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Table A.2.

Astrophysical parameters of clusters in the LMC age gap. The age determination of ESO 121-03 from Mackey et al. (2006) is presented as a range, as the authors express it. For the metallicities of YMCA 53 and YMC 61, Gatto et al. (2024) use the expected values from the age-metallicity relation determined by Piatti & Geisler (2013), Parisi et al. (2015). For YMCA 53, YMCA 61, and KMHK 1592, the assumed distance is the same as of the center of the LMC (de Grijs et al. 2014). Milone et al. (2023) estimated uncertainties only for specific clusters as indicators of the precision of their analysis. We adopted the values from Kron 1, which had the closest age to the determination for SL 2, in the same work.

Cluster Age (Gyr) [Fe/H] Distance (kpc) Extinction parameter Reference
DES001SC04 4.17 ± 1.08 −0.88 ± 0.12 47.21 ± 0.22 E(g − r) = 0.06 ± 0.05 Pieres et al. (2016)
NGC 1997 4.47 ± 0.10 −1.18 ± 0.09 46.34 ± 0.21 E(g − r) = 0.08 ± 0.01 Pieres et al. (2016)
KMHK 1762 5.50 ± 1.90 assumed as −0.91 52 . 97 7.07 + 5.85 $ 52.97^{+5.85}_{-7.07} $ E ( B V ) = 0 . 09 0.05 + 0.06 $ E(B-V) = 0.09^{+0.06}_{-0.05} $ Gatto et al. (2022)
YMCA 53 5.62 ± 2.59 assumed as 49.9 from Skowron et al. (2021) Gatto et al. (2024)
YMCA 61 6.31 ± 2.90 assumed as 49.9 from Skowron et al. (2021) Gatto et al. (2024)
KMHK 1592 8.0 ± 0.5 −1.0 ± 0.2 assumed as 49.9 assumed as E(B − V) = 0.042 ± 0.010 Piatti (2022)
ESO 121-03 8.3 − 9.8 −0.97 ± 0.10 41.88 ± 1.74 E(V − I) = 0.04 ± 0.02 Mackey et al. (2006)
6.90 ± 0.45 −0.80 ± 0.15 46.56 ± 2.14 E(B − V) = 0.05 ± 0.02 Milone et al. (2023)

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