\begin{table}%t4
  \caption{Preliminary orbital solutions, dynamical parallaxes, and system
    masses for {\toric}.}
\label{tab:orbitalelements}
%\centering
\par
\begin{tabular}{rc|c|c}
  \hline\hline
                      & & Orbit \#1  & Orbit \#2\\
  \hline
  $P$ & [yrs]           & 10.98      & 10.85      \\ 
  $T$ &                 & 1996.52    & 1996.64    \\
  $e$ &                 & 0.909      & 0.925      \\
  $a$ & [mas]           & 41.3       & 45.0       \\
  $i$ & [\degr]         & 105.2      & 103.7      \\
  $\Omega$ & [\degr]    & 56.5       & 56.9       \\
  $\omega$ & [\degr]    & 65.7       & 68.2       \\
  \hline
  $\chi^2/\textnormal{dof}$ &     & 1.61       & 1.59  \\
  \hline
  $\pi_{\rm dyn}^{a)}$    & [mas]        & $2.304 \pm 0.066$    & $2.585 \pm 0.074$ \\
  $d_{\rm dyn}^{a)}$      & [pc]         & $434 \pm 12$         & $387 \pm 11$ \\
  $(M_{\rm C1}+M_{\rm C2})^{a)}$   & [$M_{\odot}$] & $47.8 \pm 4.2$       & $44.8 \pm 3.9$ \\
  \hline
\end{tabular}
  $^{a}$ The errors on the dynamical parallaxes and
  corresponding distances were estimated by varying the measured binary flux
  ratio within the observational uncertainties, the assumed spectral types
  for the bolometric correction by one sub-class, the extinction by ${\pm} 0.2$~mag, and by using three different MLRs
  \citep[by][]{bai46,hei78,dem91}.  However, the given errors do not reflect
  the uncertainties on the orbital elements $a$ and $P$.
  Due to the presence of the multiple orbital solutions, it is currently
  not possible to quantify these errors reliably.
\end{table}