Table 2
Binary giants from the M07 sample that were the targets of an abundance analysis.
| Name | P | e | log Y | Teff | log g | [Fe/H] | TO | Ba | Spectro | Ref. | |
| (d) | (K) | (M⊙) | |||||||||
|
|
|||||||||||
| Candidate post-mass-transfer binaries | |||||||||||
| NGC 2539 209 | 11 655 | 0.16 | –2.29 | 4750 | 2.5 | +0.13 | 2.6 | N | HE | 1 | |
| NGC 2335 4 | 301 | 0.00 | –2.46 | 4750 | 1.2 | –0.03 | 4.3 | Y | HE | 1 | |
| IC 4756 139 | 3834 | 0.22 | –2.61 | 5220 | 2.7 | –0.06 | 2.7 | Y | HE | 1 | |
| NGC 2682 244 | 698 | 0.11 | –2.22 | 5150 | 2.6 | +0.00 | 1.4 | N | HE | 1 | |
| NGC 2682 170 | 4410 | 0.50 | –2.42 | 4250 | 1.7 | +0.00 | 1.4 | N | HE | 1 | |
| NGC 2682 143 | 43 | 0.00 | –2.75 | 5000 | 2.8 | +0.00 | 1.4 | N | HE | 1 | |
| NGC 2420 173 | 1479 | 0.43 | –2.42 | 5150 | 2.2 | –0.26 | 2.1 | Y | HE | 1, 2 | |
| NGC 6940 111 | 3571 | 0.30 | –2.05 | 5150 | 2.9 | +0.01 | 2.2 | N | HE | 1 | |
| NGC 2099 149 | 918 | 0.13 | –2.48 | 4900 | 2.1 | +0.08 | 3.0 | N | HE | 1 | |
| NGC 2099 966 | 3084 | 0.37 | –2.44 | 4600 | 2.1 | +0.08 | 3.0 | N? | HE | 1 | |
| NGC 2477 1044 | 3108 | 0.07 | –2.33 | 4780 | 2.6 | +0.01 | 2.1 | Y | HA | 1 | |
| NGC 4349 203 | 129.4 | 0.028 | –2.37 | 4940 | 2.2 | –0.07 | 3.2 | N | HA | 1 | |
| Binaries in the (P−e) gap | |||||||||||
| IC 4756 69 | 1994 | 0.05 ± 0.02 | –2.07 | 4870 | 2.6 | –0.06 | 2.7 | N | HE | 1 | |
| IC 4756 80 | 5791 | 0.03 ± 0.01 | –1.11 | 4910 | 2.8 | –0.06 | 2.7 | N | HE | 1 | |
| NGC 2682 224 | 6645 | 0.01 ± 0.01 | –1.04 | 4745 | 2.5 | 0.00 | 1.4 | N | HE | 1 | |
| Search for barium stars in clusters, from the literature | |||||||||||
| NGC 2420 250 | 1404 | 0.08 | –1.64 | – | – | –0.26 | 2.1 | Y | 2 | ||
| NGC 5822 2 | 1002 | 0.13 | –2.43 | 5100 | 2.4 | –0.15 | 2.1 | Y | 3 | ||
| NGC 5822 201 | ? | ? | ? | 5200 | 2.7 | –0.15 | 2.1 | Y | 3 | ||
| NGC 5822 151 | 1392 | 0.21 | –2.32 | 4900 | 2.5 | –0.11 | 2.1 | N | 4 | ||
| Reference star | |||||||||||
| NGC 752 208 | 5214 | 0.13 ± 0.01 | –1.35 | 4760 | 2.5 | –0.08 | 1.7 | N | HE | 1 | |
Notes. As before, Y ≡ f(M) /M1. The effective temperature Teff and gravity log g are derived as explained in Sect. B.1 or taken from the literature. The columns labelled TO and Ba provide the cluster turn-off mass (in M⊙) and the conclusion of the abundance analysis, respectively: Y (barium star) or N (not a barium star). In column “spectro”, HE stands for HERMES and HA for HARPS.
Reference. (1) This work; (2) Mermilliod & Mayor (2007); (3) Katime Santrich et al. (2013); (4) Sales Silva et al. (2014).
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