\begin{table}%t5
\caption{\label{fotel}The (circular) orbital solutions based on the 1031-d period.}
%%\centerline

{\small
\begin{tabular}{rcccccl}
\hline\hline\noalign{\smallskip}
Element           &  Solution 1: \ha emis. & Solution 2: \he \\
\noalign{\smallskip}\hline\noalign{\smallskip}
$P$ (d)           &1031.55 ~\p~ 0.71  & 1031.55 fixed \\
$T_{\rm RV~max}$&51759.2 ~\p ~1.4   & 51749.5~ \p ~4.5\\
$K$ (\ks)         &21.593 ~\p~ 0.071  & 20.81~ \p ~0.60 \\
$\gamma$ (\ks)    &  $^*)$          & $-12.36$ ~\p ~0.41\\
$f(m)$ (\ms)      &1.076            & 0.9634             \\
rms (\ks)         &0.944            & 7.42          \\
No. of RVs        & 437             & 430           \\
\hline
\end{tabular}}
\tablefoot{For
the \ha emission line RVs, the data were divided into five segments, covering
individual orbital periods, and treated formally as coming from different
spectrographs with different systemic RVs. Thus, we were able to
remove the slight long-term variations affecting the RVs. No such
procedure was applied to the \he RVs.  All epochs are in HJD-2~400~000;
rms is the rms of the \oc\ values.\\
$^*)$ Local $\gamma$'s ranged from $-5.8$ to $-11.6$~\ks,
all with rms errors below 1~\ks.}
\end{table}