\begin{table}%t3
%\centering
\par
\caption{\label{largedat}Andromeda mass estimated at large galactocentric radii.}
\begin{tabular}{lcccc}
\hline \hline
\noalign{\smallskip}
     Reference &  $R$ &  Mass  & $V_{\rm c}$  &  Objects \\
              &  [kpc] & [10$^{10}$~$M_\odot$] & km~s$^{-1}$ & \\
\hline 
\citet{2000MNRAS.316..929E} & 32 & $\rm 39^{+2}_{-10}$ &  $\rm 230^{+5}_{-32}$ & 17 Globular 
Clusters\tablefootmark{a} \\
This paper                  & 37 & $\rm 49^{+12}_{-14}$ & $\rm 240^{+38}_{-38}$ & 21-cm data \\
\citet{2000MNRAS.316..929E} & 41 & $\rm 48^{+34}_{-23}$ & $\rm 225^{+69}_{-63}$  & 17 Globular 
Clusters\tablefootmark{b} \\
\citet{2008ApJ...674..886L} & 55 & $\rm 55^{+4}_{-3}$   & $\rm 208^{+7}_{-6}$	 & 504 Globular Clusters \\
Galleti et al. (2006) & 60 & $\rm 44^{+26}_{-4}$  & $\rm 178^{+48}_{-8}$  & 349 Globular Clusters\tablefootmark{c} \\
\citet{2000ApJ...537L..91C} & 100 & $\rm 79^{+5}_{-5}$ & $\rm 185^{+6}_{-6}$ & 12 
Satellites\tablefootmark{d} \\
\citet{2004MNRAS.351..117I} & 125 & $\rm 75^{+25}_{-13}$  & $\rm 161^{+25}_{-15}$  & Stellar Stream \\
\citet{2006MNRAS.366.1012F} & 125 & $\rm 74^{+12}_{-12}$  & $\rm 160^{+13}_{-14}$  & Stellar Stream \\
\citet{1999AJ....118..337C} & 268 & $\rm 137^{+18}_{-18}$ & $\rm 149^{+9}_{-10}$   & 7 Satellites \\
\citet{2000MNRAS.316..929E} & 560 & $\rm 125^{+180}_{-60}$& $\rm  98^{+55}_{-27}$  & 11 
Satellites\tablefootmark{e}
 \\
\citet{2000ApJ...540L...9E} & 560 & $\rm 99^{+146}_{-63}$  & $\rm 87^{+51}_{-34}$  & 16 
Satellites\tablefootmark{f}
 \\
\hline 
\end{tabular}
\tablefoot {
\tablefoottext{a}{Best mass estimate using GCs; the lower mass extreme is the value inferred using 9 PNe, 
the upper mass extreme is from data on 11 Satellites.}
\tablefoottext{b} {Uncertanties derived from ``Error analysis'' section of original paper.}
\tablefoottext{c} {Uncertanties include uncertanties on the isotropy degree of the velocity 
distribution and the mass estimate using only the 14 most distant GCs.}
\tablefoottext{d} {Mass estimate assuming isotropic orbits; the mass range is larger, 
79$^{+174}_{-46}$, if models with only radial or circular orbits are included.}
\tablefoottext{e} {Uncertanties derived from ``Error analysis'' section of original paper.}
\tablefoottext{f} {Mass estimate assuming Osipkov-Merrit distribution function; the given mass range
includes also the mass estimated assuming a constant orbital anisotropy.}
}
\par
\end{table}