\begin{table}%t1


\caption{\label{southsample}Southern sample$^{a}$.}
%\centerline
 {
\begin{tabular}{l c c c c c}
\hline
\hline\\[-3.2mm]
Source$^b$       & $V$-range            & rms         &$L_{\rm{H_{2}O}}^c$& Epoch      & Tel$^d$\\ 
                 &($\rm{km \ s^{-1}}$)& ($\rm{mJy}$)&  (\solum)         &            &      \\
\hline
\textbf{NGC 0055}& --592, 752          & 10          & $<$0.001          &25-Jan.-2005 & T\\
\textbf{NGC 0134}&  891, 2236         & 5           & $<$0.08           &09-Sep.-2007 & T\\
\textbf{NGC 0300}& --518, 827          & 9           & $<$0.001          &24-Apr.-2005 & T\\
                 &                    &             &                   &30-Apr.-2005 &\\
                 & --547, 797          & 5           & $<$0.001          &17-Sep.-2007 &\\
                 &                    &             &                   &18-Sep.-2007 &\\
\textit{NGC 1097}&                    & 15          & $<$0.30           &13-Aug.-2003 & \\
\textbf{NGC 1313}& --262, 1083         & 4           & $<$0.005          &02-Jan.-2005 & T\\
\textit{NGC 1365}&                    & 12          & $<$0.39           &09-Jun.-2003 & \\
\textbf{NGC 1559}&  596, 1941         & 5           & $<$0.05           &09-Apr.-2005 & T\\
                 &                    &             &                   &10-Apr.-2005 &\\
\textit{NGC 1672}&                    & 19          & $<$0.41           &27-Jun.-2004 & \\
\textbf{NGC 1792}& 478, 1823          & 5           & $<$0.05           &24-Apr.-2005 & T\\
                 &                    &             &                   &30-Apr.-2005 & \\
\textit{NGC 1808}&                    & 15          & $<$0.18           &05-May-2003 &\\
\textbf{NGC 2997}& 353, 1697          & 7           & $<$0.05           &17-Apr.-2005 & T\\
                 &                    &             &                   &19-Apr.-2005 &\\
                 &                    &             &                   &24-Apr.-2005 &\\
\textbf{NGC 3256$^e$}& see Table~\ref{param}    &             &                   &            & T\\
		 &		      &		    &			&	     & A\\
\textbf{NGC 3620$^e$}& see Table~\ref{param}    &             &                   &            & T\\
		 &		      &		    &			&	     & A\\
\textbf{NGC 3621}& 35, 1380           & 5           & $<$0.02           &26-Mar.-2005 & T\\
                 &                    &             &                   &02-Apr.-2005 & \\
\textit{NGC 4945}&                    &             &  160              &20-Sep.-1978 & \\
                 &                    &             &                   &22-Sep.-1978 & \\
\textbf{NGC 5128$^f$}&--50, 1200      &   --         & --                 &10-Apr.-2005 & T \\
                 &                    &             &                   &17-Apr.-2005 &\\
                 &                    &             &                   &24-Apr.-2005 & \\
                 &407, 668            & 2           &  $<$0.02          &29-Jun.-2006 & A\\
\textit{NGC 6744}&                    & 15          & $<$0.13           &17-May-2002 & \\
\textit{NGC 7552}&                    & 13          & $<$0.41           &19-Jun.-2004 &\\
\textit{NGC 7582}&                    & 13          & $<$0.40           &27-Jun.-2004 &\\
\textbf{NGC 7793}& --445, 899          & 7           & $<$0.002          &26-Aug.-2007 & T\\
                 &                    &             &                   &31-Aug.-2005 &\\
\hline
\end{tabular}}
\par
\medskip
$^{a}$ For coordinates, systemic velocities, 100 $\rm{\mu m}$ flux densities, and references see the Table containing the entire sample of FIR bright galaxies.\\
$^b$ Bold-faced source names refer to sources observed in this study; source names in italics refer to previously measured targets. For NGC~4945, see Dos Santos \& L\`{e}pine (\cite{santos79}), Batchelor et~al. (\cite{batche82}), Greenhill et~al. (\cite{green97}). For the other sources in italics, see Kondrakto et~al. (\cite{kondra06}). \\
$^c$ Upper limits to maser luminosities are derived from $L_{\rm{H_{2}O}}/[\solum]=0.023 \times S/[\rm{Jy}] \times \Delta \textit{v}/[\rm{km \ s^{-1}}] \times \textit{D}^{2}/[\rm{Mpc^{2}}]$, where \textit{S} is 3 times the rms, in Col.~4, and $\Delta v$ is the channel width, $\rm{0.5 \ km\  s^{-1}}$ and $\rm{1.7 \ km \ s^{-1}}$ in our Tidbinbilla and ATCA observations (NGC~5128/Cen A only), respectively.\\
$^d$ Telescope: T = Tidbinbilla; A = ATCA.\\
$^e$ Newly detected maser.\\
$^f$ Observed with ATCA, because the 22~GHz continuum was too strong to obtain single-dish spectra with high baseline quality.
\end{table}