\begin{table}%t3
\par
\vspace*{2mm}
\caption {\label{t:bd}Close companions to solar-type stars with (projected) masses between 10 $M_{\rm J}$ and 80 $M_{\rm J}$.}     
%\centerline
\par
{\scriptsize
\begin{tabular}{c c c c c c c c c c l}        % centered columns (4 columns)
\hline\hline                 % inserts double horizontal lines
Object & $M_{\rm c}\sin i$ & Period & $a$ & $e$ & $i$ & $M_{\rm c}$ & SpT & Mstar & [Fe/H] & Remarks and references \\    % table heading
       & $ M_{\rm J}$  & $d$      & AU&   & deg & $ M_{\rm J}$  & & $M_{\odot}$ & \\
\hline                        % inserts single horizontal line
\multicolumn{11}{c} {Probable substellar objects with mass $M_{\rm c} > 10 M_{\rm J}$ and $a<7$ AU around solar-type stars} \\
\object{HD~29587b}      &  41    & 1474.9   &       &   0.356  &             & $41~(27)$        &  G2V  & 1.00  &  --0.61  &   \cite{halb00}, \cite{bensby2005}\tablefootmark{a}
         \\
\object{HD 38529c}      &  12.7  &  2174.3  & 3.68  &   0.36   & 160         & $37^{+36}_{-19}$ & G4IV  & 1.46  &  +0.45  & \cite{butler06}, \cite{reffert06}, \\
&  & & & & & & & & & \cite{vf}, PL, MULT, HIPG  \\  %UD
                                                                                               % 1.39  &  +0.313  encycl.
\object{HD 89707b}      &  59    & 297.708  &       &   0.952  &             & $64~(19)$        &  G1V  & 1.05  &  --0.42  &  \cite{halb00}, \cite{edvarssson93}\tablefootmark{b}
 \\
\object{HD 127506b}     &  36    &  2599    &       &   0.716  &             & $45~(21)$        &  K3V  & 0.75  &  +0.06  &  \cite{halb00}, \cite{haywood01}  \\
\object{HD 131664b}     &  18.15 &  1951    &  3.17 &   0.638  & $55\pm12$   & $23^{+26}_{-5}$   & G3V   & 1.10  &  +0.32  & this paper, HIPG \\
\object{HD 168443c}     &  18.1  &  1765.8  & 2.91  &   0.2125 & 150         & $34\pm12$        & G5    & 1.08  &  +0.08  & \cite{reffert06}, PL \\ %UD, RIBAS
                                                                                               %  1.06  &  +0.03
              &        &          &       &          &             & $<$82            &       &       &         & \cite{zuck01} \\
\object{CoRoT-3b}      &        &  4.2568  & 0.057 &    0.0   & 85.9        & $21.7\pm1.0$     & F3V   & 1.37  &  --0.02  & \cite{deleuil08}, transit\tablefootmark{c}
 \\
\object{XO-3b}         &        &  3.19152 & 0.0454&   0.26   & 84.20       & $11.79\pm0.59$   & F5V   & 1.21  &  --0.18  & \cite{winn08},  transit\tablefootmark{d}
              \\
\hline
\multicolumn{11}{c} {Objects with projected mass $10 < M_{\rm c} \sin i< 80 $ $M_{\rm J}$ and $a<7$ AU around solar-type stars} \\
\object{HD 4747b}       &  42.3  & 6832.0   & 6.70  &   0.64   &       &           &       & 0.82  & --0.22   &  \cite{nidever02}, \cite{vf} \\  %UD
\object{HD 13507b}      &  52    & 3000     & 4.3   &   0.14   &       &           &  G0   & 1.00  & +0.03   &  \cite{perrier}, \cite{vf}\tablefootmark{e}           \\
\object{HD 16760b}      &  13.13 & 466.47   & 1.084 &   0.084  &       &           &  G5V  & 0.78 & +0.07  & \cite{sato09}, \cite{bouchy09}, MULT  \\
\object{HD 30339b}      &  77.8  & 15.0778  & 0.13  &   0.25   &       &           &  F8   & 1.39 & +0.26  & \cite{nidever02}, \cite{vf} \\  %UD
\object{HD 39091b}      &  10.35 &  2063.818& 3.29  &   0.62   &       &           &  G1IV & 1.10  &  +0.05  &  \cite{butler06},  \cite{vf} \\ %UD
\object{HD 65430b}      &  67.8  & 3138.0   & 4.00  &   0.32   &       &           &       & 0.83  &  --0.12  &  \cite{nidever02}, \cite{vf} \\ %UD
\object{HD 91669b}      &  30.6  &  497.5   & 1.205 &   0.448  &       &           &       & 0.91  &  +0.31  &  \cite{witten09},  \\
\object{HD 98230b}      &  35    &  3.9805  &       &   0.0    &       &           &       & 0.86  &  --0.35  & \cite{fuhrmann08}, MULT\tablefootmark{f} \\
\object{HD~114762b}      &  11.02 &  83.90   & 0.3   &   0.34   &             &                &  F9V  & 0.93  &  -0.65  & \cite{halb00}, MULT\tablefootmark{g}  
\\
\object{HD~136118b}      &  11.9  &  1209    & 2.3   &   0.37   &       &           &  F9V  & 1.25  &  --0.05  &  \cite{butler06}, \cite{vf} \\ %UD
\object{HD~137510}       &  26    &  798.2   & 1.85  &   0.402  & $>$16 & $<$94     &  G0IV & 1.41   & +0.37  &  \cite{endl04}, \cite{vf}  \\ %UD
                                                                               %   & 1.3   & +0.16 endl
\object{HD~156846b}      &  10.45 &  359.51  & 0.99  &   0.8472 &       &           &  G0V  & 1.43  &  +0.22  &  \cite{tamuz08}, MULT   \\  
\object{HD~162020b}      &  13.75 & 8.428198 & 0.072 &   0.277  &       &           &  K2V  & 0.78  &  +0.11  &  \cite{udry02}\tablefootmark{h}           \\
\object{HD~167665b}      &  50.3  & 4385     & 5.47  &   0.337  &       &           &  G0V  & 1.11  & --0.17   & \cite{patel07}, \cite{vf} \\  %UD
\object{HD~174457b}      &  65.8  & 840.800  & 1.90  &   0.23   &       &           &       & 1.07  & --0.18   & \cite{nidever02}, \cite{vf} \\  %UD
                                                                                 % 1.19 nidever
\object{HD~184860b}      &  32.0  &  693     & 1.4   &   0.67   &       &           &  K2V  & 0.77  &  --0.04  & \cite{vogt02}, \cite{vf}, MULT \\ %UD,HIPC (5'')
\object{HD~191760b}      &  38.17 &  505.65  & 1.35  &   0.63   &       &           & G3IV/V & 1.28 & +0.29 &   \cite{jenkins09} \\
\object{HD~202206b}      &  17.4  &  255.87  & 0.83  &   0.435  &       & $<$149    &  G6V  & 1.17  & +0.35  &  \cite{correia05}, \cite{zuck01}, PL \\ %ribas
                                                                                  %  1.15  &  +0.37
\object{HD~283750b}      &   51   &  1.788   &       & 0.002    &       &           &  dK5  & 0.67  & +0.03   & \cite{halb00}, MULT\tablefootmark{i}
             \\
\object{TYC 2534-698-1b}&  39.7  & 103.698  & 0.44  &   0.385  &       &           &  G2V  & 1.00 & --0.25  & \cite{kane09}  \\
\object{HAT-P-13c}      &  15.2  & 428.5    & 1.19  &   0.691  &       &           &  G4V  & 1.22 & +0.43  & \cite{bakos09}, PL  \\
\hline
\multicolumn{11}{c}{Probable stellar companions with projected mass in the substellar range} \\
\object{HD 18445B}       &  45    &  554.6   &       &    0.558 &             & $187~(20)$          &  K2V  & 0.78  &   0.00  & \cite{halb00}, \cite{vf}, MULT\tablefootmark{j}
      \\
               &        &          &       &          & --16.1       & $178\pm20$          &       &       &         & \cite{zuck01} \\
\object{HD~33636B}       &  9.3   &  2128    &       &    0.48  & $4.1\pm0.1$ & $142^{+3.3}_{-1.8}$ &       & 1.02  &  --0.13  & \cite{bean07}\\ %UD
\object{HD~43848B}       &  25    &  2371    & 3.4   &   0.69   &  $55\pm12$  & $120^{+167}_{-43}$  & G0V   & 0.89  &  --0.03  & this paper, HIPG \\
\object{HD~110833B}      &  17    &  271.17  &       &   0.784  &             & $146~(12)$          & K3V   & 0.72  &   0.00  & \cite{halb00}, \cite{mishenina04}\tablefootmark{k}
         \\ %Mishenina+, 2004
               &        &          &       &          & 7.76        & $143\pm12$          &       &       &         & \cite{zuck01} \\
\object{HD~112758B}      &  34    &  103.258 &       &   0.139  &             & $212~(44)$          & K0V   & 0.79  &  --0.56  & \cite{halb00}, \cite{mishenina04} \\ %Mishenina+, 2004
               &        &          &       &          & 10.4        & $213\pm43$          &       &       &         & \cite{zuck01} \\
\object{HD~140913B}      &  43.2  & 147.968  & 0.55  &   0.54   &             &  $177~(73)$         &       & 1.17  & +0.13   & \cite{nidever02}, \cite{halb00}  \\  %UD
                                                                                             %% 0.98
               &        &          &       &          &  16.3       &  $181\pm74$         &       &       &         & \cite{zuck01}, \cite{vf}\tablefootmark{l}
                    \\
\object{HD~164427B}      &  46    &  108.55  &  0.46 &    0.55  & 8.5         & $372^{+106}_{-85}$  &       & 1.18  & +0.13   & \cite{zuck01} \\
               &        &          &       &          &             & $<$190              &       &       &         & \cite{tinney01}  \\
\object{HD~169822B}      &  27.2  &  293.1   &  0.84 &    0.48  & 175         & $320$               &  G5V  & 0.91  & --0.12   & \cite{vogt02}, MULT\tablefootmark{m}
        \\
\object{HD~217580B}      &  68    &  454.66  &       &  0.520   &             & $171~(14)$          &  K4V  & 0.69  &  --0.06  & \cite{halb00}, \cite{gray03}\tablefootmark{n}
                       \\ %
               &        &          &       &          & 25.2        & $172\pm15$          &       &       &         & \cite{zuck01}  \\
\object{BD-04 782B}     &  48    &  716.68  &       &    0.074 &             & $261~(15)$          &  K5V  &  0.67 &  +0.05  & \cite{halb00}, \cite{heiter03}\tablefootmark{o}
     \\ %heiter&luck+, 2003
               &        &          &       &          & 12.77       & $257\pm16$          &       &       &         & \cite{zuck01} \\
\hline                                   %inserts single line
\end{tabular}
}
\par
\smallskip
\tablefoottext{a}  {For spectroscopic binaries with brown dwarf candidates observed by Hipparcos and with an actual
mass estimate derived by~\citet{halb00}, the error distribution of the secondary masses is not Gaussian and not
symmetric. We list here the values of $M_{\rm c}$ and the accompanying one-sided errors as defined by Eq.~(5) in~\citet{halb00}.
The star has both chemical abundances and kinematics of thick disk. }
\tablefoottext{b} {Thick disk population.}
$^c$  {Transiting system.~\citet{triaud09} found a significant misalignment between the planetary orbital axis and
    $^d$  {Transiting system.~\citet{winn09} found a significant misalignment between the planetary orbital axis and
                       the stellar rotation axis ($37.3\pm3.7$~deg).}                  the stellar rotation axis ($37.6^{+10.0}_{-22.3}$~deg).}
\tablefoottext{e} {The orbit in \citet{perrier} is preliminary, with only limited phase coverage.~\citet{perrier} also report no detection with AO.}	   
\tablefoottext{f}  {Assuming synchronous rotation and orbit aligment~\citet{fuhrmann08} derive $i=15$ and $M_{\rm c}=0.14_{-0.05}^{+0.09}~M_{\odot}$
               for the companion. The system is a quadruple with another SB at $a=2.53$~arcsec (21 AU) with $e=0.41$  from \object{HD~98230}.}	   
$^g$  {The possibility that the star is seen nearly pole-on because of its very low projected rotational velocity is widely
           debated in the literature. \cite{halb00} derive a very uncertain astrometric mass $112~M_{\rm J}$ with an error of
           $103~M_{\rm J}$. An additional low-mass companion close to the substellar boundary detected at 130~AU by
           \cite{patience02}. The star is a member of the thick disk population.}	   \tablefoottext{h} {\citet{zuck01} derive an astromeric solution that gives a companion mass of $3.0\pm0.94~M_{\odot}$, not compatible with
           the stellar properties of the primary. Probably a spurious result due to the short orbital period.}
   \tablefoottext{i} {\cite{halb00} derive  an astrometric mass  of $182~M_{\rm J}$ with a large error of $470~M_{\rm J}$.
             \cite{glebocki95} estimate $i=22\pm10$ and then $M=136\pm39~M_{\rm J}$ from the rotation period (synchronous with the orbit) and projected
             rotational velocity, assuming the rotation axis is perpendicular to the orbital plane. However, misalignements can not be ruled out,
             especially considering that the system has a wide WD companion. The system is probably associated with the Hyades \citep{catalan08}.
             Metallicity from \cite{catalan08}.}       
  \tablefoottext{j} {Also resolved with direct imaging by \cite{beuzit04}. Quintuple system (see \cite{bd07} and references therein). } 
  \tablefoottext{k} {Purely astrometric orbital solution in Hipparcos.}   
  \tablefoottext{l} {The significance of the orbital solution in \cite{zuck01} is about 0.92.} 
   \tablefoottext{m} {Triple system, see \cite{bd07}. Flagged as stochastic solution in Hipparcos.} 
   \tablefoottext{n} {Purely astrometric orbital solution in Hipparcos.}  
  \tablefoottext{o} {Flagged as stochastic solution in Hipparcos.}\vspace*{3mm}
           \end{table}