Table 1
The metal content, TO, RGB bump brightness, and age estimates from both TO and
for the selected sample of GCs.
| Cluster | [Fe/H] | [α/Fe] | [M/H]a | mF606W(TO) | MF606W(TO) | mF606W(Bump) | Age(MSTO)b | Age()c |
|
|
||||||||
| NGC 0104 | –0.76 | 0.42 | –0.45 ± 0.11 | 17.53 ± 0.07 | 4.27 ± 0.11 | 14.26 ± 0.004 | 13.98 ± 2.11 | 9.66 ± 3.55 |
| NGC 0362 | –1.30 | 0.30 | –1.09 ± 0.12 | 18.74 ± 0.05 | 3.95 ± 0.09 | 15.17 ± 0.007 | 11.85 ± 1.62 | 7.02 ± 1.18 |
| NGC 1851 | –1.18 | 0.38 | –0.90 ± 0.14 | 19.40 ± 0.05 | 3.93 ± 0.09 | 15.84 ± 0.008 | 10.88 ± 1.70 | 7.95 ± 2.17 |
| NGC 5904 | –1.33 | 0.38 | –1.05 ± 0.11 | 18.37 ± 0.03 | 3.97 ± 0.09 | 14.73 ± 0.008 | 11.95 ± 1.53 | 7.75 ± 1.19 |
| NGC 6093 | –1.75 | 0.24 | –1.58 ± 0.14 | 19.67 ± 0.05 | 4.01 ± 0.09 | 15.72 ± 0.010 | 14.69 ± 1.93 | 8.53 ± 1.74 |
| NGC 6218 | –1.33 | 0.41 | –1.03 ± 0.11 | 18.18 ± 0.04 | 4.13 ± 0.09 | 14.49 ± 0.013 | 14.12 ± 1.99 | 8.60 ± 1.86 |
| NGC 6254 | –1.57 | 0.37 | –1.30 ± 0.11 | 18.36 ± 0.04 | 4.00 ± 0.09 | 14.47 ± 0.012 | 13.32 ± 1.80 | 10.38 ± 1.91 |
| NGC 6341 | –2.35 | 0.46 | –2.01 ± 0.12 | 18.60 ± 0.04 | 3.86 ± 0.09 | 14.49 ± 0.011 | 14.23 ± 1.77 | 8.79 ± 1.07 |
| NGC 6541 | –1.82 | 0.43 | –1.50 ± 0.14 | 18.70 ± 0.04 | 4.02 ± 0.09 | 14.76 ± 0.010 | 14.51 ± 1.97 | 9.38 ± 1.87 |
| NGC 6637 | –0.59 | 0.31 | –0.37 ± 0.13 | 19.40 ± 0.07 | 4.27 ± 0.11 | 16.10 ± 0.008 | 13.69 ± 2.26 | 12.57 ± 3.91 |
| NGC 6723 | –1.10 | 0.50 | –0.72 ± 0.13 | 18.90 ± 0.05 | 4.21 ± 0.09 | 15.34 ± 0.010 | 14.12 ± 2.15 | 10.73 ± 3.61 |
| NGC 6752 | –1.55 | 0.43 | –1.23 ± 0.11 | 17.26 ± 0.03 | 4.02 ± 0.09 | 13.39 ± 0.012 | 13.28 ± 1.75 | 10.58 ± 1.76 |
Notes.
Cluster global metallicity obtained by combining the [Fe/H] estimates from Carretta et al. (2009) and the average α-elements enhancement from Carretta et al. (2010a) according to Eq. (3) in Salaris et al. (1993). The associated error bar is obtained by propagating the errors in [Fe/H] and [α/Fe] discussed in Sect. 2 accordingly.
Cluster age in Gyr estimated by using the TO magnitude and the theoretical calibration shown in the upper panel of Fig. 2.
Cluster age in Gyr estimated by using the
parameter and the theoretical calibration shown in the lower panel of Fig. 2.
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