\begin{table}%t1
 \caption{H$_2$O Observations and abundance limits.}\label{tbl-table}
\small%\centerline
{
\begin{tabular}{lcccccccccl}
            \hline\hline
%&&&&&&&&&& \\[-8pt]
            Source      & Coordinates & $T_{\rm sys}$ & $t_{\rm int}$
& rms$^a$ & $\Delta V({\rm CO})$  & $I({\rm H_2O})$$^b$ & $D$ & $M_{\rm H_2}$$^c$ &
$x(o{\rm -H_2O})$$^d$ & CO Reference \\
& (J2000) & (K) & (hr) & (mK) & (km s$^{-1}$) & (K km s$^{-1}$) & (Mpc) & ($10^9$ $M_\odot$) & & \\
            \hline
%&&&&&&&&&& \\[-8pt]
NGC 253 & 00:47:35.2 $-$25:17:20 &  4100 &   18.5     & 13  & 450  & 1.6
& 2.5 & 0.60 & $<$$2.0\times 10^{-9}$ & Sorai et~al. (\cite{s00}) \\
IC 342  & 03:46:49.6  +68:05:45   &  3700  &  25.0 &  10   & 130 & 0.56 & 3.9 & 0.39 & $<$$2.6\times 10^{-9}$ & Helfer et~al. (\cite{h03}) \\
M 82   & 09:55:54.0  +69:40:57   &  3400  & 20.1  &  10   & 400  & 1.9
& 3.9 & 1.56 & $<$$1.7\times 10^{-9}$ & Walter et~al. (\cite{w02}) \\
N4258  & 12:18:57.5  +47:18:14    &  4300  &  17.4 & 13   & 450  & 1.4 & 8.1 & 0.81 & $<$$1.3\times 10^{-8}$ & Helfer et~al. (\cite{h03}) \\
CenA  &  13:25:27.6 $-$43:01:08 &  4500  & 17.2 &  10        & 600  & 1.2 & 4.0 & 0.29 & $<$$7.8\times 10^{-9}$ & Eckart et~al. (\cite{e90}) \\
M 51  &   13:29:53.1 +47:11:48 
   &  3900   & 23.7   & ~~8 &   200      &  0.56  & 7.7 & 1.64 & $<$$2.4\times 10^{-9}$ & Helfer et~al. (\cite{h03}) \\
\hline
\end{tabular}}
\medskip
$^a$ Rms noise at a resolution of 2.7~km~s$^{-1}$.
$^b$~Three~sigma upper limit integrated over $\Delta V({\rm CO}$); values for M~82 and NGC~253 include scaling by~1.61 and~1.15, respectively, to account for pointing errors; see text.
$^c$~Assumes $X_{\rm CO} = 2$~$\times$ $10^{20}$~H$_2$~cm$^{-2}$ (K~km~s$^{-1}$)$^{-1}$.
$^d$~Three~sigma upper limit assuming $n_{\rm H_2} = 10^6$~cm$^{-3}$ and $T_K = 40$~K. Depending on the average density of the molecular gas on large scales and the mass fraction in dense
cores, these abundance limits could be larger by a~factor of~$\sim$$10$
or more (see text).
\end{table}