Table 3
Distribution of SB2 and SB3 candidates among the different observed fields.
| Field/cluster | log age | vr | # stars | # SB2 | # SB3 | SB2/total | SB3/SB2 | |||||||||
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| [yr] | [km s-1] | doe | Confirmed | A | B | C | doe | Confirmed | A | B | C | [%] | [%] | |||
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| Field | 27 786 | 263 | 185 | 82 | 48 | 55 | 24 | 5 | 5 | 0.67 | 3 | |||||
| Bulge | 2633 | 6 | 6 | 1 | 3 | 2 | 0 | 0 | 0.23 | |||||||
| Cha I | 616 | 5 | 2 | 2 | 1 | 0 | 0.49 | |||||||||
| Corot | 1966 | 13 | 7 | 5 | 2 | 0 | 0 | 0.36 | ||||||||
| γ2 Vel | 1116 | 28 | 16 | 2 | 7 | 7 | 2 | 0 | 1.43 | |||||||
| ρ Oph | 278 | 2 | 1 | 1 | 1 | 0 | 0.72 | |||||||||
|
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| IC 2391 | 7.74 | 14.49 ± 0.14 | 398 | 4 | 3 | 2 | 1 | 4 | 0 | 0.75 | ||||||
| IC 2602 | 7.48 | 18.12 ± 0.30 | 1784 | 6 | 3 | 1 | 1 | 1 | 3 | 0 | 0.17 | |||||
| IC 4665 | 7.60 | −15.95 ± 1.13 | 559 | 6 | 5 | 2 | 2 | 1 | 1 | 0 | 0.89 | |||||
| M 67 | 9.60 | 33.8 ± 0.5 | 25 | 4 | 4 | 4 | 0 | 0 | 16.00 | |||||||
| NGC 2243 | 9.60 | 59.5 ± 0.8 | 715 | 38 | 1 | 1 | 14 | 0 | 0.14 | |||||||
| NGC 2264 | 6.48 | 24.69 ± 0.98 | 1565 | 78 | 4 | 2 | 2 | 18 | 0 | 0.26 | ||||||
| NGC 2451 | 7.8 (A) | 22.70 (A) | 1599 | 18 | 11 | 3 | 5 | 3 | 7 | 1 | 1 | 0.69 | 9 | |||
| 8.9 (B) | 14.00 (B) | |||||||||||||||
| NGC 2516 | 8.20 | 23.6 ± 1.0 | 726 | 19 | 8 | 1 | 4 | 3 | 10 | 1 | 1 | 1.10 | 13 | |||
| NGC 2547 | 7.54 | 15.65 ± 1.26 | 367 | 7 | 1 | 1 | 3 | 0 | 0.27 | |||||||
| NGC 3293 | 7.00 | −12.00 ± 4.00 | 517 | 158 | 9 | 1 | 5 | 3 | 55 | 0 | 1.74 | |||||
| NGC 3532 | 8.48 | 4.8 ± 1.4 | 94 | 1 | 1 | 1 | 0 | 0 | 1.06 | |||||||
| NGC 4815 | 8.75 | −29.4 ± 4 | 174 | 11 | 2 | 1 | 1 | 0 | 0 | 1.15 | ||||||
| NGC 6005 | 9.08 | −24.1 ± 1.3 | 531 | 12 | 4 | 2 | 1 | 1 | 8 | 1 | 1 | 0.75 | 25 | |||
| NGC 6530 | 6.30 | −4.21 ± 6.35 | 1252 | 95 | 5 | 2 | 3 | 1 | 0 | 0.40 | ||||||
| NGC 6633 | 8.78 | −28.8 ± 1.5 | 1643 | 17 | 15 | 3 | 7 | 5 | 0 | 0 | 0.91 | |||||
| NGC 6705 | 8.47 | 34.9 ± 1.6 | 994 | 108 | 19 | 5 | 3 | 11 | 52 | 1 | 1 | 1.91 | 5 | |||
| NGC 6752 | 10.13 | −24.5 ± 1.9 | 728 | 8 | 1 | 1 | 0 | 0 | 0.14 | |||||||
| NGC 6802 | 8.95 | 11.9 ± 0.9 | 156 | 7 | 2 | 2 | 7 | 1 | 1 | 1.28 | 50 | |||||
| Tr 14 | 6.67 | −15.0 | 858 | 82 | 3 | 2 | 1 | 19 | 0 | 0.35 | ||||||
| Tr 20 | 9.20 | −40.2 ± 1.3 | 1316 | 84 | 19 | 3 | 7 | 9 | 24 | 1 | 1 | 1.44 | 5 | |||
| Tr 23 | 8.90 | −61.3 ± 0.9 | 164 | 5 | 1 | 1 | 5 | 0 | 0.61 | |||||||
| Be 25 | 9.70 | + 134.3 ± 0.2 | 38 | 2 | 2 | 2 | 1 | 0 | 5.26 | |||||||
| Be 81 | 8.93 | 48.3 ± 0.6 | 265 | 5 | 2 | 1 | 1 | 6 | 0 | 0.75 | ||||||
|
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| Total | 50 863 | 1092 | 342 | 128 | 107 | 107 | 266 | 11 | 7 | 1 | 3 | 0.68 | 3 | |||
Notes. The column “log age” lists the logarithm of the cluster age (in years) from Cantat-Gaudin et al. (2014; NGC 6705), Spina et al. (in prep.; IC 2391, IC 2602, IC4665, NGC 2243, NGC 2264, NGC 2541, NGC 2547, NGC 3293, NGC 3532, NGC 6530), Bellini et al. (2010; M 67), Bragaglia & Tosi (2006; NGC 2243), Sung et al. (2002; NGC 2516), Friel et al. (2014; NGC 4815), Jacobson et al. (2016; NGC 6005, NGC 6633), VandenBerg et al. (2013; NGC 6705), Tang et al. (2017; NGC 6802), Donati et al. (2014; Tr 20 and Berkeley 81, written Be 81), Overbeek et al. (2017; Tr 23), and Carraro et al. (2007; Be 25). The column vr lists the radial velocity; for the clusters with ages older than 100 Myr see Jacobson et al. (2016, only UVES targets) excepted for M 67 (Casamiquela et al. 2016), NGC 2243 (Smiljanic et al. 2016); Friel et al. (2014; NGC 4815), Harris (1996; NGC 6752). For the young clusters, see Dias et al. (2002; IC 2391, IC 2602, IC 4665, NGC 2264, NGC2451, NGC 2547, NGC 3293, NGC 6530), and Carraro et al. (2007; Be 25). The column “# stars” lists the number of stars in that particular field/cluster observed by the GES. The column “doe” gives the number of SBs detected automatically, whereas the column “confirmed” represents the number of SBs kept after visual inspection of CCFs and associated spectra. The columns labelled “A”, “B”, and “C” list the number of confirmed systems by confidence flag (probable, possible, and tentative, respectively). No SB2 or SB3 candidates have been found yet with the doe code for the following clusters within the GES: Be 44 (93), M 15 (109), M 2 (110), NGC 104 (1138), NGC 1851 (127), NGC 1904 (113), NGC 2808 (112), NGC 362 (304), NGC 4372 (120), NGC 4833 (102), and NGC 5927 (124), where the numbers in parentheses give the number of stars observed in each cluster.
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