\begin{table}%t2
\caption{\label{tab:scales2}Characteristics of our type 2 AGN mid-IR spectroscopic sample.}
%\centering
\par
\begin{tabular}{l c c c  c c c  c c c }
\hline\hline \noalign{\smallskip}
Object           & Type\tablefootmark{a}  & $z$      & $D_L$\tablefootmark{b} & \multicolumn{3}{c}{log Luminosities (erg/s)} & \multicolumn{3}{c}{Object scales}  \\
                 &           &        & (Mpc)     & $\Lx$ ($\nh$)\tablefootmark{c} & $\Loiii$\tablefootmark{d} & $\Lm$\tablefootmark{e} & $\rsub$\tablefootmark{f} (pc) & 8~$\micron$ (pc)$^g$ & res. ($\rsub$) \\ 
                 \hline
        NGC~2110 &       S1i & 0.0080 & ~33.2     & 42.60 (22.57) & 40.35 & 43.00         & \textit{0.028} & ~39.2 & \textit{1392} \\
    ESO~428--G14 &        S2 & 0.0063 & ~26.0     & $\ldots$ ($>$24) & 40.62 & 42.73         & \textit{0.020} & ~30.8 & \textit{1509} \\
    MCG--5-23-16 &       S1i & 0.0095 & ~39.5     & 43.24 (22.47) & 40.63 & 43.53         & \textit{0.052} & ~46.6 & \textit{~900} \\
        NGC~4507 &       S1h & 0.0128 & ~53.0     & 43.34 (23.46) & 41.57 & 43.69         & \textit{0.062} & ~62.1 & \textit{1004} \\
    MCG--3-34-64 &       S1h & 0.0176 & ~73.2     & 42.78 (23.69) & 41.45 & 44.14         & \textit{0.104} & ~84.9 & \textit{~814} \\
        NGC~5643 &        S2 & 0.0047 & ~19.2     & $\ldots$ ($>$24) & 40.55 & 42.49         & \textit{0.016} & ~22.9 & \textit{1471} \\
        NGC~5995 &      S1.9 & 0.0257 & 107~~     & 43.52 (21.95) & 42.01 & 44.06         & \textit{0.095} & 122~~ & \textit{1294} \\
         IC~5063 &       S1h & 0.0109 & ~45.3     & 42.87 (23.28) & 41.28 & 43.82         & \textit{0.072} & ~53.2 & \textit{~737} \\
        NGC~7582 &       S1i & 0.0044 & ~18.3     & 42.04 (22.98) & 40.15 & 42.71         & \textit{0.020} & ~21.8 & \textit{1093} \\
        NGC~7674 &       S1h & 0.0277 & 116~~     & 43.72 (24.00) & 41.93 & 44.26         & \textit{0.120} & 132~~ & \textit{1103} \\ 
        \hline
\end{tabular}
\tablefoot {\tablefoottext{a}{AGN types from \citet{Ver06}: S: Seyfert, L: LINER, S1i: optical type~2 with broad Hydrogen lines in the infrared; S1h: type~2 with detected polarized optical broad lines;}
\tablefoottext{b}{luminosity distance based on CMB~reference frame redshifts from NED and $H_0=73$, $\Omega_{\rm m}=0.27$, and $\Omega_{\rm vac}=0.73$;}
\tablefoottext{c}{$\Lx$~= absorption-corrected 2$-$10~keV luminosity from \citet{Dad07}, except IC~5063 \citep{Tue08}, \mbox{MCG--3--34--64} and NGC~4507 \citep{Hon08}, NGC~5995 \citep{Hor08}, and NGC~7674 \citep{Bia05}; logarithmic intrinsic Hydrogen column densities in units of $10^{22}$~cm$^{-2}$ from \citet{Tue08}, except ESO~428--G14 \citep{Del08}, NGC~5643 \citep{Mai98}, and NGC~7674 \citep[][changing-look AGN]{Bia05};}
\tablefoottext{d}{[\ion{O}{iii}] fluxes from \citet{Stt03} (NGC~4507, IC~5063, NGC~7674), \citet{Mel08} (NGC~5643, NGC~7582), \citet{Gu06} (ESO~428--G14, MCG--3--34--64), \citet{Haa07} (NGC~2110), \citet{Win92a} (\mbox{MCG--5--23--16}), and \citet{Tra03} (NGC~5995);}
\tablefoottext{e}{$\Lm\equiv\nuLnu(12~\micron)$; this work;}
\tablefoottext{f}{based on Eq.~(\ref{eq:sLm});}
\tablefoottext{g}{theoretical diffraction limit for a 8.2~m VLT telescope: 0$\farcs$25 at~8~$\micron$, 0$\farcs$31 at 10~$\micron$, 0$\farcs$37 at~12~$\micron$.}}
\end{table}