\begin{table}%t7
%\renewcommand{\arraystretch}{0.5}
\caption{Results of the lightcurve+spectroscopy solution for all objects in our sample. $R,r,M,m$: radii and masses of the primary and secondary. $i$: orbital inclination. The last column summarizes the nature of the system, with a number referring to the section where each case is treated. Question marks and brackets denote cases where the resolution is only tentative,  colons (":") the values with high uncertainties.}
%\centerline
{   
\begin{tabular}{l l l l l l l l  } \hline\hline
Name & $R$ & $r$  & $M$ & $m$ & $i$ & Nature & Section\\  
 &[$\Rsol$] & [$\Rsol$]&[$\Msol$]& [$\Msol$]& [$^\circ$] & & \\ \hline 
OGLE-TR-63      & (1.6)& (0.15) & & & & M eclipsing  binary? &[\ref{ssb1_3}]\\
OGLE-TR-64 &	      1.29$\pm$0.11& 0.97: &1.37$\pm$0.02& 0.87 $\pm$0.01 &83 & grazing eclipsing binary &[\ref{ssb2_1}]\\
OGLE-TR-65 &   1.58$\pm$0.07&1.59$\pm$0.05 &1.15$\pm$0.03&1.11$\pm$0.03 &70 & triple system & [\ref{ssb2_3}]\\
OGLE-TR-68	& & & & & & eclipsing binary?	&[\ref{snoccf}]\\
OGLE-TR-69 &  1.44 $\pm$ 0.10 & 1.06 $\pm$ 0.20 &   &   & 82 & grazing eclipsing binary &[\ref{ssb2_5}]\\
OGLE-TR-72  	    &1.49$\pm$ 0.12	    &0.31:   &             &0.26:   &86-87     & M eclipsing binary   &[\ref{ssb1_1}] \\
OGLE-TR-76 &   1.2$\pm$0.2 & & & 0.64: &$>$77 & triple system  &[\ref{ssb2_2}]\\
OGLE-TR-78  	    &1.51$\pm$0.05&0.24 $\pm$0.013 &             &0.243$\pm$0.015 &$>$85 & M eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-81    & (1.4)& & & & & triple system? &[\ref{ssb2_5}]\\
OGLE-TR-82	& & & & & & unsolved	&[\ref{snoccf}]	\\
OGLE-TR-84	& & & & & & eclipsing binary?	&[\ref{snoccf}]	\\
OGLE-TR-85 &   1.30$\pm$0.13  & &  & 0.39: &$>$77 & triple system &[\ref{ssb2_2}]\\
OGLE-TR-89	& & & & & & false transit detection?	&[\ref{snoccf}]	\\
OGLE-TR-93 &   (2.0):& &   & &  & triple system? &[\ref{ssb2_5}]\\
OGLE-TR-94       &  (1.7)& ($>$0.2) & & & & M eclipsing binary? &[\ref{ssb1_3}]\\
OGLE-TR-95    & (1.8)& & & & & multiple system &[\ref{ssb2_2}]\\
OGLE-TR-96 &   (1.4)&(1.2) &  &   &84 & grazing eclipsing binary &[\ref{ssb2_5}]\\
OGLE-TR-97    & & & & & & multiple system &[\ref{ssb2_5}]\\
OGLE-TR-98       & (2.2)& (0.34)& & & & M eclipsing binary? &[\ref{ssb1_3}]\\
OGLE-TR-99       & (1.1)& (0.19)& & & & M eclipsing binary? &[\ref{ssb1_3}]\\
OGLE-TR-105 	    &2.06$\pm$0.30 &  &             &1.05: &82 & G eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-106 	    &1.31$\pm$0.09 &0.181$\pm$0.013 &             &0.116$\pm$0.021 &$>$85 & M eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-107	& & & & & & eclipsing binary ?	&[\ref{snoccf}]	\\
OGLE-TR-109	& & & & & & unsolved &[\ref{snovar}]\\
OGLE-TR-110&   (1.32)&(1.28) &  & &84 & grazing eclipsing binary &[\ref{ssb2_5}]\\
OGLE-TR-111     & $\rm 0.88^{+0.10}_{-0.03}$  & $\rm 0.103^{+0.013}_{-0.06}$& $\rm 0.82^{+0.15}_{-0.02}$&  0.00050$\pm$0.00010& & planet &[\ref{planets}]\\
OGLE-TR-112 &  3.5::&  & &0.4:: & $>$70  & quadruple system &[\ref{ssb2_4}]\\
OGLE-TR-113       & 0.765$\pm$0.025&  0.111$\pm$0.006&  0.77$\pm$0.06 & 0.00130$\pm$0.00020 & & planet &[\ref{planets}]\\
OGLE-TR-114 &  0.73$\pm$0.09&0.72$\pm$0.09 &0.82$\pm$0.08&0.82$\pm$0.08 &83 & triple system  &[\ref{ssb2_3}]\\ 	
OGLE-TR-118	& & & & & & false transit detection?		&[\ref{snoccf}]\\
OGLE-TR-120 	    &1.62$\pm$0.07 &0.42$\pm$0.02 &             &0.47$\pm$0.04 &$>$88 & M eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-121 	    &1.33$\pm$0.15 &0.33: &             &0.35: &85 (fixed) & M eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-122 	    &$\rm 1.05^{+0.20}_{-0.09}$&$\rm 0.120^{+0.024}_{-0.013}$ &             &0.092$\pm$0.009 &$>$88 & M eclipsing binary &[\ref{ssb1_1}]\\
OGLE-TR-123	& & (0.1) & &(0.07) & & M eclipsing binary? &[\ref{ssb1_2}]\\
OGLE-TR-124	& & & & & & false transit detection? &[\ref{snovar}]\\
OGLE-TR-125 	    &1.94$\pm$0.18 &0.211$\pm$0.027 &             &0.209$\pm$0.033 &$>$86 &M eclipsing binary  &[\ref{ssb1_1}]\\
OGLE-TR-126      & (1.8)& (0.25)& & & & M eclipsing binary? &[\ref{ssb1_3}]\\
OGLE-TR-127	& & & & & & false transit detection?	&[\ref{snoccf}]	\\
OGLE-TR-129	& & & & & & M eclipsing binary? &[\ref{ssb1_2}]\\
OGLE-TR-130 	    &1.13$\pm$0.04 &0.25: &             &0.39: &85 (fixed)  &M eclipsing binary &[\ref{ssb1_1}] \\
OGLE-TR-131	& & & & & & false transit detection? &[\ref{snovar}]\\     
OGLE-TR-132       & 1.43$\pm$0.10 & 0.116$\pm$0.008  &  1.35$\pm$0.06&  0.00113$\pm$0.00012& & planet &[\ref{planets}]\\\hline
\end{tabular}}   \medskip
%
%
%
%
{\bf Individual notes:}
{\em OGLE-TR-64}:
 the period is twice the OGLE estimate. With the new period, the even transits are clearly shallower than the odd transits (0.030 and 0.018~mag respectively), reflecting the luminosity difference between the two components.
%
%
%\item[OGLE-TR-81]
%
%The single spectrum shows two components, with \vsini=21 and $<5$ km/s. The first value is compatible with synchronised rotation with $R\sim 1.4$ $\Rsol$.  The second would indicate $R<0.5 \Rsol$, and therefore indicates that the second component is not synchronised. The transit shape is V-shaped, indicating a probable high impact parameter. This information is compatible with a triple system scenario, where the first component is eclipsed by an unseen companion, and the third component contaminates the spectra and dilutes the light. 
%
%
%
{\em  OGLE-TR-85}:
the spectra consist of a broad component superimposed on an even broader component. We assumed that the wide-lined system had a constant radial velocity, which yields a much better orbital solution for the other component than allowing it to vary. The parameters of the second component somewhat depend on the choice of fixed parameters for the first.
%
{\em OGLE-TR-89}:
%
the CCF shows the possible presence of a second, very wide component, but the signal-to-noise ratio is not high enough to measure it with confidence.
%
{\em OGLE-TR-93}:
%
%Only one measurement was obtained for this object, showing two components in the CCF. The rotation velocities are \vsini=45~\kms and $<$5~\kms respectively. If synchronised with the period of $P=2.2$ days, the first value would indicate $R_A\sim 1.96 \Rsol$. The second would indicate an unrelated third body. The surface ratio of the two CCF components is 2.21/0.92 (\kms), indicating that if the two objects have similar temperatures, the first contributes $\sim 2/3$ of the light. 
%Fitting the photometric transit curve with this constraint yields $r\sim 0.34 \Msol$ for the unseen eclipsing companion.  The light curve of this object shows a sinusoidal modulation with half the period of the transit \citep{Sir03}, with an amplitude compatible with the presence of an eclisping companion with $m\sim 0.34 \Msol$. While this tentative scenario explains all available data, other configurations cannot be eliminated entirely.
The transit depth and ellipsoidal modulation amplitude \citep{Sir03} are compatible with a $r\sim m \sim 0.34 \Msol$ transiting companion. 
%
%\item[OGLE-TR-97]
%
%One spectrum indicating a clear triple-lined system. The projected rotation velocity of the three components are 10.7~\kms, 9.4~\kms and $\sim$4~\kms\ respectively. None of these values are compatible with synchronisation, even with double the period ($P_{OGLE}$=0.57 days).  Clearly, one spectrum is not sufficient to solve this case.
%
{\em OGLE-TR-99}: there is a slight indication of a second dip in the CCF, but the depth and width of this possible dip are not compatible with a simple explanation of the transit in terms of an eclipsing binary. We therefore prefer the explanation in terms of a single dip, that gives a coherent solution.
%
%
{\em OGLE-TR-105}:
%
both the eclipse and anti-eclipse are visible in the lightcurve. Tthe orbital period is twice the OGLE estimate. The eclipse depth ratio and the derived radii are compatible with a solar-type G dwarf eclipsing an evolved late-F star, with both stars on the same isochrone.
%
{\em OGLE-TR-112}:
%
two sets of lines are superimposed on the very wide and shallow lines of the star undergoing the transit (see Fig.~\ref{ccf}). The flux ratios and the difference between the two systemic velocities are compatible with a gravitationally bound quadruple system consisting of two close binary systems, one of them eclipsing. 
%
{\em OGLE-TR-114}:
%
the velocity of the third component shows a slight drift over the measurement period ($\dot{V_r}=43\pm$12 m/s), which may indicate that it is gravitationally bound to the other two on a wider orbit. The surface of the three CCF dips are similar, which would be compatible with such a case. The orbit of OGLE-TR-114ab shows large velocity residuals around a circular orbit, that do not correspond to a Keplerian eccentric orbit. 
%
{\em OGLE-TR-118}:
%
the CCF in the two measured spectra is compatible with a very broad dip, with \vsini~$\sim$~40~\kms. This would imply $R\sim 1.4$~$\Rsol$ assuming tidal synchronisation, but the radial velocity change would then be of the order of 5~\kms, which would be too small for an orbital solution with a massive companion. This is the faintest star in our sample, and the signal-to-noise ratio of the spectra is not high enough to have confidence in the presence of a signal in the CCF. 
\label{param}
\label{tsummary}
\end{table}