\begin{table}%t1
%\centering
\par
\caption{\label{tab1}Basic properties and resulting $M/L$~ratios for the sample of dSph galaxies.}
\begin{tabular}{@{}llllllll@{}}
\hline   \hline \noalign{\smallskip}
Galaxy & $~~~\sigma~[\rm{km~s^{-1}}]~~~~~~~~$ & $R_{\rm hl}~[\rm{kpc}]~~~~~ $ & $L_{\rm tot}~\times10^{5}~L_{\odot}$
& $(M/L)_{A}~~~~~~~~~~~$ & $(M/L)~~~~~~~~~~~~~$ & $\langle \chi \rangle ~~~~~~~~~~$  &  
Age of Youngest \\
      & & & & & & &  Component [Gyr]\\
 \hline\noalign{\smallskip}
Carina & $7\pm~1.8$   & 0.290 & 4.3   & $\rm 5.6^{+5.2}_{-2.9}$  &  $\rm 6.8^{+8.3}_{-4.6}$   & 7  &  3   \\
& & & & & & \\
Draco      & $8\pm~1.5$   & 0.230 & 2.6   & $\rm 43.9^{+29}_{-19.3}$  &  $\rm 17.0^{+13.9}_{-8.9}$ & 4.1  & 10   \\
& & & & & & \\
LeoI & $8\pm~1.2$   & 0.330 & 48.0  & $\rm 0.7^{0.65}_{-0.3}$   &  $\rm 1.0^{+0.6}_{-0.44}$  & 5.7  & 2     \\
 & & & & & & \\
 Sextans    & $7\pm~1.0$   & 0.630 & 5.0   & $\rm 9.2^{+5.3}_{-3.0}$   &  $\rm 6.3^{+4.2}_{-2.8}$   & 13.4 & (2--6) \\
  & & & & & & \\
 Fornax     & $12\pm~1.3$  & 0.400 & 150.0 & $\rm 1.4^{+0.45}_{-0.35}$&  $\rm 1.4^{+0.6}_{-0.4}$   & $>$3.4   & (2--3)  \\
  & & & & & & \\
 Sculptor   & $9.5\pm~1.7$ & 0.160 & 22.0  & $\rm 3.7^{+2.2}_{-1.4}$  &  $\rm 3.4^{+2.1}_{-0.7}$   & $>$2.2 & $>$5     \\
  & & & & & & \\
 LeoII      & $6\pm 1.4$   & 0.185 & 7.0   & $\rm 1.85^{+2}_{-1.1}$   &  $\rm 2.3^{+2.4}_{-04}$    & 5.5  & 6.5    \\
  & & & & & & \\
 Ursa Minor & $8\pm 2$     & 0.300 & 5.8   & $\rm 5.8^{+6.5}_{-3.6}$   &  $\rm 8.0^{+9.8}_{-5.1}$   & $>$5.3 & 12     \\
\noalign{\smallskip}\hline
\end{tabular}
\tablefoot{$(M/L)_{A}$ gives the values for the mass to light
ratios calculated by Angus (\cite{Angus08}), and $M/L$~those
in this study under the proposed model. Total luminosities (in the $V$
band) and half-light radii are from Wilkinson et~al. (\cite{Wilkinson06}), Wilkinson et~al. (\cite{Wilkinson04}), Koch et~al. (\cite{Koch07a}), Kleyna et~al. (\cite{Kleyna04}), Walker et~al. (\cite{Walker06}), Mateo (\cite{Mateo98}),
Coleman et~al. (\cite{Coleman07}) and Irwin \& Hatzidimitriou (\cite{Irwin95}), for the galaxies in the table, in
the order given, as summarised in Gilmore et~al. (\cite{Gilmore07}). Velocity dispersions are from adjusting a constant value to the data of Angus (\cite{Angus08}). $\langle \chi \rangle$ gives the average value of the parameter $\chi$ as defined in  Sect.~2, which measures the relative relevance of the Newtonian and 
the low acceleration limit of the MOND formalism terms in Eq.~(6). The final column gives an estimate of the age of
the youngest stellar population present in each of the systems,
for Carina, Ursa Minor, LeoI, and LeoII from Hernandez et~al. (\cite{Hernandez00}), for Fornax from Coleman \& de~Jong (\cite{Coleman08}), for Draco from Aparicio et~al. (\cite{Aparicio01}), for
Sextans from Lee et~al. (\cite{Lee03}), and for Sculptor from Babusiaux et~al. (\cite{Babusiaux05}).}
\end{table}