Table 5.
Ba, Eu, Gd, and Dy abundances and errors for the 19 Gaia benchmarks stars identified in our sample.
| Star | T eff | log(g) | [M/H] | [Ba/Fe] | N l | [Eu/Fe] | N l | [Gd/Fe] | N l | [Dy/Fe] | N l | Spec. |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| F dwarf | ||||||||||||
| Procyon | 6424 | 3.81 | −0.34 | +0.30±0.25 | 3 | +0.20±0.11 | 3 | +0.11±0.47 | 4 | +0.13±0.28 | 2 | U |
| HD 49933 | 6482 | 3.90 | −0.54 | −0.40±0.37 | 2 | −0.07±0.49 | 3 | +0.67±0.50 | 3 | +0.18±0.45 | 2 | H |
| HD 84937 | 6300 | 3.71 | −2.33 | − | 0 | <+1.70 | 1 | <+1.70 | 2 | <+1.30 | 1 | U |
| FGK subgiants | ||||||||||||
| ;Eri | 5033 | 3.82 | +0.09 | −0.11±0.15 | 3 | +0.02±0.07 | 4 | −0.05±0.32 | 5 | −0.04±0.45 | 2 | H |
| HD 140283 | 5700 | 3.48 | −2.52 | <+2.00 | 2 | <+1.60 | 1 | <+1.60 | 1 | <+1.40 | 1 | F |
| ɛ For | 5041 | 3.42 | −0.67 | +0.04±0.33 | 3 | +0.37±0.10 | 3 | +0.49±0.22 | 3 | +0.47±0.35 | 2 | F |
| α Hyi | 5775 | 4.02 | −0.11 | +0.17±0.21 | 3 | +0.05±0.24 | 2 | −0.05±0.25 | 3 | +0.15±0.37 | 2 | F |
| Solar-type | ||||||||||||
| α Cen A | 5764 | 4.18 | +0.23 | −0.08±0.19 | 3 | −0.13±0.14 | 3 | −0.11±0.41 | 4 | −0.18±0.43 | 2 | H |
| HD 22879 | 5680 | 3.82 | −1.03 | +0.08±0.09 | 2 | +0.34±0.18 | 2 | +0.46±0.22 | 2 | +0.48±0.28 | 2 | H |
| Sun | 5707 | 4.33 | −0.04 | −0.07±0.07 | 3 | +0.04±0.19 | 4 | −0.06±0.29 | 5 | +0.04±0.20 | 2 | F |
| τ Cet | 5262 | 4.45 | −0.56 | −0.04±0.06 | 2 | +0.47±0.36 | 3 | −0.01±0.24 | 3 | +0.22±0.45 | 1 | F |
| α Cen B | 5151 | 4.41 | +0.18 | −0.11±0.23 | 3 | −0.03±0.03 | 3 | −0.05±0.45 | 4 | <+0.40 | 1 | H |
| 18 Sco | 5796 | 4.34 | +0.04 | +0.03±0.06 | 3 | +0.11±0.33 | 4 | −0.11±0.32 | 5 | +0.22±0.20 | 2 | H |
| μ Ara | 5789 | 4.39 | +0.25 | +0.02±0.09 | 3 | +0.10±0.27 | 3 | −0.06±0.62 | 3 | −0.10±0.12 | 2 | F |
| β Vir | 6061 | 3.86 | +0.17 | −0.07±0.19 | 3 | −0.22±0.45 | 3 | −0.36±0.37 | 4 | −0.17±0.13 | 2 | H |
| Red giants | ||||||||||||
| Arcturus | 4286 | 1.81 | −0.53 | − | 0 | +0.21±0.15 | 2 | +0.33±0.27 | 3 | +0.19±0.22 | 2 | U |
| ɛ Vir | 5197 | 2.98 | +0.12 | +0.77±0.19 | 3 | +0.13±0.17 | 3 | −0.02±0.41 | 3 | +0.31±0.11 | 2 | F |
| α Tau | 3839 | 1.12 | −0.03 | <+0.40 | 1 | <+0.40 | 1 | <+0.40 | 1 | <0.40 | 1 | F |
| K dwarfs | ||||||||||||
| ɛ Eri | 5170 | 4.72 | −0.06 | +0.23±0.17 | 3 | +0.25±0.42 | 3 | − | 0 | +0.34±0.51 | 2 | F |
Notes. The number of spectral lines used to derive the r- and s-process abundances is indicated by N l. The spectrograph is also indicated in the last column. We note that for the Sun we averaged parameters and abundances of 22 solar spectra.
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