New stellar age estimates using SPInS based on Gaia DR3 photometry and LAMOST DR8 abundances

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Volume 692 (December 2024)

A&A, 692 (2024) A243

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Table 1

Clusters with their properties taken from the literature.

Cluster	Distance (pc)	A_V (mag)	Age (Myr)	[Fe/H] (dex)	Age_SPInS,mode (Myr)	Age_SPInS (Myr)	N_stars
Melotte 22	128	0.18 ⁽¹⁾	77 ⁽¹⁾, 109 ⁽²⁾, 125 ⁽⁴⁾	0.051 ± 0.078 ⁽ⁱⁱ⁾	150	$230_{- 68}^{+ 161}$ $\[230_{-68}^{+161}\]$	6
NGC 1039	534	0.24 ⁽²⁾	131 ⁽¹⁾, 250 ⁽²⁾	−0.046 ± 0.092 ⁽ⁱⁱ⁾	350	$386_{- 111}^{+ 822}$ $\[386_{-111}^{+822}\]$	20
NGC 3114	1021	0.27 ⁽¹⁾	144 ⁽¹⁾, 130 ⁽³⁾, 158 ⁽⁴⁾	0.050 ± 0.060 ⁽ⁱ⁾	350	$338_{- 108}^{+ 193}$ $\[338_{-108}^{+193}\]$	133
NGC 2287	688	0.06 ⁽³⁾	169 ⁽¹⁾, 250 ⁽³⁾, 200 ⁽⁴⁾	−0.110 ± 0.010 ⁽ⁱ⁾	650	$1071_{- 573}^{+ 1570}$ $\[1071_{-573}^{+1570}\]$	170
NGC 6475	285	0.30 ⁽¹⁾	223 ⁽¹⁾, 346 ⁽²⁾, 251 ⁽⁴⁾	−0.012 ± 0.050 ⁽ⁱⁱⁱ⁾	350	$592_{- 243}^{+ 840}$ $\[592_{-243}^{+840}\]$	87
NGC 2516	423	0.22 ⁽²⁾	239 ⁽¹⁾, 302 ⁽²⁾, 178 ⁽⁴⁾	0.050 ± 0.110 ⁽ⁱ⁾	450	$457_{- 113}^{+ 129}$ $\[457_{-113}^{+129}\]$	21
NGC 3532	498	0.07 ⁽²⁾	350 ⁽¹⁾, 398 ⁽²⁾, 350 ⁽³⁾, 354 ⁽⁴⁾	−0.034 ± 0.012 ⁽ⁱⁱⁱ⁾	650	$1082_{- 485}^{+ 1432}$ $\[1082_{-485}^{+1432}\]$	408
NGC 2447	1018	0.11 ⁽³⁾	549 ⁽¹⁾, 549 ⁽²⁾, 560 ⁽³⁾, 562 ⁽⁴⁾	−0.050 ± 0.010 ⁽ⁱ⁾	650	$774_{- 158}^{+ 405}$ $\[774_{-158}^{+405}\]$	118
NGC 2632	183	0.08 ⁽²⁾	676 ⁽¹⁾, 708 ⁽²⁾, 630 ⁽⁴⁾	0.118 ± 0.014 ⁽ⁱⁱⁱ⁾	750	$829_{- 158}^{+ 288}$ $\[829_{-158}^{+288}\]$	45
NGC 5822	854	0.39 ⁽¹⁾	912 ⁽¹⁾, 890 ⁽³⁾, 891 ⁽⁴⁾	0.080 ± 0.080 ⁽ⁱ⁾	950	$1074_{- 178}^{+ 273}$ $\[1074_{-173}^{+273}\]$	113
NGC 6819	2765	0.40 ⁽¹⁾	2238 ⁽¹⁾, 1995 ⁽⁴⁾, 2400 ⁽⁵⁾, 2200 ⁽⁶⁾	−0.050 ± 0.010 ⁽ⁱⁱⁱ⁾	2950	$3151_{- 627}^{+ 864}$ $\[3151_{-627}^{+864}\]$	136
NGC 2682	889	0.12 ⁽³⁾	4265 ⁽¹⁾, 3467 ⁽²⁾, 3630 ⁽³⁾, 3630 ⁽⁴⁾	−0.075 ± 0.007 ⁽ⁱⁱⁱ⁾	4450	$5166_{- 1022}^{+ 1297}$ $\[5166_{-1022}^{+1297}\]$	124
NGC 188	1698	0.26 ⁽²⁾	7079 ⁽¹⁾, 5495 ⁽²⁾, 7585 ⁽⁴⁾, 6000 ⁽⁷⁾	−0.030 ± 0.015 ⁽ⁱⁱⁱ⁾	6750	$7412_{- 1091}^{+ 1312}$ $\[7412_{-1091}^{+1312}\]$	143
NGC 6397	2488	0.56	12600 ⁽⁸⁾, 13000⁽⁹⁾, 12800 ⁽¹⁰⁾	−1.990 ± 0.010 ^(iv)	13450	$13292_{- 943}^{+ 764}$ $\[13292_{-943}^{+764}\]$	83

Notes. We include the ages determined in this work (see Sect. 4.2, median with uncertainties using the median and 16/84 quantiles, and the mode of the distributions), and the number of stars used (N_stars). Distances to OCs correspond to the values derived by Cantat-Gaudin et al. (2020), except for the globular cluster NGC 6397 for which we use distance and extinction derived by Baumgardt & Vasiliev (2021). ⁽¹⁾ Cantat-Gaudin et al. (2020), ⁽²⁾ Gaia Collaboration (2018), ⁽³⁾ Tsantaki et al. (2023), ⁽⁴⁾ Netopil et al. (2022), ⁽⁵⁾ Brewer et al. (2016), ⁽⁶⁾ Rodrigues et al. (2017), ⁽⁷⁾ Meibom et al. (2009), ⁽⁸⁾ Correnti et al. (2018), ⁽⁹⁾ VandenBerg et al. (2013), ⁽¹⁰⁾ Torres et al. (2015). ⁽ⁱ⁾ Netopil et al. (2016), ⁽ⁱⁱ⁾ Zhong et al. (2020), ⁽ⁱⁱⁱ⁾ Casamiquela et al. (2021), ^(iv) Carretta et al. (2009).

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