\begin{table}%t3
\caption{Line parameters of newly detected masers.}\label{t3}
%\centerline
 {\begin{tabular}{lcccrrcccl}
\hline\hline
Source & Adopted          & Epoch & $\int{S{\rm d}V}^{a}$    & $V_{\rm LSR,opt}^{a,b}$ & $\Delta V_{1/2}^{a}$ &
         Channel          & rms   & log~$L_{\rm H_2O}^{d}$  & Comments \\
       & distance         &       &                               &                              &                           &
         width$^{c}$ &       &                               &          \\  
       & (Mpc)            & (2002)& (mJy km~s$^{-1}$)            & (km~s$^{-1}$)               & (km~s$^{-1}$)            &
         (km~s$^{-1}$)   & (mJy) & ($L_{\odot}$)                 &          \\  
\hline 
Mrk~1066          & 48&Mar. 07& $ 696\pm61  $& $3547.2\pm1.4$ &$  38.7\pm04.6$ & 1.08 & 5.3&    1.6     & see Fig.~\ref{mrk1066a} \\
                   &   &      & $ 169\pm12  $& $3635.9\pm0.1$ &$   2.1\pm00.2$ & 1.08 & 5.3&    1.0     & see Fig.~\ref{mrk1066a} \\
                   &   &      & $ 171\pm17  $& $3635.9\pm0.1$ &$   1.9\pm00.2$ & 0.07 &29.7&    1.0     & see Fig.~\ref{mrk1066b} \\
                   &   &Mar. 10& $ 822\pm59  $& $3547.8\pm1.3$ &$  38.3\pm03.4$ & 1.08 & 5.6&    1.6     & see Fig.~\ref{mrk1066a} \\
                   &   &      & $ 193\pm13  $& $3636.2\pm0.1$ &$   2.1\pm00.2$ & 1.08 & 5.6&    1.0     & see Fig.~\ref{mrk1066a} \\
                   &   &      & $ 157\pm16  $& $3636.1\pm0.1$ &$   1.2\pm00.2$ & 0.07 &34.9&    0.9     & see Fig.~\ref{mrk1066b} \\
                   &   &May 03& $ 566\pm16  $& $3552.8\pm7.7$ &$  46.2\pm16.9$ & 1.08 &15.0&    1.5     & see Fig.~\ref{mrk1066a} \\
                   &   &      & $ 166\pm33  $& $3635.9\pm0.2$ &$   1.7\pm00.4$ & 1.08 &15.0&    0.9     & see Fig.~\ref{mrk1066a} \\
                   &   &Sep. 27& $ 143\pm31  $& $3635.2\pm0.2$ &$   2.0\pm00.5$ & 1.08 &13.7&    0.9     & see Fig.~\ref{mrk1066a} \\
                   &   &      &  	     &	  &                &           &	    &             \\
Mrk~34$^{e}$ &205&Mar. 08& $  \phantom{0}46\pm14 \phantom{0} $&$14661.2\pm0.4$ &$   2.1\pm00.8$ & 1.16 & 5.8&    1.6     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 354\pm52 \phantom{0} $&$14837.6\pm2.3$ &$  31.9\pm05.3$ & 1.16 & 5.8&    2.5     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 417\pm78 \phantom{0} $&$15771.7\pm8.7$ &$  88.2\pm16.2$ & 9.29 & 1.9&    2.6     & see Fig.~\ref{mrk34b} \\
                   &   &Mar. 17& $ 335\pm57\phantom{0}  $&$14840.5\pm2.9$ &$  36.5\pm07.8$ & 1.16 & 5.5&    2.5     & see Fig.~\ref{mrk34a} \\
                   &   &May 07& $  \phantom{0}77\pm24\phantom{0}  $&$14674.9\pm0.8$ &$   5.0\pm01.9$ & 1.16 & 6.6&    1.9     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 323\pm62 \phantom{0} $&$14838.7\pm2.9$ &$  31.2\pm07.6$ & 1.16 & 6.6&    2.5     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 995\pm122 $&$15754.9\pm8.0$ &$ 130.4\pm18.4$ & 9.30 & 2.3&    3.0     & see Fig.~\ref{mrk34b} \\
                   &   &May 09& $ \phantom{0} 67\pm25 \phantom{0} $&$14658.2\pm0.8$ &$   4.7\pm02.2$ & 4.67 & 3.4&    1.8     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 559\pm81 \phantom{0} $&$14837.4\pm3.1$ &$  43.9\pm08.2$ & 4.67 & 3.4&    2.7     & see Fig.~\ref{mrk34a} \\
                   &   &      & $ 607\pm92 \phantom{0} $&$15787.2\pm9.6$ &$ 115.5\pm19.9$ &18.67 & 1.4&    2.8     & see Fig.~\ref{mrk34b} \\
                   &   &      & $ 117\pm32 \phantom{0} $&$15738.2\pm1.1$ &$   6.9\pm03.0$ & 4.67 & 3.2&    2.1     & see Fig.~\ref{mrk34b} \\
                   &   &      & $ 394\pm87 \phantom{0} $&$15803.1\pm4.2$ &$  47.8\pm15.0$ & 4.67 & 3.2&    2.6     & see Fig.~\ref{mrk34b} \\
                   &   &      &  	     &	  &                &           &	    &             \\
NGC~3556          & 12&Mar. 12& $ 505\pm72 \phantom{0} $&  $738.5\pm1.1 $&$  15.1\pm2.2 $ & 1.06 &11.6&    0.2     & see Fig.~\ref{ngc3556} \\
                   &   &Mar. 15& $ \phantom{0} 99\pm29\phantom{0}  $&  $738.0\pm0.3 $&$   2.1\pm0.5 $ & 1.06 &10.1&  --0.5     & see Fig.~\ref{ngc3556} \\
                   &   &      & $ 421\pm78 \phantom{0} $&  $740.3\pm1.6 $&$  17.9\pm4.8 $ & 1.06 &10.1&    0.1     & see Fig.~\ref{ngc3556} \\
                   &   &May 05& $ 229\pm35 \phantom{0} $&  $737.2\pm0.4 $&$   4.8\pm0.8 $ & 1.06 &10.9&  --0.1     & see Fig.~\ref{ngc3556} \\
                   &   &Sep. 27& $ 329\pm75 \phantom{0} $&  $737.1\pm1.1 $&$  10.0\pm2.9 $ & 4.21 & 6.5&    0.0     & see Fig.~\ref{ngc3556} \\
                   &   &      &  	     &                &                &           &	    &             \\
Arp~299           & 42&Mar. 16& $6210\pm242 $& $3101.8\pm05.1$&$ 260.2\pm11.5$ & 4.30 & 4.8&    2.4     & see Fig.~\ref{arp299a} \\
\hline
\end{tabular}}
\medskip
$^a$ Obtained from Gaussian fits. \\
$^b$ See the caption to Fig.~\ref{mrk1066a}. \\
$^c$ Channel width of the spectra used for the Gaussian fits. Some of the 
   spectra shown in Figs.~\ref{mrk1066a}--\ref{arp299b} are smoothed. \\
$^d$ $L_{\rm H_2O}$/[$L_{\odot}$] = 0.023 $\times$ $\int{S {\rm d}V}$/[Jy~km~s$^{-1}$] $\times$ $D^2$/[Mpc$^2$]. \\
$^e$ To the observations of the high velocity feature (15787~km~s$^{-1}$) from May 9: the first Gaussian 
   fit refers to the smoothed profile shown in Fig.~\ref{mrk34b}; the latter two component fit refers to the 
   unsmoothed spectrum with a channel spacing of 4.7~km~s$^{-1}$. \\
\end{table}