\begin{table}%t2
\caption{\label{res}Main results obtained from the analysis of the optical spectra of the 17~AGNs of the present  sample of {\it Swift} sources.}
%\centerline
 {\tiny \begin{tabular}{lcccccrccl}
\hline \hline
\multicolumn{1}{c}{Object} & $F_{\rm H_\alpha}$ & $F_{\rm H_\beta}$ &
$F_{\rm [OIII]}$ & Class & $z$ & \multicolumn{1}{c}{$D_L$} & \multicolumn{2}{c}{$E(B-V)$}&\multicolumn{1}{c}{ $L_{\rm Radio}$}\\
\cline{8-9}
& & & & & & (Mpc) & Gal. & AGN&\multicolumn{1}{c}{(erg~s$^{-1}$)}\\
\hline
Swift J0059.4+3150 & * & 87 $\pm$ 5& 37 $\pm$ 2 & Sy1.2 & 0.015 & 84.2 & 0.061& -- &\multicolumn{1}{c}{--}\\
& * & [105 $\pm$ 6] & [45 $\pm$ 3] & & & & & & \\
& & & & & & & & &\\
& & & & & & & & &\\
Swift J0134.1$-$3625 & 9.4 $\pm$ 0.3 & in abs.& 5.3 $\pm$ 2.2 & Sy2 & 0.029 & 136.7 & 0.020 &--& \multicolumn{1}{c}{--}\\
& [9.9 $\pm$ 0.4] & [in abs.] & [5.6 $\pm$ 2.3] & & & & & &\\
& & & & & & & & &\\
Swift J0342.0$-$2115 & * & 2000 $\pm$ 400 & 400 $\pm$ 80& Sy1 & 0.0139 & 67.6 & 0.032 &--& \multicolumn{1}{c}{--} \\
& * & [2700 $\pm$ 600] & [460 $\pm$ 90] & & & & & &\\
& & & & & & & & &\\
Swift J0350.1$-$5019 & 38 $\pm$ 3 & 6.9 $\pm$ 0.9 & 11 $\pm$ 1 & Sy2 & 0.035 & 165.8 & 0.015 & 0.216&\multicolumn{1}{c}{--}  \\
& [39 $\pm$ 3] & [7.2 $\pm$ 0.9] & [11 $\pm$ 1] & & & & & &\\
& & & & & & & & & \\
Swift J0505.7$-$2348 & 38 $\pm$ 1 & 9 $\pm$ 1 & 48 $\pm$ 1 & Sy2 & 0.036 & 172.1 & 0.040 & 0.144 & $3.1 \times 10^{38}$ (1.4~GHz)  \\
& [41 $\pm$ 1] & [10 $\pm$ 1] & [55 $\pm$ 1] & & & & & & \\
& & & & & & & & &\\
Swift J0501.9$-$3239 & 180 $\pm$ 20 & 52 $\pm$ 11 & 320 $\pm$ 30 & Sy2 & 0.0126 & 58.9 & 0.017 & 0.036 & 7.0 $\times$ 10$^{37}$ (843~MHz)\\
& [190$\pm$20] & [59 $\pm$ 13] & [350  $\pm$  30] & & & & & &\\
& & & & & & & & &\\
Swift J0640.1$-$4328 & 3.1 $\pm$ 0.5 & 0.7 $\pm$ 0.3 &2.3 $\pm$ 0.4 & Sy2& 0.061 & 293.9 & 0.084 & -- & 8.1 $\times$ 10$^{39}$ (843~MHz)\\
&[4.1 $\pm$ 0.7] & [3.6 $\pm$ 1.7] & [3.0 $\pm$ 0.6] & & & & & &\\
& & & & & & & & &\\
Swift J0727.5$-$2406 & *  & 2.1 $\pm$ 0.7 & 21 $\pm$ 1 & Sy1.9& 0.123& 619.0 & 1.047&--& $1.9 \times 10^{40}$ (1.4~GHz)  \\
& * & [47 $\pm$ 7] & [385 $\pm$ 17] & & & & & &\\
& & & & & & & & &\\
Swift J0739.6$-$3144 & 36 $\pm$ 2 & 2.3 $\pm$ 0.5 & 32 $\pm$ 1 & Sy2 & 0.026 & 122.3 & 0.613 & 0.360 & 2.5 $\times$ 10$^{38}$ (1.4~GHz)\\
& 142 $\pm$ 7 & [18 $\pm$ 4] & [216 $\pm$ 5] & & & & & & $6.4 \times 10^{38}$ (843~MHz)\\
& & & & & & & & &\\
Swift J0743.0$-$2543 & * & 11 $\pm$ 2 & 4.5 $\pm$ 0.7 & Sy1.2  & 0.023 & 108.0 & 0.678 & -- & $1.2 \times 10^{37}$ (1.4~GHz) \\
& *& [146 $\pm$ 20] & [38 $\pm$ 6] & & & & & &\\
& & & & & & & &  &\\
Swift J0811.5+0937 & -- & in abs. &--& XBONG & 0.286 & 1582.6 & 0.026& --&$ 1.8 \times 10 ^{40}$ (1.4~GHz)\\
& & [in abs.] & & & & & & &\\
& & & & & & & & &\\
Swift J0902.0+6007  & *& $52 \pm 5$ & $98 \pm 5$ & Sy2  & 0.012 & 56.2 & 0.043 &0.198& $1.6 \times 10^{38}$ (1.4~GHz)  \\
& *& [58 $\pm$ 6] & [114 $\pm$ 6] & & & & & &\\
& & & & & & & & &\\
Swift J0904.3+5538& *& 30.9 $\pm$ 7.9 &23.1  $\pm$ 0.8 & Sy1.5  & 0.0374 & 177.4 & 0.021& -- &\multicolumn{1}{c}{--} \\
& *& [36.1 $\pm$ 9.9] & [24.5 $\pm$ 0.9] & & & & & &\\
& & & & & & & & &\\
Swift J0911.2+4533 & 4.2 $\pm$ 0.2 & $<$0.3& 4.4 $\pm$ 0.2 & Sy2 & 0.0269 & 127.1 & 0.019 & $>$0.360& $8.4 \times 10^{37}$ (1.4~GHz) \\
& [4.4 $\pm$ 0.2] & [$<$ 0.2] & [4.4 $\pm$ 0.3] & & & & & &\\
& & & & & & & & &\\
Swift J0917.2$-$6221  & *& 1450 $\pm$ 40 & 270 $\pm$ 3 & Sy1.2  & 0.057 & 274.3 & 0.182 & -- & $4.7 \times 10^{39}$ (843~MHz)  \\
& * & [2380 $\pm$ 60] & [518 $\pm$ 6] & & & & & &\\
& & & & & & & & &\\
& & & & & & & &  &\\
Swift J0923.7+2255 & *& 127 $\pm$ 13 & 92 $\pm$ 4 & NLSy1  & 0.034 & 160.9 & 0.043&--& $4.5 \times 10^{38}$ (1.4~GHz)  \\
& *& [140 $\pm$ 14] & [105 $\pm$ 5] & & & & & &\\
& & & & & & & & &\\
Swift J1049.4+2258 & 26 $\pm$ 1& 4.4 $\pm$ 0.4 & 87 $\pm$ 1 & Sy2  & 0.033 & 156.0 & 0.029 & 0.261 & \multicolumn{1}{c}{--}\\
& [29 $\pm$ 1]& [4.7 $\pm$ 0.5]& [$93 \pm 1$] & & & & & &\\
& & & & & & & & &\\
\hline
\end{tabular}}
\medskip
Note: emission line fluxes are reported both as observed and (between square brackets) corrected for the intervening Galactic absorption $E(B-V)_{\rm Gal}$ along the object line of sight (from Schlegel et~al. \cite{Schlegel1998}). Line fluxes are in units of 10$^{-15}$~erg~cm$^{-2}$~s$^{-1}$. The typical error on the redshift measurement is  $\pm$0.001  but for the SDSS and 6dFGS spectra, for which an uncertainty of  $\pm$0.0003 can be assumed; $^*$:~heavily blended with [N {\sc ii}] lines.
\end{table}