\begin{table}%t5
\par
\caption{\label{tab:uma_mem_par}Stellar parameters of the 18 Sun-like stars.}
%\centerline
 {\tiny
\begin{tabular}{lrrrrrrrrrrrrrr}
\hline\hline\\[-3mm]
Object&$T_{\rm eff}$&$\log g$&[Fe/H]&[Mg/Fe]&\multicolumn{1}{c}{$\xi_{\rm t}$}&\multicolumn{1}{c}{$\zeta_{\rm RT}$}&\multicolumn{1}{c}{$v\sin i$}&ref.&\multicolumn{1}{c}{$M$}&\multicolumn{1}{c}{$R$}&$B.C._V$&$M_{\rm bol}$&$d_{\rm sp}$&\multicolumn{1}{c}{$\frac{d_{\rm sp}-d_{\rm HIP}}{d_{\rm HIP}}$}\\
&[K]&[cm/s$^2$]&&&[km~s$^{-1}$]&[km~s$^{-1}$]&[km~s$^{-1}$]&&[$M_\odot$]&[$R_\odot$]&&&[pc]&\multicolumn{1}{c}{[\%]}\\
\hline
\multicolumn{15}{l}{\it M01k}\\[1mm]
            HD  11131 &  5796& 4.43&--0.10& 0.00&0.97&3.70&  1.5&  2& 1.00& 1.01&--0.13& 4.73& 23.8&  0.6\\
%\vspace{\tablinesep}
                                         &    70& 0.10&0.07& 0.05&0.20&& 1.0&& 0.05& 0.04&&0.07& 3.3&\\
         HD  24916~A&  4600& 4.60&--0.03&--   &--  & -- &  2.1&  3& 0.70& 0.69&--0.57& 6.48& 15.4& --2.4\\
%\vspace{\tablinesep}
                                         &   100& 0.20&0.15& --  & -- && 2.0&& 0.05& 0.03&&0.09& 3.7&\\
            HD  26923  &  5975& 4.41&--0.06&--0.01&0.99&4.40&  $<$1.0&  2& 1.07& 1.01&--0.11& 4.57& 22.4&  5.5\\
%\vspace{\tablinesep}
                                         &    70& 0.10&0.07& 0.05&0.20&&--  && 0.05& 0.04&&0.07& 3.0&\\
            HD  38393    & 6310& 4.28$^1$&--0.05& 0.01&1.30&5.70&  8.1&  1& 1.23& 1.33&--0.08& 3.74&   --&  --\\
%\vspace{\tablinesep}
                                         &    60& 0.03&0.05& 0.06&0.20&& 1.0&& 0.05& 0.04&&0.05&  --&\\
            HD  41593    &  5278& 4.54& 0.02&--0.01&1.12&1.70&  4.3&  2& 0.89& 0.82&--0.24& 5.57& 15.8&  2.5\\
%\vspace{\tablinesep}
                                         &    80& 0.10&0.07& 0.05&0.20&& 1.0&& 0.05& 0.03&&0.06& 2.2&\\
%            HD  111456    &  6300& 4.32&  --&  --& --&5.70& 41.0&  4&   --&   --&   --&   --&   --&  --\\
            HD  112196    & 6110& 4.39$^1$& 0.01& 0.02&1.31&4.90& 12.0&  1& 1.15& 1.14&--0.09& 4.22&   --&  --\\
%\vspace{\tablinesep}
                                        &    60& 0.06&0.05& 0.05&0.20&& 1.0&& 0.05& 0.08&&0.14&  --&\\
%            HD  134083   &  6480& 4.30&  --&  --&-- &6.40& 45.0&  4&   --&   --&   --&   --&   --&  --\\
            HD  167389   &  5895& 4.37&--0.02&--0.03&0.99&4.00&  3.3&  1& 1.05& 1.01&--0.12& 4.64& 36.8& 10.0\\
%\vspace{\tablinesep}
                                         &    80& 0.15&0.07& 0.05&0.20&& 1.0&& 0.05& 0.04&&0.07& 6.5&\\
            HD  184960   &  6310& 4.22&--0.08&--0.01&1.55&5.70&  8.0&  1& 1.23& 1.43&--0.08& 3.59& 25.6&  0.0\\
%\vspace{\tablinesep}
                                        &    80& 0.10&0.05& 0.05&0.20&& 1.0&& 0.05& 0.05&&0.06& 3.1&\\
\hline
\multicolumn{15}{l}{{\it M01k, K03k, K03f}}\\[1mm]
            HD  59747  &  5094& 4.55&--0.03&--0.01&1.00&0.90&  1.5&  2& 0.83& 0.76&--0.31& 5.90& 20.8&  5.8\\
%\vspace{\tablinesep}
                                         &    90& 0.10&0.07& 0.05&0.20&& 1.0&& 0.05& 0.04&&0.08& 2.9&\\
            HD  109647   &  4980& 4.70& 0.05&--0.07&0.80&0.40&  3.1&  1& 0.83& 0.74&--0.36& 6.05& 24.0& --8.8\\
%\vspace{\tablinesep}
                                          &60& 0.15&0.15& 0.15&0.20&& 1.0&& 0.05& 0.03&&0.08& 4.3&\\
            HD  110463     & 4940& 4.68& 0.00&--0.02&0.86&0.40&  3.1&  1& 0.80& 0.75&--0.38& 6.05& 20.9& --9.8\\
%\vspace{\tablinesep}
                                         &    80& 0.18&0.10& 0.10&0.20&& 1.0&& 0.05& 0.03&&0.07& 4.5&\\
%\vspace{\tablinesep}
            HD  115043   &  5850& 4.36&--0.10& 0.05&1.26&3.90&  7.5&  1& 1.05& 1.03&--0.13& 4.64& 28.3& 9.3\\
%\vspace{\tablinesep}
                                        &    70& 0.13&0.07& 0.05&0.20&& 1.0&& 0.05& 0.04&&0.06& 4.4&\\
\hline
\multicolumn{15}{l}{{\it K03k, K03f}}\\[1mm]
            HD  28495    & 5465& 4.45&--0.05& 0.00&0.93&2.34&  4.5&  1& 0.95& 0.85&--0.19& 5.35& 31.3& 13.8\\
%\vspace{\tablinesep}
                                          &    90& 0.12&0.05& 0.05&0.20&& 1.0&& 0.10& 0.04&&0.08& 4.8&\\
            HD  39587  &  5920& 4.39&--0.07&--0.01&0.95&4.20&  8.7&  2& 1.04& 1.03&--0.12& 4.59&  9.1&  5.3\\
%\vspace{\tablinesep}
                                          & 70& 0.10&0.07& 0.05&0.20&& 0.8&& 0.05& 0.04&&0.05& 1.3&\\
            HD  71974~A$^2$   &  5570& 4.49&--&--&--&2.8&3.2&1 &--&--&--&--& --&--\\
%\vspace{\tablinesep}
                                         &    100& 0.19&--&--&--&&1.0&&--&--&&--&--&\\
            HD  109011   &  5000& 4.60& --0.12&--0.03&$\la$0.52&0.50&  5.0&  1& 0.83& 0.81&--0.34& 5.85& 22.3& --6.0\\
%\vspace{\tablinesep}
                                          &100& 0.20&0.07& 0.07&--&& 1.0&& 0.05& 0.07&&0.17& 5.3&\\
            HD  171746~A & 6100& 4.36$^1$&--0.04& 0.03&1.50&4.80&  8.3&  1& 1.15& 1.18&--0.10& 4.16&   --&  --\\
%\vspace{\tablinesep}
                                          &    80& 0.06&0.06& 0.05&0.20&& 1.0&& 0.05& 0.08&&0.14&  --&\\
            HD  171746~B &  6040& 4.37$^1$& 0.02&--0.04&1.51&4.60&  7.3&  1& 1.10& 1.16&--0.10& 4.24&   --&  --\\
%\vspace{\tablinesep}
                                       &    80& 0.06&0.05& 0.05&0.20&& 1.0&& 0.05& 0.08&&0.14&  --&\\
\hline
\end{tabular}}
\medskip
\par
The stellar parameters of the sample stars which were studied following the methods of \citet{Fuhrmann98}. The stars are grouped according to the samples they form part of (Table~\ref{tab:uma_mem_data}). The following quantities are listed with the second line providing the errors bars: {(2)} effective temperature, {(3)} surface gravity, {(4)} iron abundance, {(5)} magnesium abundance relative to iron, {(6)} microturbulence parameter, {(7)} macroturbulence parameter, {(8)} projected rotational velocity, {(9)} source of the values: 1~= this work, 2~= \citetalias{Fuhrmann04}, 3~= \citet{Koenig06}, {(10)} mass, {(11)} radius, {(12)} bolometric correction based on \citet{AAM95}, {(13)} absolute bolometric magnitude (from {\em Hipparcos} distance), {(14)} spectroscopic distance, and {(15)}~relative offset from {\em Hipparcos} distance.\\
$^1$ Surface gravity derived from {\em Hipparcos} parallax as described in Sect.~\ref{sect:hipparcos}. The comparison of spectroscopic distance with {\em Hipparcos} distance cannot be done.\\
$^2$ The stellar parameters are preliminary because HD~71974 is a spectroscopically unresolved binary (see discussion of individual objects in Sect.~\ref{sect:mult}). Abundances could not be derived.
\end{table}