\begin{table}%T3
\caption{\label{tab3}Parameters for BCGs.} 
\small %\centering
\par
\begin{tabular}{ccccccccccc}
\hline
\hline\noalign{\smallskip}
BCG&pc &j/cj & $\beta \cos \theta$&$S_{\rm c,5}$&Log~$P_{\rm c,5}$&$S_{\rm t,408}$&Log~$P_{\rm t,408}$&$S_{\rm VLBI}$/&Core&Notes\\
&structure&ratio&&mJy&W/Hz&mJy&W/Hz&$S_{\rm c, 5~GHz}$($\%$)&dominance&\\
\hline  
NGC~708& c   &--&--&5&21.47&364&23.33&60&0.26&5\\ 
NGC~910& n.d.&--&2&--&--&--&--&$<$25&--&5\\ 
3C~75A&1s&$\geq$6.2&$\geq$0.35&6&21.87&190&23.37&100&0.60&1\\ 
3C~75B&1s&$\geq4.6$&$\geq$0.3&20&22.39&190&23.37&100&2&1\\ 
3C~84&2s&2&0.14&28.17~$\times$~10$^{3}$&25.29&51.68~$\times$~10$^{3}$&25.56&80&70.79&2\\ 
UGC~3274&n.d.&--&--&$<$1.4&--&--&--&--&--&5\\
UGC~2489&1s&$\geq$2.8&$\geq$0.2&4&22.32&2.83~$\times$~10$^{3}$&25.17&90&0.13&3\\
NGC~2329&1s&$\geq$4.5&$\geq$0.29&160&23.14&1300&24.05&50&4.3&4\\
CGCG~261-059&1s&$\geq$1.8&$\geq$0.12&1.5&21.71&6.54&22.34&100&1.8&5\\ %125
NGC~2832&n.d.&--&--&2.4&--&--&--&$<$21&--&5\\
NGC~3550&n.d.&--&--&$<$1.4&--&--&--&--&--&5\\
4C~29.41&1s&$\geq$3.8&$\geq$0.26&41&23.33&135.2&23.84&100&8.71&6\\
IC~2738&n.d.&--&--&--&--&--&--&--&--&5\\
IC~708&1s&$\geq$6.5&$\geq$0.36&110&23.47&901.1&24.39&40&5.62&7\\ %32
IC~712&n.d.&--&--&14.02&22.58&48.72&23.12&$<$3&4.37&11\\
NGC~3842&n.d.&--&--&9&22.98&101.88&23.03&$<$8&0.36&11\\
3C~264&1s&$\geq$6&$\geq$0.34&200&23.32&17~$\times$~10$^{3}$&25.25&100&1.17&8\\ %63
NGC~4874&1s&$\geq$1.6&$\geq$0.09&1.1&21.13&351.96&23.63&100&0.08&9\\ %61
UGC~10143&n.d.&--&--&$<$2&$<$21.77&14.87&22.64&$-$&$<$1.35&5\\
NGC~6041A&c&--&--&$\leq$0.9&$\leq$21.92&21.5&22.84&100&1.45&5\\ %300
NGC~6047&n.d.&--&--&8.3&22.42&1960&24.80&$<$7&0.28&12\\
UGC~10187&n.d.&--&--&$<$2&$<$21.81&111.7&23.56&--&$<$0.41&5\\
NGC~6086&n.d.&--&--&$<$1&$<$21.37&201.35&23.68&--&$<$0.12&5\\
NGC~6173&1s&$\geq$1.4&$\geq$0.07&3.7&21.89&12.97&22.44&40&2.40&5\\
3C~338&2s&2.2&0.16&480&24.01&18.12~$\times$~10$^{3}$&25.59&30&3.47&10\\ %19
3C~465&1s&$\geq$20&$\geq$0.54&246&23.74&10.38~$\times$~10$^{3}$&25.37&100&2.57&8\\ %68
NGC~7768&1s&$\geq$1.1&$\geq$0.02&0.74&21.08&2.6&21.62&100&1.17&5\\ %97
\noalign{\smallskip}
B2 0836+29II&1s&$\geq$20&$\geq$0.54&131&24.31&1139&25.24&100&11.20&13\\
Hydra A&2s&1.2&0.04&168&24.08&132~$\times$~10$^{3}$&26.98&100&0.58&14\\
4C 26.42&2s&1.4&0.07&53&23.71&3153&25.48&80&2.04&15\\
3C 317&2s&1.5&0.08&310&23.93&132~$\times$~10$^{3}$&26.56&100&0.72&16\\
B2151+174&2s&4&0.27&164&25.40&538&25.92&100&53&17\\
PKS 2322-123&2s&1.2&0.04&59.3&24.0&7.2~$\times$~10$^{3}$&26.11&80&1.66&18\\
PKS 1246-410&1s&$\geq$9&0.34&64.4&22.27&2463&23.86&30&0.76&19\\
\hline
\end{tabular}
\tablefoot{$S_{\rm t, 408}$: 1)~From NVSS with $\alpha\sim0.5$, 2)~from \citet{pa91} with $\alpha\sim0.5$; 3)~from \citet{pe90} where $\alpha\sim0.5$, 4)~from \citet{bo93}, 5)~from \citet{fe85},  6)~from \citet{ow97} with $\alpha\sim0.5$, 7)~from \citet{va79} where $\alpha\sim0.6$, 8)~from \citet{fe94},  9)~from \citet{gio01} and NED information with $\alpha\sim 0.5$, 10)~from \citet{fe87} with $\alpha\sim 0.5$, 11)~from \citet{ow97}, 12)~from \citet{tay02} and NED information,  13)~from \citet{ve95},  14)~from \citet{tay90, tay96}, 15)~from \citet{liu09}, 16)~from \citet{ve04}, 17)~from \citet{au06} and from NED with $\alpha\sim 0.5$ (408~MHz) and~$\alpha\sim 0$ (5~GHz), 18)~from \citet{tay99} and NED information and~19)~from \citet{tas06} assuming $\alpha=0.5$. $S_{\rm c}$ is for the arcsecond core flux density at 5~GHz and $S_{\rm VLBI}$ is a correlated flux density at 5~GHz in our VLBI data.\\
We give the name of the BCG (Col.~1), the parsec-scale  morphology (Col.~2: core~(c), one sided (1~s) or two sided (2~s) jet structure), the jet/counterjet surface brightness ratio (Col.~3), $\beta$cos$\theta$ (Col.~4), the arcsecond core flux density $S_{\rm c, 5}$ at~5~Ghz (Col.~5), the arcsecond core power Log~$P_{\rm c, 5 }$ at~5~GHz (Col.~6), the total arcsecond flux density $S_{\rm t, 408}$ (Col.~7) and the total arcsecond power Log~$P_{\rm t, 408 }$ (Col.~8) at 408 MHz, the total VLBI flux density and arcsecond core flux density ratio $S_{\rm VLBI}$/$S_{\rm c, 5}$ at 5~GHz (Col.~9), the core dominance (see Sect.~5.2) (Col.~10). The last column is for the notes.  }
\vspace*{4mm}
\end{table}