Table 1
Observational data used for this work: source, number of giants (defined as log g < 3.2), number of dwarfs (log g ≥ 3.2), method of analysis, spectral resolution, and abundances used.
Source | n_giants | n_dwarfs | Method | Spectral resolution | Abundances |
---|---|---|---|---|---|
Placco et al. (2014) (compilation) | 335(a) | 158 | 1D LTE | 35 000–60 000 | C, N, Sr, Ba |
Molaro et al. (2023) (compilation) | 27 | 24 | 1D LTE | 32 000–140 000 | 12C, 13C, Sr, Ba |
Israelian et al. (2004) | 0 | 31 | 1D LTE | 35 000–50 000 | N, O |
Spite et al. (2005) | 16(b) | 0 | 1D LTE(c) | 47 000 | N, O |
Lai et al. (2008) | 16 | 12 | 1D LTE | 60 000 | C, N, O |
Fabbian et al. (2009) | 0 | 43 | 1D NLTE | 60 000 | C, O |
Norris et al. (2013) | 15 | 6 | 1D LTE | 40 000 | O |
Zhao et al. (2016) | 0 | 11 | 1D NLTE | 60 000 | C, O |
Cescutti et al. (2022); François et al. (2024) | 41 | 0 | 1D LTE | 65 000–115 000 | Sr, Ba |
Notes. (a)An evolutionary correction has been applied to the C abundances (Placco et al. 2014). (b)Only unmixed giants have been selected, using the surface abundance of Li as a diagnostic of the mixing (Spite et al. 2005). (c)Nitrogen and oxygen have been corrected for 3D effects (Spite et al. 2005).
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