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Table 3
Spectral lines we used to determine the stellar Fe, Sr, Ba, and Eu abundances.
| Species | λ,Å | Eexc, eV | log gf | Ref. |
|---|---|---|---|---|
| Fe II | 4923.93 | 2.89 | −1.42 | (1) |
| Fe II | 5018.44 | 2.89 | −1.23 | (1) |
| FeII | 5197.58 | 3.23 | −2.24 | (2) |
| Fe II | 5264.81 | 3.23 | −3.02 | (2) |
| Fe II | 5284.11 | 2.89 | −3.09 | (2) |
| Fe II | 5325.55 | 3.22 | −3.21 | (2) |
| Fe II | 5414.07 | 3.22 | −3.54 | (2) |
| Fe II | 5425.26 | 3.20 | −3.28 | (2) |
| Sr II | 4077.72 | 0.00 | 0.15 | (3) |
| Sr II | 4215.54 | 0.00 | −0.17 | (3) |
| Ba II | 5853.67 | 0.60 | −1.00 | (3) |
| Ba II | 6496.90 | 0.60 | −0.38 | (3) |
| Eu II | 4129.72 | 0.00 | 0.22 | (4) |
| Eu II | 3819.671 | 0.00 | 0.51 | (4) |
| Eu II | 3907.111 | 0.21 | 0.17 | (4) |
| Eu II | 4205.022 | 0.00 | 0.21 | (4) |
Notes. (1) Mashonkina et al. (2019), (2) Raassen & Uylings (1998) corrected by −0.11 dex following Grevesse & Sauval (1999), (3) Reader et al. (1980), (4) Lawler et al. (2001). 1 Only for HE2327-5642, 2 for HE2327-5642 and HE1219-0312.
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