He-enriched STAREVOL models for globular cluster multiple populations - Self-consistent isochrones from ZAMS to the TP-AGB phase

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Volume 690 (October 2024)

A&A, 690 (2024) A22

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Table 1.

Initial chemical composition and α enhancement of our stellar tracks for each cluster

Name	[Fe/H]_1P	[α/Fe]	Z	Y_1P	Y_2P	Age^(*) [Gyr]	Age^(†) [Gyr]
NGC 4590	−2.2	+0.35	0.0002	0.248	[0.26, 0.27, 0.3, 0.33, 0.37, 0.4, 0.425, 0.45]	12.03 $_{- 0.54}^{+ 0.54}$ $^{+0.54}_{-0.54}$	12.75±0.75
NGC 6752	−1.53	+0.3	0.0009	0.248415	[0.27, 0.3, 0.4, 0.6]	13.48 $_{- 0.54}^{+ 0.81}$ $^{+0.81}_{-0.54}$	13.00 ± 0.50
NGC 2808	−1.15	+0.3	0.002	0.249	[0.26, 0.27, 0.3, 0.33, 0.37, 0.40, 0.425]	10.93 $_{- 1.03}^{+ 1.20}$ $^{+1.20}_{-1.03}$	12.00 ± 0.75
NGC 6441	−0.5	+0.2	0.008	0.255	[0.27, 0.3, 0.33, 0.37, 0.4, 0.425]	10.44 $_{- 1.62}^{+ 2.78}$ $^{+2.78}_{-1.62}$	12.25 ± 0.75

Notes. We also provide cluster ages from recent investigations to give a reference. Here, we recall that the derived ages depend on the physical parameters used in the stellar codes. ^(*)Ages taken from Valcin et al. (2020). ^(†)Ages taken from Tailo et al. (2020)

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