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Table 6

Main results for the 42 OCs analysed, indicating, for each cluster, the number of stars from the sample detected in UVES and GIRAFFE; the number of stars with EW(Li) values; the number of stars selected as candidate members (including RV, astrometric and Li members, as well as the final members); and the number of Li-rich giant contaminants.

Clustera UVES GIRAFFE Membership Li-rich G
All stars With Li All stars With Li RV Gaia Li Final outliers
NGC 6530 52 5 1931 1325 470 200 359 343 11
ρ Oph 23 20 288 277 48 29 37 44 2
Trumpler 14 43 11 1859 1045 228 55 165 159 11
Cha I 47 36 660 623 102 54 88 87 6
NGC 2244 8 6 444 385 143 79 123 116 1
NGC 2264 113 70 1740 1539 621 423 507 503 10
λ Ori 116 103 720 675 207 142 163 161 3
Col 197 8 3 401 363 123 86 104 92 7
γ Vel 79 50 1183 1140 234 1
NGC 2232 47 28 1822 1722 750 56 84 68 9
NGC 2547 54 33 423 372 151 0
IC 2391 48 26 386 374 56 27 37 35 6
IC 2602 131 89 1721 1651 309 43 59 55 24
IC 4665 34 30 533 514 233 29 51 33 0
NGC 2451 A/B 90 70 1566 1537 106 10

NGC 6405 21 12 680 486 251 80 53 51 1
Blanco 1 37 31 426 373 142 119 101 98 0
NGC 6067 27 16 753 327 209 126 60 56 0
NGC 6649 6 0 277 62 42 21 4 2 0
NGC 2516 51 32 708 645 460 378 379 376 0
NGC 6709 10 10 720 590 322 71 53 49 10
NGC 6259 16 14 478 264 125 71 39 35 0
NGC 6705 49 31 1017 579 391 313 142 139 0
Berkeley 30 14 13 318 144 78 44 24 24 0
NGC 6281 16 7 304 214 82 38 23 23 1
NGC 3532 67 51 1094 809 518 411 323 384 11
NGC 4815 14 12 204 92 68 50 30 29 0
NGC 6633 57 38 1605 1463 617 35 62 67 9

NGC 2477 11 10 114 0 86 71 9 9 0
Trumpler 23 16 15 165 70 51 41 25 23 0
Berkeley 81 14 14 265 159 69 42 25 24 0
NGC 2355 11 11 197 149 119 129 87 86 0
NGC 6802 13 13 184 69 77 51 36 32 2
NGC 6005 19 19 541 298 174 112 55 49 3
Pismis 18 10 10 134 72 41 24 12 10 0
Melotte 71 9 9 111 0 71 64 4 4 0
Pismis 15 11 11 322 201 91 66 33 31 1
Trumpler 20 29 26 1184 404 451 367 116 104 0
Berkeley 44 7 7 86 73 39 33 31 30 0
NGC 2243 27 27 634 576 469 446 289 289 8
M67 42 36 95 85 109 89 96 96 0

Notes. (a)Regarding the clusters γ Vel, NGC 2547 and NGC 2451 A and B, we directly used the selections obtained by several studies listed in Table 1.

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