\begin{table}%t4
\par
\caption{\label{tab:massresults}Envelope and disk masses for the full sample of Class~0 and~I sources.}
%\centerline
 {\begin{tabular}{llll}\hline\hline
Source      & $M_{\rm env}$$^{a}$ & $M_{\rm disk}$$^{b}$  & $M_{\rm star}$$^{c}$ \\
            & [$M_\odot$]   & [$M_\odot$] & [$M_\odot$] \\ \hline
\multicolumn{4}{c}{\emph{Class 0}} \\[1.0ex]
L1448-mm    & 0.96 & 0.044 & $\ldots$ \\
IRAS2A      & 1.0  & 0.056 & $\ldots$ \\
IRAS4A1     & 4.5$^{d}$  & 0.46  & $\ldots$ \\ 
IRAS4A2     & --$^{d}$   & 0.25  & $\ldots$ \\
IRAS4B      & 2.9$^{d}$  & 0.24  & $\ldots$ \\
IRAS4B$'$   & --$^{d}$   & 0.089 & $\ldots$ \\
L1527       & 0.56 & 0.029 & $\ldots$ \\
L483        & 0.82 & 0.0$^e$   & $\ldots$ \\
B335        & 0.93 & 0.017 & $\ldots$ \\ 
L1157       & 0.94 & 0.12  & $\ldots$ \\[1.0ex]
\multicolumn{4}{c}{{\it Class I}} \\[1.0ex]
L1489-IRS   & 0.11          & 0.018       & 1.3$^{f}$    \\
TMR1        & 0.11          & 0.0094      & $\ldots$    \\
TMC1A       & 0.12          & 0.035       & 0.35--0.7$^g$ \\
GSS30-IRS3  & 0.096         & 0.026       & $\ldots$    \\
WL~12        & 0.054         & 0.011       & $\ldots$    \\
Elias 29    & 0.047         & 0.011       & 2.5$^{h}$         \\
IRS~43       & 0.026         & 0.0081      & 1.0$^{i}$         \\
IRS~54$^j$   & $\ldots$      & $<$0.001    & $\ldots$    \\
IRS~63       & 0.098         & 0.053       & 0.36$^{h}$        \\ \hline
\end{tabular}}
\par
\smallskip
$^{a}$ Envelope mass determined from the direct scaling of the JCMT peak flux
(minus the disk contribution). $^{b}$ Disk mass assuming a uniform dust temperature of
30~K. $^{c}$ Central mass from Keplerian velocity profiles (see specific references for details). $^{d}$IRAS4A1 and IRAS4A2,
respectively IRAS4B and IRAS4B$'$ have larger scale circumbinary
envelopes.  $^e$ The compact flux in L483 is consistent with being solely from the
larger scale envelope. $^{f}$ Stellar mass from \cite{brinch07b}, envelope and disk masses calculated under same
assumptions as for the remainder of the sources using the continuum data from \citeauthor{brinch07b} $^g$ \cite{brown99chandler}. 
$^{h}$ \cite{lommen08}, $^{i}$ This work. $^j$ IRS~54 is undetected in both interferometric and single-dish maps. A 3$\sigma$ upper limit to its disk mass is estimated from the SMA observations.
\end{table}