All Tables

Table 1: WMAP+SBBN primordial abundances predicted when $\eta = (6.14 \pm 0.25) \times 10^{-10}$ (or $\Omega _{\rm b} h^2 = 0.0224 \pm$ 0.0009; Spergel et al. 2003) is adopted.
Table 2: Literature sources.
Table 3: The data sample and its main characteristics, as found in the literature. The whole table is available on-line.
Table 4: Photometry and reddening excesses. The whole table is available on-line.
Table 5: Final temperatures as derived from different reddening corrections. The whole table is available on-line.
Table 6: Final Li abundances as derived by using different sets of ${T}_{\rm eff}$ . The whole table is available on-line.
Table 7: Discrepant cases in the original works of R96, R99, and BM97. Columns identified by a $\Delta$ symbol represent the difference on that given quantity ( ${T}_{\rm eff}$ , [Fe/H], EW, and lithium abundance) between R96 and BM97 (when a target has a second entry, this refers to R99 - BM97).
Table 8: Quantities extracted from the HIPPARCOS catalogue for our sample stars ((B-V) and E(B-V) are given in Table 4). The whole table is available on-line.
Table 9: Characteristics and evolutionary status of the sample stars. The whole table is available on-line.
Table 10: Distribution of the evolutionary status in our different sub-classes. The last line indicates the status that we could attribute to the stars which were first labelled as "unsure'' (see the text for more details).
Table 11: Number of dwarfs in each subsample.
Table 12: Average value of A(Li) $_{\rm NLTE}$ , average and standard deviation, and rms for the dwarf stars : mean $^{\pm {\rm aver}}_{\pm {\rm stand}}$ (rms). We separate the clean and the complete sample and give the results for 2 limits in effective temperature.
Table 13: Straight average value of A(Li) $_{\rm NLTE}$ , average and standard deviation for the turnoff and subgiant stars: mean $^{\pm {\rm aver}}_{\pm {\rm stand}}$ (rms). We separate the clean and the complete samples and present the results for 2 limits in effective temperature.
Table 14: Average value of A(Li) $_{\rm NLTE}$ and average deviation for [Fe/H] $\leq$ -1.5: When all the stars are considered regardless of their possible duplicity or variability (Col. a), when all the suspected and confirmed binaries are omitted (Col. b), and when only the confirmed binaries are excluded (Col. c). In cases (b) and (c) the stars reported as variable in SIMBAD are not considered. The first and second lines contain the values for the clean and the complete samples respectively.
Table 15: Sample stars with Li upper limits. The stars with a * lie in the ranges in effective temperature and metallicity chosen to delimitate the Li plateau. The others are either cooler or more metal-rich. The $\char93$ indicates the stars for which a v sin i value higher than 4.5 km s^-1 could be derived by Ryan et al. (2002) or Ryan & Elliott (2004). See the text for more details.
Table 16: Sample stars with published ⁶Li detection. The data are from Smith et al. (1998, sln98), Cayrel et al. (1999a, c99) and Nissen et al. (2000, n00). Columns 2 and 3 give the ${T}_{\rm eff}$ (2) and [Fe/H] values that we attributed to the stars while Cols. 4 and 5 display the values quoted in the original papers. For completeness, we note that a re-analysis by Asplund et al. (2005) of HIP 8572 and HIP 96115 from very high resolution and S/N UVES (Dekker et al. 1999) spectra finds a slightly less than 2 $\sigma$ detection for HIP 8572 and no ⁶Li detection for HIP 96115.
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Table 3: The data sample and its main characteristics, as found in the literature.
Table 4: Photometry and reddening excesses.
Table 5: Final temperatures as derived from different reddening corrections.
Table 6: Final Li abundances as derived by using different sets of ${T}_{\rm eff}$ .
Table 8: Quantities extracted from the HIPPARCOS catalogue for our sample stars ((B-V) and E(B-V) are given in Table 4).
Table 9: Characteristics and evolutionary status of the sample stars.