\begin{table}%t1
   \caption{\label{tab1}Observational results.}
%\centerline
 {
  \small  \begin{tabular}{lll}
       \hline\hline
       \noalign{\smallskip} & $V$~Cam	&  $R$~Leo \\
       \hline\noalign{\smallskip}
       Phase of optical lightcurve$^{(1)}$ & 0.08 & 0.10 \\
       Oscillation period of circular polarization$^{(2)}$
                  & $(5.4\pm 0.1)$~h & $(6.3 \pm 0.3)$~h \\
       False-alarm probability$^{(3)}$ & 4\% & 16\%  \\
       Radial velocity of maser spots$^{(4)}$ 
                  & 7.5~km~s$^{-1}$ & 4.4~km~s$^{-1}$ \\
       Mean circular polarization
                  & $-0.3\%$ & $+2.0\%$ \\
       Mean magnetic flux density in maser$^{(5)}$
                  & $\sim$100~mG & $\sim$1~G \\
 Peak-to-peak variation of fractional polarization 
 & $2.8\% = 5.6~\sigma_{\rm rms}$
 & $3.7\% = 7.4~\sigma_{\rm rms}$  \\
Fluctuation of magnetic field$^{(5)}$& $\sim$1~G & $\sim$1~G \\
\hline
\end{tabular}}
\medskip
 $^{(1)}$  With respect to the maximum of the optical lightcurve; $^{(2)}$ for V~Cam the second harmonic of the modelled rotation period; $^{(3)}$~with respect to the null hypothesis (data are Gaussian noise); $^{(4)}$~with respect to the local standard of rest; $^{(5)}$ order-of-magnitude estimate based on the Zeeman hypothesis, and for a linewidth of 1~km~s$^{-1}$. This corresponds to
a maser at $3~r_{\rm J}$ and a planetary magnetic dipole field eight times stronger than Jupiter's (Wiesemeyer \cite{Wiesemeyer2008}).  
\end{table}