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Table 4
Abundances of the GBS of the neutron-capture process elements.
| El. | λ (Å) | [X/Fe]α Cen A | [X/Fe]τ Cet | [X/Fe]β Hyi | [X/Fe]18 Sco |
|---|---|---|---|---|---|
| 3800–4800 Å | |||||
| Sr I(NLTE) | 4607.33 | − 0.02 ± 0.08 ± 0.07 | − 0.05 ± 0.08 ± 0.07 | − 0.05 ± 0.11 ± 0.07 | + 0.05 ± 0.1 ± 0.06 |
| Sr II | 4215.52 | 0.00 ± 0.2 ± 0.1 | − 0.07 ± 0.19 ± 0.1 | − 0.07 ± 0.22 ± 0.09 | + 0.06 ± 0.19 ± 0.09 |
| Y II | 4398.01 | − 0.03 ± 0.15 ± 0.09 | − 0.14 ± 0.11 ± 0.07 | − 0.04 ± 0.1 ± 0.07 | + 0.01 ± 0.13 ± 0.07 |
| Zr II | 4050.32 | + 0.02 ± 0.12 ± 0.06 | − 0.07 ± 0.14 ± 0.08 | − 0.02 ± 0.13 ± 0.08 | − 0.01 ± 0.11 ± 0.06 |
| Zr II | 4208.98 | + 0.01 ± 0.15 ± 0.07 | − 0.05 ± 0.1 ± 0.09 | − 0.04 ± 0.12 ± 0.05 | + 0.01 ± 0.10 ± 0.07 |
| La II | 3988.51 | − 0.04 ± 0.1 ± 0.06 | − 0.01 ± 0.15 ± 0.06 | − 0.02 ± 0.15 ± 0.06 | + 0.10 ± 0.1 ± 0.07 |
| La II | 4086.71 | − 0.08 ± 0.15 ± 0.08 | − 0.05 ± 0.17 ± 0.07 | − 0.06 ± 0.16 ± 0.07 | + 0.06 ± 0.12 ± 0.08 |
| Ce II | 4073.47 | 0.00 ± 0.13 ± 0.06 | 0.03 ± 0.15 ± 0.05 | 0.00 ± 0.15 ± 0.05 | + 0.08 ± 0.08 ± 0.06 |
| 4800–6800 Å | |||||
| Cu I | 5105.54 | + 0.15 ± 0.20 ± 0.09 | − 0.08 ± 0.20 ± 0.11 | − 0.01 ± 0.15 ± 0.11 | − 0.02 ± 0.10 ± 0.10 |
| Y II | 4883.69 | + 0.02 ± 0.15 ± 0.13 | − 0.08 ± 0.13 ± 0.09 | − 0.06 ± 0.15 ± 0.08 | − 0.09 ± 0.09 ± 0.07 |
| Y II | 5087.42 | + 0.05 ± 0.15 ± 0.1 | − 0.11 ± 0.13 ± 0.07 | − 0.05 ± 0.11 ± 0.07 | − 0.10 ± 0.10 ± 0.07 |
| Zr II | 5112.27 | − 0.06 ± 0.20 ± 0.06 | − 0.01 ± 0.1 ± 0.07 | − 0.10 ± 0.07 ± 0.06 | + 0.01 ± 0.08 ± 0.07 |
| Ba II | 5853.69 | + 0.04 ± 0.15 ± 0.12 | − 0.12 ± 0.12 ± 0.07 | − 0.08 ± 0.17 ± 0.11 | − 0.04 ± 0.15 ± 0.1 |
| Ce II | 5274.23 | − 0.02 ± 0.14 ± 0.08 | − 0.08 ± 0.1 ± 0.05 | − 0.06 ± 0.08 ± 0.09 | + 0.03 ± 0.1 ± 0.05 |
Notes. The first source of uncertainty is due to the best fit procedure, while the second is related to uncertainties in the stellar parameters (details on the computations can be found in Sect. 3.4).
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