS~63               &  16 31 35.7  & $-$24 01 29.6  &  530  & 3.3     & 125 \\ \hline
\end{tabular}}				            
\smallskip
\par
$^{a}$For NGC~1333-IRAS2A \cite{evans09} quote a luminosity of 76~$L_\odot$. Estimating the luminosity from scaling the 70~$\mu$m flux using the approach of \cite{dunham08} gives a luminosity of 19.6~$L_\odot$, which agrees well with previous estimates from modeling the SED in the range 16--20~$L_\odot$. The higher luminosity in the c2d compilation is a result of the SED of IRAS2A being unconstrained at 24~$\mu$m (Dunham, priv. comm) -- and we therefore adopt a luminosity of 20~$L_\odot$ for this source. $^{b}$ The Spitzer maps of NGC~1333-IRAS4B shows significant emission from a nearby outflow shock within the typical single-dish beam. As total luminosity for this source, we adopt the sum of the two components, SSTc2d J032912.06+311305.4 and SSTc2d J032912.06+311301.7, from \cite{evans09}. $^{c}$ The emission from GSS30-IRS3 (LFAM1) and GSS30-IRS1 are not separated in the Spitzer catalog (the latter dominates the emission and its luminosity is quoted here).
\vspace*{3mm}
\end{table}