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\begin{document}
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%\title{The B3-VLA CSS sample}
%\subtitle{V. VLBA images at 6 and 3.6 cm}

%\author{M. Orienti\inst{1,2} \and
%D. Dallacasa\inst{1,2} \and
%C. Fanti\inst{2,3} \and
%R. Fanti\inst{2,3} \and
%S. Tinti\inst{4}
% \and C. Stanghellini\inst{5}  
% }


%%%%%%%%%%%%%%%%%% Table 1
\begin{table*}
\small{
\begin{center}
\begin{tabular}{lcclccccrr}
\hline
\hline
Source&Id&$m_{R}$&~~~$z$&$S_{4.9}^{VLA}$&$S_{5.0}^{VLBA}$&$S_{8.4}^{VLA}$&$S_{8.4}^{VLBA}$&LAS&LLS\\
 & & & &mJy&mJy&mJy&mJy&mas&kpc $h^{-1}$\\
~~~~~(1)&(2)&(3)&~~(4)&(5)&(6)&(7)&(8)&(9)&(10)\\
\hline
&&&&&&&&&\\
0039+373&g& &1.006&261.0&232.6&120.3&--&120&0.50\\
0147+400&E& & &293.2&231.8&195.8&175.8&80&$\sim$0.33\\
0703+468&E& & &630.7&574.3&400.1&346.7&70&$\sim$0.28\\
0822+394&g& &1.180&338.9&309.3&191.9&144.2&60&0.26\\
0840+424A&E& & &576.7&506.9&379.2&331.9&120&$\sim$0.53\\
1008+423&E& & &236.2&205.6&153.0&--&80&$\sim$0.35\\
1049+384&g&20.9&1.018&200.6&177.6&104.9&--&200&0.90\\
1133+432&E& & &499.1&464.7&286.3&242.4&35&$\sim$0.15\\
1136+383&E& & &177.5&160.5&117.0&--&55&$\sim$0.25\\
1159+395&g&23.4&2.370&252.0&225.9&165.9&--&60&0.25\\
1242+410&Q&19.7&0.811&663.1&565.2&473.9&407.3&45&0.17\\
1343+386&Q&17.5&1.844&380.3&348.8&278.2&209.1&110&0.50\\
1432+428B&E& & &386.3&326.2&251.1&198.7&40&$\sim$0.20\\
1441+409&E& & &347.6&294.6&212.5&--&120&$\sim$0.50\\
2304+377&G&19.7&0.40 $R$&569.6&481.0&324.9&--&120&0.40\\
2330+402&E& & &328.6&259.4&190.6&164.7&100&$\sim$0.36\\
2348+450&G& &0.978&233.4&206.2&123.3&--&310&1.30\\
2358+406&E& & &577.0&521.9&365.0&321.4&100&$\sim$0.37\\
&&&&&&&&&\\
\hline
\end{tabular} 
\end{center} } 
\caption{The VLBA sample. Column 1: source name (B1950);
Column 2: optical identification (Id) from Paper I; G = galaxy on
the {\it POSS}
prints, g = galaxy fainter than the {\it POSS} limit, Q = quasar, E =
unknown optical counterpart (Vigotti et al. \cite{vigotti});
Column 3: {\it R} magnitude;
Column 4: redshift; ``{\it R}'' indicates a photometric redshift from
{\it R} (from {\it POSS} prints) magnitude (see Paper I for details);
Column 5: VLA 4.9 GHz flux density, from Paper I;
Column 6: total VLBA 5.0 GHz flux density, measured on the
images presented here;
Column 7, 8: as for column 5, 6 but at 8.4 GHz;
Column 9: VLBA Largest Angular Size, measured on the
most suitable images at the different resolution and frequency, 
presented here;
Column 10: Largest Linear Size from VLBA data;
for E sources $z$ = 1.00 was assumed and LLS is given with a leading
``$\sim$''.}
\label{Table 1}
\end{table*} 
%%%%%%%%%%%%%% End of Table 1

%%%%%%%%%%%%%% Table 2 
\begin{table*}
\begin{center}
\begin{tabular}{clrrrrrrr}
\hline
\hline
Source& &$S_{5.0}$&$S_{8.4}$&$\alpha_{1.67}^{5.0}$&$\alpha_{5.0}^{8.4}$&$\theta_{1}$&$\theta_{2}$&p.a.\\
 & &mJy&mJy& & &mas&mas&deg \\
(1)&(2)&(3)~~&(4)~~&(5)~&(6)~&(7)&(8)&(9) \\
\hline
&&&&&&&&\\
0039+373&N$\sim$&124.0& &1.04& &19&12&80 \\
 &S$\sim$&108.6& &1.17& &24&11&30 \\
0147+400&E&157.1&121.6&0.26&0.49&2.4&2.2&126 \\
 &C&14.5&18.5& &--0.47&1.5&0.3&176 \\
 &W$\sim$&76.6&23.6&1.05&2.27&11&6&120 \\
0703+468&E&218.2&131.7&0.82&0.97&4.3&2.4&57 \\
 &W&353.8&212.8&0.76&0.98&4.9&2.9&51 \\
0822+394&E$\sim$&238.2&120.0&0.97&1.32&33&12&60 \\
 &W$\sim$&67.0&25.4&1.20&1.87&26&10&75 \\
0840+424&N&409.8&252.4&0.78&0.93&6.9&2.9&176 \\
 &C&30.7&31.2& &--0.03&5.0&2.6&161 \\
 &S$\sim$&67.8&35.6&1.02&1.24&26&14&160 \\
1008+423&E$_{1}\sim$&9.2& &$<$1.40& &12&7&120 \\
 &E$_{2}\sim$&13.6& & & &22&8&120 \\
 &Ce$\sim$&5.4& &0.86& &14&5&75 \\
 &W$\sim$&175.4& &0.75& &27&18&40 \\
1049+384&W$_{1}\sim$&74.6& &1.08& &17&13&140 \\
 &W$_{2}\sim$&83.8& &0.82& &19&10&130 \\
 &E$_{1}\sim$&15.1& &0.30& &10&6&115 \\
 &E$_{2}\sim$&4.2& &1.66& &6&5&0  \\
1133+432&N&307.2&160.1&0.87&1.26&2.1&2.0&43 \\
 &S&151.7&78.2&1.01&1.28&3.5&2.1&20 \\
1136+383& N$\sim$ &112.0 &    & 0.64 & & 20&  8&170 \\
        & C$\sim$ & 10.8 &    & 0.69 & & 10&  5&170 \\
        & S$\sim$ & 42.0 &    & 0.99 & & 10& 10& 0 \\
1159+395&N$\sim$&153.0& &0.70& &32&12&145 \\
 &S$\sim$&71.7& &0.76& &13&12&0 \\
1242+410&N$\sim$&127.5&73.7&0.45&1.06&10&9&20 \\
 &C&39.0&46.0& &--0.32&2.6&0.5&20 \\
 &J$\sim$&193.5&128.0& &0.80&12&4&20 \\
 &S$\sim$&188.9&136.8&$<$0.61&0.62&15&9&20 \\
1343+386&C&73.9&50.3&0.14&0.74&4.9&2.0&0 \\
 &S&238.1&134.4&0.86&1.10&4.4&3.3&56 \\
1432+428&E&296.7&191.4&0.63&0.85&4.5&2.7&97 \\
 &W$\sim$&29.6&8.3&1.15&2.45&19&12&95 \\
1441+409&E$\sim$&43.3& &1.06& &16&9&65 \\
 &C&29.9& &0.31& &2.1&1.2&63 \\
 &Ce$\sim$&54.0& &0.87& &14&9&60 \\
 &W$\sim$&177.9& &0.83& &11&9&65 \\
2304+377&W$\sim$&403.1& &0.83& &40&11&100 \\
 &E$_{1}\sim$&43.2& &0.20& &7&7&0 \\
 &E$_{2}\sim$&22.4& &0.55& &9&6&70 \\
 &E$_{3}\sim$&12.4& &2.10& &11&9&90 \\
2330+402&W&214.9&147.6&0.40&0.73&1.3&1.1&66 \\
 &Ce$\sim$&20.0&10.6&1.03&1.22&6&4&110 \\
 &E$\sim$&8.7&5.7&2.23&0.81&8&7&115 \\
 &E$^{*}$&15.0&4.9& & & & & \\
2348+450&N$\sim$&62.4& &0.79& &24&10&150 \\
 &S$\sim$&143.7& &0.86& &98&16&150 \\
2358+406&N$_{1}\sim$&29.8&15.1&1.06&1.31&7&4&150 \\
 &N$_{2}\sim$&54.9&26.8&1.23&1.38&15&8&110 \\
 &C&21.4&23.6&&--0.19&4.0&1.4&149 \\
 &S$\sim$&359.2&224.1&0.58&0.91&14&9&150 \\
 &S$^{*}$&21.0&10.0& & & & & \\
&&&&&&&&\\
\hline
\end{tabular} 
\end{center}   
\caption{Observational parameters of source components. 
Columns 1 and 2: Source name { (B1950)} and sub-component label; ``$\sim$''
indicates that the component is extended: its flux density is
measured using TVSTAT and the angular sizes of major and minor axis
are measured on the image contour plot (see text);
Columns 3 and 4: VLBA flux density at 5.0 and 8.4 GHz respectively;
Columns 5 and 6: spectral indices $\alpha_{1.67}^{5.0}$ and
$\alpha_{5.0}^{8.4}$ obtained from the data of Paper II and those
presented here;
Columns 7, 8 and 9: deconvolved angular sizes of major and minor axis of
the best-fitting Gaussian component and position angle of the major
axis as estimated
on the most suitable images at the different resolution and frequency, 
using JMFIT.}
\label{Table 2}
\end{table*}  
%%%%%%%%%%%%%% End of Table 2

\end{document}
