Table 6.
Mean abundances for NGC 3293 compared to the solar photospheric values (Asplund et al. 2021) and previous non-LTE spectroscopic studies in the literature.
| Sun | NGC 3293 |
|||
|---|---|---|---|---|
| This study | Hunter et al. (2009) | Mathys et al. (2002) | ||
| y | 0.076 ± 0.003 (a) | 0.096 ± 0.019 (129) | ... | 0.124 ± 0.018 (6) (b) |
| log ϵ(C) | 8.46 ± 0.04 | 8.13 ± 0.16 (25) | 7.97 ± 0.19 (27) | 8.20 ± 0.10 (6) |
| log ϵ(N) | 7.83 ± 0.07 | 7.72 ± 0.14 (24) | 7.60 ± 0.15 (27) | 7.77 ± 0.10 (6) |
| log ϵ(O) | 8.69 ± 0.04 | ... | 8.65 ± 0.17 (26) | 8.50 ± 0.13 (6) |
| log ϵ(Ne) | 8.06 ± 0.05 (c) | 7.91 ± 0.08 (12) | ... | ... |
| log ϵ(Mg) | 7.55 ± 0.03 | 7.45 ± 0.18 (128) | 7.22 ± 0.16 (26) | ... |
| log ϵ(Si) | 7.51 ± 0.03 | 7.56 ± 0.25 (28) (d) | 7.42 ± 0.09 (27) (e) | ... |
| [N/C] | −0.63 ± 0.09 | −0.40 ± 0.21 (22) | −0.37 ± 0.21 (27) | −0.43 ± 0.15 (6) |
| [N/O] | −0.86 ± 0.09 | ... | −1.05 ± 0.26 (26) | −0.73 ± 0.17 (6) |
Notes. Non cluster-members (Sect. 3.3) were excluded. The number of stars the estimate is based on is given in brackets.
The microturbulence was adjusted to derive the same Si abundance for each star in the cluster (see Hunter et al. 2007; Trundle et al. 2007).
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