\begin{table}%t4
%\centering
\par
\caption{\label{tab:outer_radii}Adopted disk outer radii.}  
\small 
\begin{tabular}{lcccc}
\hline \hline\noalign{\smallskip}
Object & $R_{\rm{out}}${$\!\!\!\!$\tablefootmark{a}} (K02) & $R_{\rm{out}}${$\!\!\!\!$\tablefootmark{a}} (AW07) & $R_{\rm{g}}${$\!$\tablefootmark{b}} (I09) & Adopted $R_{\rm{out}}$-interval \\
& (AU) & (AU) & (AU) & (AU)\\
\hline\noalign{\smallskip}
AA Tau  & $\rm 214^{+63}_{-51}$ & $\rm 400^{+600}_{-75}$ & ...    & $200{-}400$      \\
CI Tau  & ...      & $225\pm 50$        & ...    & $150{-}250$     \\
CW Tau  & ...      & ...       & ...    & $100{-}300$  \\
CX Tau  & ...      & ...       & ...    & $100{-}300$  \\
CY Tau  & $211\pm 28$       & ...       & $230$  & $230{-}330$                \\
DE Tau  & ...      & ...       & ...    & $100{-}300$  \\
DL Tau  & $\rm 152^{+28}_{-27}$ & $\rm 175^{+50}_{-25}$  & ...    & $150{-}250$        \\
DM Tau  & $220\pm 47$       & $\rm 150^{+250}_{-100}$ & $160$          & $160{-}260$ \\
DN Tau  & $147\pm 469$      & $\rm 100^{+300}_{-25}$ & $125$  & $125{-}225$      \\
DO Tau  & $98\pm 52$ & ...       & ...    & $100{-}200$ \\
DR Tau  & $193\pm 141$      & $\rm 100^{+175}_{-25}$ & $90$ & $90{-}190$          \\
DS Tau  & ...      & ...       & ...    & $100{-}300$ \\
FM Tau  & ...      & ...       & ...    & $100{-}300$ \\
FZ Tau  & ...      & ...       & ...    & $100{-}300$ \\
GM Aur  & $\rm 151^{+63}_{-29}$ & $150\pm 25$ & $270$ & $270{-}370$ \\
GO Tau  & ...      & $\rm 350^{+650}_{-175}$ & $160$ & $160{-}260$\\
HO Tau  & ...      & ...       & ...    & $100{-}300$  \\
IQ Tau  & $\rm 329^{+403}_{-70}$ & ...      & ...    & $250{-}400$ \\
RY Tau  & $81\pm 128$       & $150\pm 25$        & $115$ & $115{-}215$\\
SU Aur  & ...      & ...       & ...    & $100{-}300$ \\
UZ Tau E  & ...    & ...       & $160$           & $160{-}260$\\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a} {$R_{\rm{out}}$ listed here results from image fitting using a truncated power-law for the surface density profile. K02: Kitamura et~al. (\cite{Kit02}); AW07: Andrews \& Williams (\cite{And07}).}
\tablefoottext{b} {$R_{\rm{g}}$ is the radius within which the 95\% of the flux is observed, after fitting the visibility of the source with a Gaussian; we used this value, when available, as a lower limit for our adopted $R_{\rm{out}}$-interval. I09: Isella et~al. (\cite{Ise09}).}}
\end{table}