Table 6
Abundances of the neutron-capture elements in the bluer region of the spectrum (3800–4800 Å).
| IC 2391 | IC 2391 | IC2391 | IC2391 | IC2391 | IC2391 | IC2602 | |
|---|---|---|---|---|---|---|---|
| CNAME | 08440521−5253171 | 08440521−5253171 | 08440521−5253171 | PMM1142 | PMM665 | PMM4362 | 10440681−6359351 |
| Instrument | UVES | FEROS | HARPS | UVES | UVES | UVES | HARPS |
| S∕N | 70 | 68 | 53 | 66 | 25 | 29 | 46 |
| v sin i ± σ | 18.4 ± 0.4 | 18.4 ± 0.4 | 18.4 ± 0.4 | 7.5 ± 0.4 | 8.2 ± 0.3 | 9 ± 0.3 | 12.1 ± 0.4 |
| v sin ilit. | 16.7 ± 0.8 | 16.7 ± 0.8 | 16.7 ± 0.8 | 7.3 (*) | 7.47 (*) | 8.61 (*) | 12.2 ± 0.7 |
| [Sr/Fe]I ± σ1 ± σ2 | – | − 0.05 ± 0.15 ± 0.08 | − 0.1 ± 0.20 ± 0.07 | – | – | – | + 0.03 ± 0.15 ± 0.09 |
| [Sr/Fe]II ± σ1 ± σ2 | – | − 0.08 ± 0.17 ± 0.09 | − 0.05 ± 0.20 ± 0.09 | – | + 0.03 ± 0.17 ± 0.10 | − 0.01 ± 0.17 ± 0.08 | − 0.04 ± 0.18 ± 0.08 |
| [Y/Fe]4398Å ± σ1 ± σ2 | + 0.3 ± 0.2 | + 0.25 ± 0.20 ± 0.08 | + 0.3 ± 0.25 ± 0.09 | + 0.31 ± 0.12 ± 0.10 | + 0.29 ± 0.16 ± 0.10 | + 0.20 ± 0.15 ± 0.11 | + 0.37 ± 0.30 ± 0.09 |
| [Zr/Fe]4050Å ± σ1 ± σ2 | – | – | – | − 0.01 ± 0.10 ± 0.08 | + 0.01 ± 0.17 ± 0.09 | – | – |
| [Zr/Fe]4208Å ± σ1 ± σ2 | – | – | – | + 0.03 ± 0.12 ± 0.07 | + 0.04 ± 0.20 ± 0.07 | + 0.03 ± 0.15 ± 0.08 | – |
| [La/Fe]3988Å ± σ1 ± σ2 | − 0.1 ± 0.10 ± 0.07 | − 0.10 ± 0.15 ± 0.07 | − 0.05 ± 0.20 ± 0.07 | − 0.11 ± 0.10 ± 0.08 | − 0.01 ± 0.12 ± 0.06 | − 0.06 ± 0.12 ± 0.07 | − 0.03 ± 0.25 ± 0.08 |
| [La/Fe]4087Å ± σ1 ± σ2 | – | – | – | − 0.06 ± 0.15 ± 0.06 | − 0.09 ± 0.13 ± 0.07 | − 0.08 ± 0.16 ± 0.08 | + 0.02 ± 0.30 ± 0.08 |
| [Ce/Fe]4073Å ± σ1 ± σ2 | – | – | – | − 0.03 ± 0.20 ± 0.07 | + 0.01 ± 0.15 ± 0.08 | – | – |
Notes. Individual abundances of the s-process elements derived with the lines in the 380–480 nm range. The first source of uncertainty (σ1) is due to the best fit procedure, while the second (σ2) is related to uncertainties in the stellar parameters (details of the computations can be found in Sect. 3.4). (*)Velocities are from De Silva et al. (2013).
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