\begin{table}%t2
\caption{Determined atmospheric parameters for \corots, the Sun, and \acenb.}\label{tab:vwa}
\par
%%\centerline

{\small
\begin{tabular}{lcclclllccc}
\hline
\hline
       & \multicolumn{4}{c}{$\langle$\feonetwo$\rangle$}     & $\langle$Mg~1b$\rangle$  &  $\langle$Ca6122$\rangle$  & $\langle$Ca6162$\rangle$  & $\langle$Ca6439$\rangle$    & \multicolumn{2}{c}{$\langle$Isol.\ lines$\rangle$}  \\ % [\kms]}  \\
Spec.  & \teff\ [K]  & \logg & \multicolumn{1}{c}{\feh} &  \vmicro\ [\kms] & \multicolumn{1}{c}{\logg}  & \multicolumn{1}{c}{\logg}  & \multicolumn{1}{c}{\logg}   & \multicolumn{1}{c}{\logg}    & \vsini & \vmacro  \\ %  & [\kms] & [\kms]     \\ \hline
\hline
 H1      & $   5180\pm67$ & $ 4.30\pm0.08$  & $+0.11\pm0.13$ & $ 0.98\pm0.07$ & $3.89\pm0.46 $ &$4.44\pm0.08$ & $4.43\pm0.10 $ &$4.34\pm0.19 $ &  1.3   & 1.2  \\ % HARPS, spec1
 H1~\sme& $   5280\pm44$ & $ 4.44\pm0.06$  & $+0.13\pm0.06$ & $ 0.80\pm0.07$ & $4.62        $ &$4.66       $ & $4.53        $ &               &        &      \\ % HARPS, spec1 - SME analysis
 H2      & $   5300\pm41$ & $ 4.46\pm0.08$  & $+0.14\pm0.13$ & $ 0.80\pm0.09$ & $4.02\pm0.47 $ &$4.43\pm0.05$ & $4.56\pm0.06 $ &$4.13\pm0.35 $ &  1.1   & 1.2  \\ % HARPS, spec2
 H3      & $   5350\pm31$ & $ 4.57\pm0.06$  & $+0.15\pm0.09$ & $ 0.76\pm0.07$ & $4.14\pm0.44 $ &$4.50\pm0.09$ & $4.77\pm0.07 $ &$4.72\pm0.26 $ &  1.1   & 1.2  \\ \hline % HARPS,spec3
 H1-7    & $   5280\pm35$ & $ 4.48\pm0.06$  & $+0.13\pm0.09$ & $ 0.80\pm0.05$ & $3.94\pm0.52 $ &$4.47\pm0.06$ & $4.60\pm0.08 $ &$4.32\pm0.27 $ &  0.9   & 1.4  \\ % HARPS, spec1-7=comb.
 H1-107  & $   5300\pm25$ & $ 4.54\pm0.05$  & $+0.13\pm0.08$ & $ 0.77\pm0.05$ & $3.91\pm0.55 $ &$4.51\pm0.06$ & $4.58\pm0.05 $ &$4.45\pm0.18 $ &        &      \\ % HARPS = 107 spe.
 H1-107~\sme&$5290\pm44$ & $ 4.49\pm0.06$  & $+0.13\pm0.06$ & $ 0.80\pm0.05$ & $4.43        $ &$4.49       $ & $4.49        $ &               &        &      \\ % HARPS = 107 spe. -- SME analysis
 U1      & $  5300\pm17$ & $ 4.50\pm0.03$ & $+0.11\pm0.06$ & $ 0.70\pm0.08$ & $3.94\pm0.49 $ &$4.42\pm0.05$ & $4.46\pm0.06 $ &$4.41\pm0.19 $ &  $ $   & $ $     \\  \hline % UVES spec 
 Ceres   & $  5767\pm17$ & $ 4.44\pm0.03$ & $-0.01\pm0.03$ & $ 1.01\pm0.03$ & $4.50\pm0.08 $ &$4.46\pm0.20$ & $4.43\pm0.10 $ &$4.43\pm0.42$  &  1.4   & 2.1  \\ %  Solar
 Ganymede& $  5757\pm17$ & $ 4.43\pm0.04$ & $-0.00\pm0.04$ & $ 0.93\pm0.03$ & $4.51\pm0.10 $ &$4.33\pm0.17$ & $4.38\pm0.08 $ &$4.47\pm0.37$  &  1.1   & 2.3  \\ %  Solar
 Moon    & $  5775\pm25$ & $ 4.48\pm0.03$ & $+0.02\pm0.04$ & $ 0.91\pm0.04$ & $4.41\pm0.08 $ &$4.53\pm0.20$ & $4.41\pm0.14 $ &$4.50\pm0.33$  &  2.1   & 2.2  \\ %  Solar
\hline
 \acenb  & $  5185\pm25$ & $ 4.50\pm0.03$ & $+0.31\pm0.05$ & $ 0.83\pm0.04$ & $4.01\pm0.50 $ &$4.53\pm0.07$ & $4.51\pm0.05 $ &$4.65\pm0.16$  &  1.0   & 0.8  \\ %  Alpha Cen B
\hline
\end{tabular}}
\tablefoot{Results are from \vwa\ except H1 and H1-107, which are also
given for the \sme\ analysis. The 1-$\sigma$ uncertainties are internal errors.}
%% We find $T_{\rm eff}=5185\pm25$~K, $\log g = 4.50\pm0.03$, ${\rm [Fe/H] = +0.31 \pm 0.05$
\par
% Results from \sme\ is given for the H1-107 spectrum.
% The method is indicated in angled brackets. 
% The 1-$\sigma$ uncertainties stated here are internal errors. 
% The \vsini\ and \vmacro\ are determined from isolated spectral lines; 
% the $1$-$\sigma$ uncertainty range for each parameter is $(+1.0, -0.5)$ ~\kms.
\end{table}