\begin{table}%t1
\caption{The barium syndrome among YSyS. The spectral type of the
cool component is taken from \citet{Muerset-99}, or references therein.
In column labelled "nebula'', "y''~means that an optical nebula has been 
detected, and~"PN'' that, based on its emission line spectrum, the star has traditionally been
included in planetary nebulae catalogues, even though no optical nebula may be visible. The column labelled "$P$''~lists the orbital period, from \citet{Muerset-99}.}\label{Tab:yellow}
%\centerline
{
\begin{tabular}{lllrrcllll}
\hline
\hline
 Name          & Sp. typ. & [Fe/H]   & \multicolumn{1}{c}{$V_r$}    &
\multicolumn{1}{c}{$b$}   & [Ba/Fe] &
$V \sin \; i$ & Nebula & $P$  & Ref. \\
               &          &          & \multicolumn{1}{c}{(km~s$^{-1}$)}   
                                         & \multicolumn{1}{c}{($^\circ$)}
&& \multicolumn{1}{c}{(km~s$^{-1}$)} & & (d) &\\
\hline
\multicolumn{10}{c}{d'-type}\\
\hline
V417 Cen & G8-K2 & $\sim$$0.0$ & & $-1$ & 0.5 &  70 & y &  247 & (5, 11)\\
HDE 330036& G5 & 0.02 & $-14$ & $+4$ & 0.88 & 100 & PN & -- & (14, 17)\\
\multicolumn{1}{r}{=Cn 1--1}\\ 
AS 201  & G5 & 0.07 & & $+7$ & 0.63 &  25 & y & -- & (12, 17)\\
V471/V741 Per & G5 &  ? &$-$12 & $-$9 & $>$$0$ & &PN & -- &(2)\\ 
\multicolumn{1}{r}{=M 1--2}\\ 
St H$_\alpha$ 190 & G5 & 0.0 & $\sim$$10$ & $-$35 & $\sim$$0.5$ & 100 &
bip. outf.& -- & (10, 13)\\ 
Wray 157 & G5 & ? \\ 
Hen 1591 & $<$K4 & ?\\
\hline
\multicolumn{10}{c}{s-type}\\
\hline
UKS Ce-1 & C4, 5Jch & ? & +20 & +20 & $>$$0$ &&&  -- & (6)\\
S 32  & C1, 1CH & ? & +325 & $-$30 &  $>$$0$ &  & & 612 & (6, 14)\\
Hen 2-467 & K0  & $-$1.1 & $-$109 & $-$12 &  +0.8  &&n & 478 & (4, 16)\\ 
BD$-21^\circ$3873 & K2 & $-$1.1 & +204 & +37 & +0.5 & & n &282 & (3, 15, 16) \\
           &     & $-$1.3   &          &        & +0.3 & &&&(9)\\  
AG Dra & K2 & $-$1.3 & $-$148 & +41 & +0.5 & & n &554 & (8, 16)\\
CD $-43^\circ$14304 & K7 & $-$1.4 & +27 & $-41$ & ?  &  &&1448 & (7, 18)\\
\hline
\noalign{\smallskip}
\multicolumn{10}{c}{Chemical evolution of the Galaxy}\\
   & & $-$1.0  & & &   $<$$0.2$ &&&  & (1) \\
\hline
\end{tabular}}
\medskip
References: (1) Edvardsson et~al. 1993, A\&A, 275, 101; (2) \citealt{Grauer-Bond-81}, PASP,
93, 630; (3) Pereira et~al. 1997, AJ, 114, 2128; (4)~\citealt{Pereira-98}, AJ, 116,
1977; (5) Pereira et~al. 2003, in Symbiotic stars probing stellar evolution,
ed.~R.~L.~M. Corradi, J. Miko\l ajewska, \& T.~J. Mahoney, Astron. Soc. Pacific Conf. Ser. (San~Francisco), 85; (6) Schmid 1994, A\&A, 284, 156; (7) Schmid et~al. 1998, A\&A, 329, 986; (8) \citealt{Smith-96}, A\&A, 315, 179; (9) \citealt{Smith-97}, A\&A, 324, 97; (10) Smith et~al. 2001, ApJ, 556, L55; (11) Van~Winckel et~al. 1994, A\&A, 285, 241;  (12) \citealt{Schwarz-91}, A\&A, 243, 469; (13) Munari et~al. 2001, A\&A, 369, L1; (14) \citealt{Schmid-Nussbaumer-93}, A\&A, 268, 159; (15) Munari \& Patat 1993, A\&A, 277, 195; (16) \citealt{Corradi-99}, A\&A, 343, 841; (17) Pereira et~al. 2005, A\&A, 429, 993; (18)~The metallicity is from Pereira, priv. comm.
\end{table}