\begin{table}%t10
\caption{\label{tab10}Spectroscopic $T_{\rm eff}$ and Li~abundances$^{1}$ derived for the
subgroup of Li~detected (left) and Li~non-detected stars (right).}
\small%\centerline
{
\begin{tabular}{lcccclcc}
\hline\hline
\multicolumn{3}{c}{Li~detected}& ~~~~~~~~~~& 
\multicolumn{3}{c}{Li~non-detected}\\
\hline
&  {$T_{\rm eff}$} &  {log $\varepsilon$(Li)}& &
 & {$T_{\rm eff}$}&  {log $\varepsilon$(Li)}\\
IRAS name&K& 12 $+$ {log $N$(Li)} & &IRAS name &K~&12 $+$ {log $N$(Li)}\\ 
\hline\noalign{\smallskip}
01085$+$3022 & 3300 & 2.4  	    &&03507$+$1115$^{2}$ &$\dots$&$\dots$\\
02095$-$2355 & 3300 & 1.6          &&05098$-$6422 &3000&$<$$-$1.0\\
04404$-$7427$^{**}$ &$\dots$ &$\dots$ &&05151$+$6312 &3000&$<$+0.0\\
05027$-$2158 & 2800 & 1.1            &&07080$-$5948 &3000&$<$+0.5\\
05559$+$3825 & 2900 & 0.6          &&07445$-$2613 &2900&$<$$-$1.0\\
06300$+$6058 & 3000 & 0.7       &&10189$-$3432 &2900&$<$$-$1.0\\
07222$-$2005$^{**}$ &$\dots$ &$\dots$ &&10261$-$5055 &3000&$<$$-$1.0\\
07304$-$2032 & 2700 & 0.9         &&13379$-$5426 &2900&$<$+0.0\\
09429$-$2148 & 3300 & 2.2         &&13442$-$6109$^{4}$ &3000&$<$$-$1.0\\
11081$-$4203 & 3000 & 1.3        &&13475$-$4531 &2900&$<$$-$1.0 \\
11525$-$5057 & 3300&  0.9 &&14086$-$0730$^{**}$&$\dots$&$\dots$\\
12377$-$6102$^{**}$ &$\dots$&$\dots$ &&14086$-$6907$^{**}$ &$\dots$&$\dots$\\
14337$-$6215 & 3300 &2.4$^{*}$   &&14247$+$0454 &2700&$<$+0.5\\
15211$-$4254 & 3300 & 2.3       &&14266$-$4211 &2900&$<$+0.0\\
15255$+$1944 & 2900 & 1.0      &&15193$+$3132 &2800&$<$+0.0\\
15576$-$1212 & 3000 & 1.1 	    &&15586$-$3838 &3000&$<$+0.0\\
16030$-$5156 & 3000 &1.5     &&16037$+$4218 &2900&$<$$-$1.0\\
16260$+$3454 & 3300 & 2.7	    &&16503$+$0529 &2800&$<$$-$1.0\\
18025$-$2113$^{2}$&$\dots$&$\dots$  &&17034$-$1024 &3300&$<$+0.0\\
18057$-$2616$^{3}$ & 3000 &$\dots$ &&17359$-$2138$^{**}$ &$\dots$&$\dots$\\
18413$+$1354 & 3300 &1.8    &&18050$-$2213 &2900&$<$$-$1.0\\
18429$-$1721 & 3000 &1.2     &&18304$-$0728$^{2}$ &$\dots$&$\dots$\\
19129$+$2803 & 3300 &3.1$^{*}$ &&18454$-$1226$^{4}$&3300&$<$+0.0\\
19361$-$1658$^{5}$&3000&1.9/2.0 &&19147$+$5004 &3000&$<$+0.0\\
20052$+$0554 & 3300 &2.6   &&19157$-$1706 &3300&$<$+0.0\\
 & &                                &&19412$+$0337 &3300&$<$+0.0\\    
 & &                   	            &&20343$-$3020 &3000&$<$$-$1.0\\ 
 & &                   		    &&20350$+$3741  &3000&$<$+0.0\\   
 & &                   		    &&22180$+$3225 &3300&$<$+0.0\\    
 & & 			            &&22466$+$6942&3300&$<$+0.0\\
 & & 			            &&22510$+$3614 &3000&$<$$-$1.0&\\
 & & 				    &&23492$+$0846$^{4}$ &3000&$<$$-$1.0\\
\hline
\end{tabular}}
\smallskip
$^{1}$ The uncertainty in the derived Li~abundances is estimated to be 
around $\pm$0.4$-$0.6~dex.\\
$^{2}$ Possible double~lined spectroscopic binary.\\
$^{3}$ The lithium~line has a P cygni-type profile.\\
$^{4}$ Possible non-AGB~star.\\
$^{5}$ Observed Li~abundances in two different runs.\\
$^{*}$ The abundance value must be treated with some caution because the~line is
resolved in two components (circumstellar and stellar) and the abundance
estimate corresponds to the photospheric abundance needed to fit the stellar
component.\\
$^{**}$ The S/N ratio at 6708~\AA~is very low to derive any reliable 
{$T_{\rm eff}$} and/or Li~abundance estimate. 
\end{table}