Table 10: Spectroscopic $T_{\rm eff}$ and Li abundances1 derived for the subgroup of Li detected (left) and Li non-detected stars (right).
Li detected            Li non-detected
  $T_{\rm eff}$ log $\varepsilon $(Li)     $T_{\rm eff}$ log $\varepsilon $(Li)
IRAS name K 12 + log N(Li)   IRAS name K  12 + log N(Li)

01085+3022		 3300 2.4   03507+11152 $\dots$ $\dots$
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   13442-61094 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
18025-21132 $\dots$ $\dots$   17034-1024 3300 <+0.0
18057-26163 3000 $\dots$   17359-2138** $\dots$ $\dots$
18413+1354 3300 1.8   18050-2213 2900 <-1.0
18429-1721 3000 1.2   18304-07282 $\dots$ $\dots$
19129+2803 3300 3.1*   18454-12264 3300 <+0.0
19361-16585 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+08464 3000 <-1.0
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 Å is very low to derive any reliable $T_{\rm eff}$ and/or Li abundance estimate.

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