Table 1.
Sample clusters, their parameters, and average maximum Li abundance.
| Cluster | Age | RGC | [Fe/H] | A(Li)max | N stars | Teff range |
|---|---|---|---|---|---|---|
| (Gyr) | (kpc) | used | (K) | |||
| NGC 6530 | 0.002 | 6.76 | −0.041 ± 0.009 | 3.38 ± 0.06 | 8 | 4490–5300 |
| Trumpler 14 | 0.002 | 7.62 | −0.03 ± 0.016 | 3.45 ± 0.07 | 62 | 4200–5150 |
| Chamaeleon I | 0.002 | 8.0 | −0.07 ± 0.017 | 3.25 ± 0.11 | 23 | 3475–4310 |
| ρ Oph | 0.003 | 8.0 | −0.08 ± 0.006 | 3.34 ± 0.14 | 13 | 3390–4630 |
| NGC 2264 | 0.003 | 8.71 | −0.06 ± 0.04 | 3.31 ± 0.07 | 12 | 4032–5154 |
| IC 4665 | 0.028 | 7.65 | 0.00 ± 0.02 | 3.32 ± 0.16 | 12 | 5240–6250 |
| IC 2602 | 0.03 | 7.95 | −0.02 ± 0.10 | 3.29 ± 0.18 | 10 | 5290–6705 |
| NGC 2547 | 0.035 | 8.04 | −0.006 ± 0.009 | 3.27 ± 0.14 | 21 | 5615–6930 |
| NGC 6067 | 0.10 | 6.81 | 0.20 ± 0.08 | 3.41 ± 0.13 | 4 | 6630–7370 |
| NGC 2516 | 0.11 | 7.98 | −0.06 ± 0.05 | 3.20 ± 0.07 | 5 | 6580–6950 |
| NGC 6259 | 0.21 | 7.03 | 0.21 ± 0.04 | 3.40 ± 0.06 | 4 | 6600–7050 |
| NGC 6705 | 0.30 | 6.33 | 0.16 ± 0.04 | 3.43 ± 0.12 | 10 | 7050–7470 |
| Berkeley 81 | 1 | 5.49 | 0.22 ± 0.07 | 3.45 ± 0.15 | 11 | 6490–7480 |
| NGC 6802 | 1.00 | 6.96 | 0.10 ± 0.02 | 3.36 ± 0.14 | 5 | 6760–7230 |
| Ruprecht 134 | 1.00 | 4.60 | 0.26 ± 0.06 | 3.42 ± 0.10 | 11 | 6500–6990 |
| Trumpler 20 | 1.4 | 6.86 | 0.15 ± 0.07 | 3.38 ± 0.13 | 4 | 7025–7170 |
| NGC 2420 | 2.20 | 10.76 | −0.13 ± 0.04 | 3.05 ± 0.07 | 21 | 6290–6550 (upper TO) |
| NGC 2243 | 4.9 | 10.4 | −0.38 ± 0.04 | 2.96 ± 0.06 | 5 | 5890–6190 (upper TO) |
Notes. Ages and metallicities were taken from Spina et al. (2017), Magrini et al. (2017), Randich et al. (2018), Casali et al. (2019). The error bars represent the standard deviation of the stars that contribute to the calculation of the mean. The actual error in the mean is a factor of 
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