Table 7
Mean values of the abundance ratios [X/Fe] of the GBS and the YOCs, and comparison with the literature values.
| Star/Cluster | [Cu/Fe] | [Sr/Fe] | [Y/Fe] | [Zr/Fe] | [Ba/Fe] | [La/Fe] | [Ce/Fe] |
|---|---|---|---|---|---|---|---|
| α Cen A | + 0.15 ± 0.20 | − 0.01 ± 0.01 | + 0.01 ± 0.04 | − 0.01 ± 0.04 | + 0.04 ± 0.15 | − 0.06 ± 0.03 | − 0.01 ± 0.01 |
| Luck (2018) | +0.18 ± 0.07 | − 0.08 ± 0.17 | − 0.01 ± 0.04 | − 0.07 ± 0.04 | − 0.12 ± 0.03 | − 0.07 ± 0.02 | − 0.04 ± 0.03 |
| Casamiquela et al. (2020) | + 0.07 ± 0.02 | – | − 0.07 ± 0.02 | - | − 0.11 ± 0.02 | − 0.01 ± 0.03 | − 0.11 ± 0.03 |
| Casali et al. (2020) | + 0.11 ± 0.03 | + 0.03 ± 0.01 | − 0.01 ± 0.01 | − 0.07 ± 0.02 | − 0.07 ± 0.01 | – | − 0.06 ± 0.02 |
| τ Cet | − 0.08 ± 0.20 | − 0.06 ± 0.01 | − 0.11 ± 0.03 | − 0.04 ± 0.03 | − 0.12 ± 0.12 | − 0.03 ± 0.03 | − 0.03 ± 0.08 |
| Luck (2018) | + 0.08 ± 0.08 | − 0.12 | − 0.09 ± 0.02 | + 0.07 ± 0.05 | − 0.08 ± 0.01 | + 0.17 ± 0.06 | + 0.07 ± 0.04 |
| Casamiquela et al. (2020) | + 0.05 ± 0.02 | – | − 0.02 ± 0.02 | – | − 0.09 ± 0.02 | + 0.11 ± 0.04 | − 0.14 ± 0.08 |
| β Hyi | − 0.01 ± 0.15 | − 0.06 ± 0.01 | − 0.05 ± 0.01 | − 0.05 ± 0.04 | − 0.08 ± 0.17 | − 0.04 ± 0.02 | − 0.03 ± 0.03 |
| Jofré et al. (2015a) | – | – | – | – | + 0.09 ± 0.10 | – | – |
| Bensby et al. (2014) | – | – | − 0.12 ± 0.11 | – | + 0.03 ± 0.05 | – | – |
| 18 Sco | − 0.02 ± 0.10 | + 0.055 ± 0.005 | − 0.06 ± 0.05 | 0.00 ± 0.01 | − 0.04 ± 0.15 | + 0.08 ± 0.03 | + 0.06 ± 0.04 |
| Luck (2018) | − 0.06 ± 0.04 | − 0.04 ± 0.17 | + 0.02 ± 0.02 | + 0.01 ± 0.09 | + 0.02 ± 0.01 | + 0.01 ± 0.02 | + 0.02 ± 0.03 |
| Casamiquela et al. (2020) | − 0.04 ± 0.02 | – | + 0.04 ± 0.01 | – | + 0.02 ± 0.01 | − 0.06 ± 0.03 | − 0.01 ± 0.04 |
| Casali et al. (2020) | − 0.03 ± 0.02 | + 0.09 ± 0.01 | + 0.07 ± 0.01 | + 0.06 ± 0.01 | + 0.04 ± 0.01 | – | + 0.07 ± 0.01 |
| IC 2391 | − 0.07 ± 0.02 | − 0.04 ± 0.05 | + 0.23 ± 0.03 | + 0.02 ± 0.02 | + 0.53 ± 0.02 | − 0.07 ± 0.03 | − 0.01 ± 0.02 |
| D’Orazi et al. (2009) | – | – | – | – | + 0.68 ± 0.07 | – | – |
| De Silva et al. (2013) | – | – | – | – | + 0.62 ± 0.07 | – | – |
| D’Orazi et al. (2017) | – | – | + 0.08 ± 0.02 | + 0.09 ± 0.03 | – | + 0.14 ± 0.02 | + 0.15 ± 0.05 |
| IC 2602 | − 0.10 ± 0.02 | − 0.01 ± 0.05 | + 0.19 ± 0.04 | 0.0 ± 0.35 (**) | + 0.40 ± 0.02 | − 0.01 ± 0.04 (**) | |
| D’Orazi et al. (2009) | – | – | – | – | +0.64 ± 0.07 | – | – |
| D’Orazi et al. (2017) | – | – | +0.08 ± 0.02 | +0.06 ± 0.01 | – | +0.10 ± 0.02 | +0.02 ± 0.02 |
| Spina et al. (2021) | − 0.15 ± 0.05 | - | + 0.17 ± 0.11 | – | + 0.34 ± 0.14 | – | – |
| IC 4665 | + 0.05 ± 0.04 | – | +0.34 ± 0.1 | – | + 0.60 ± 0.02 | – | – |
| Spina et al. (2021) | − 0.27 ± 0.05 | – | + 0.29 ± 0.16 | – | + 0.37 ± 0.16 | + 0.48 ± 0.05 (***) | |
| NGC 2264 (*) | − 0.17 ± 0.15 | – | + 0.28 ± 0.05 | – | + 0.41 ± 0.12 | – | – |
| NGC 2516 | − 0.06 ± 0.03 | – | +0.09 ± 0.04 | – | + 0.31 ± 0.03 | – | + 0.03 ± 0.25 (**) |
| D’Orazi et al. (2009) | – | – | – | - | +0.41 ± 0.04 | – | – |
| Maiorca et al. (2011) | – | – | +0.16 ± 0.03 | – | – | – | +0.18 ± 0.02 |
| Magrini et al. (2018) | – | – | +0.11 ± 0.06 | +0.58 ± 0.07 | +0.20 ± 0.08 | – | +0.38 ± 0.10 |
| NGC 2547 | − 0.07 ± 0.05 | – | +0.16 ± 0.01 | – | + 0.53 ± 0.01 | – | – |
Notes. The uncertainties for the GBS stars is the standard deviation of different lines (for Cu and Ba, for which we only analysed one line, the error is the quadratic sum of σ1 and σ2). The uncertainties of the mean abundances computed for our clusters are the errors on the mean, representing the star-to-star variation. (*)Since we analysed only one star in this SFR, we report the individual abundance values and the uncertainties on the fitting procedure. (**)Measurement based on only one target. (***)Values affected by strong blends (Buder et al. 2021).
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