\begin{table}%T4
\caption{\label{starplanet_param_table}Planet and star parameters.}     
\small
%\centering
\par
\begin{tabular}{l l}        
\hline\hline                 \noalign{\smallskip}
\multicolumn{2}{l}{\emph{Ephemeris}} \\
\hline
Planet orbital period $P$ [days] & 13.2406 $\pm$ 0.0002 \\
Planetary transit epoch $T_{ \rm tr}$ [HJD-2~400~000] & 54~273.3436 $\pm$ 0.0012 \\
Planetary transit duration $d_{\rm tr}$ [h] & 2.98 $\pm$ 0.06 \\
Planetary occultation epoch $T_{\rm occ}$\tablefootmark{a} [HJD-2~400~000] & 54~276.49 $\pm$ 0.41 \\
Planetary occultation duration $d_{\rm occ}$ [h] & 2.08 $\pm$ 0.18 \\
Epoch of periastron $T_{0}$ [HJD-2~400~000] & 54~990.85 $\pm$ 0.08 \\
\noalign{\smallskip}
\multicolumn{2}{l}{\emph{Derived parameters from radial velocity observations}} \\
%\hline    
Orbital eccentricity $e$  &  0.53 $\pm$ 0.04 \\
Argument of periastron $\omega$ [deg] & 218.9 $\pm$ 6.4 \\ 
Radial velocity semi-amplitude $K$ [\ms] & 301 $\pm$ 10 \\
Systemic velocity  $V_{\rm r}$ [\kms] & 15.330 $\pm$ 0.007 \\
O$-$C residuals [\ms] & 29 \\
\noalign{\smallskip}
\multicolumn{2}{l}{\emph{Fitted and fixed transit parameters}} \\
%\hline
$\theta_{2}$\tablefootmark{b} & 0.00483 $\pm$ 0.00009 \\
Radius ratio $k=R_{\rm p}/R_{*}$ & 0.1269 $\pm$ 0.0038 \\
Inclination $i$ [deg] & 88.55 $\pm$ 0.2 \\
$u_{+}$ (fixed) & +0.72 \\
$u_{-}$ (fixed) &  +0.30 \\
\noalign{\smallskip}
\multicolumn{2}{l}{\emph{Derived transit parameters}} \\
%\hline
$a/R_{*}$\tablefootmark{c} & 31.33 $\pm$ 2.15 \\
$a/R_{\rm p}$ & 247 $\pm$ 21 \\
$(M_{*}/\Msun)^{1/3} (R_{*}/\Rsun)^{-1}$ & 1.33 $\pm$ 0.09 \\
Stellar density $\rho_{*}$ [$\rm g\;cm^{-3}$] & 3.32 $\pm$ 0.70\\
Impact parameter $b$\tablefootmark{d} & 0.85 $\pm$ 0.03\\
\noalign{\smallskip}
\multicolumn{2}{l}{\emph{Spectroscopic parameters of the star}} \\
%\hline
Effective temperature $T_{\rm{eff}}$[K] & 5075 $\pm$ 75 \\
Surface gravity log~$g$ [cgs]&  4.65 $\pm$  0.10 \\
Metallicity $[\rm{Fe/H}]$ [dex]& +0.26 $\pm$ 0.07 \\
Stellar rotational velocity $V \sin{i_{*}}$ [\kms] & 2.0 $\pm$ 0.5 \\
Spectral type & K1V \\
\noalign{\smallskip}
\multicolumn{2}{l}{\emph{Stellar and planetary physical parameters}} \\
%\hline
Star mass [\Msun]\tablefootmark{e} &  0.89 $\pm$ 0.05 \\
Star radius [\Rsun]\tablefootmark{e} &  0.79 $\pm$ 0.05  \\
Planet mass $M_{\rm p}$ [\Mjup ]  &  2.75  $\pm$ 0.16 \\
Planet radius $R_{\rm p}$ [\Rjup]  &  0.97 $\pm$ 0.07 \\
Planet density $\rho_{\rm p}$ [$\rm {g\;cm^{-3}}$] &  3.70 $\pm$ 0.83 \\
Planet surface gravity log~$g_{\rm p}$ [cgs] &  3.93 $\pm$  0.08 \\
Planet rotation period $P_{\rm p, rot}$ [days]\tablefootmark{f} &  4.25 $\pm$ 0.53 \\
Distance of the star $d$ [pc] & 345 $\pm$ 70 \\
Orbital semi-major axis $a$ [AU] & 0.1055 $\pm$ 0.0021 \\
Orbital distance at periastron $a_{\rm per}$ [AU] & 0.0496 $\pm$ 0.0039 \\
Orbital distance at apoastron $a_{\rm apo}$ [AU] &  0.1614 $\pm$ 0.0047 \\
Equilibrium temperature at the averaged distance
$T_{\rm eq}$ [K]\tablefootmark{g} & 600 $\pm$ 23 \\
Equilibrium temperature at periastron
$T^{\rm per}_{\rm eq}$ [K]\tablefootmark{g} & 935 $\pm$ 54 \\
Equilibrium temperature at apoastron
$T^{\rm apo}_{\rm eq}$ [K]\tablefootmark{g} & 518
$\pm$ 20 \\
\noalign{\smallskip}
\hline  
\end{tabular}     
\tablefoot{\tablefoottext{a}{$T_{\rm occ}= T_{\rm tr}+\frac{P}{\pi} \cdot \left(\frac{\pi}{2}+(1+\csc^2{i})\cdot e~\cos{\omega}\right)$;}\\
\tablefoottext{b}{phase of the  end of transit egress 
in the reference system defined by \citet{GimenezPelayo83};} \\
\tablefoottext{c}{$a/R_{*}=\frac{1+e \cdot \cos\nu_{2}}{1-e^{2}} 
\cdot \frac{1+k}{\sqrt{1-\cos^{2}({\nu_{2}+\omega-\frac{\pi}{2}})\cdot \sin^{2}{i}}}$, where $\nu_{2}$ is the true anomaly measured from the periastron passage at the  end of transit egress (see \citealt{Gimenez09});}\\
\tablefoottext{d}{$b=\frac{a \cdot \cos{i}}{R_{*}} \cdot \frac{1-e^{2}}{1+e \cdot \sin{\omega}}$;}\\
\tablefoottext{e}{from CESAM stellar evolution models. See Sect.~\ref{stellar_planet_param} for details;}\\
\tablefoottext{f}{assuming the planet to be in a pseudo-synchronous rotation;}\\
\tablefoottext{g}{black body equilibrium temperature for an isotropic 
planetary emission.} }
\vspace*{-0.5mm}
\end{table}