Inferring the efficiency of convective-envelope overshooting in red giant branch stars

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Volume 700 (August 2025)

A&A, 700 (2025) A163

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Table 1.

Properties (age, chemical composition, and reddening) and RGBb luminosities for all the clusters in our sample.

NGC	t_Age [Gyr]	[Fe/H]	[α/Fe]	[M/H]	E(B − V)	log L_RGBb [L_⊙]
1261	10.83 ± 0.42	−1.27 ± 0.08	0.360 ± 0.040 (1)	−1.01 ± 0.09	0.01 (P16)	$1 . 81_{- 0.01}^{+ 0.01}$ $1.81^{+0.01}_{-0.01}$
2298	12.84 ± 0.59	−1.96 ± 0.04	0.500 ± 0.100 (2)	−1.58 ± 0.09	0.22 (P16)	$1 . 85_{- 0.02}^{+ 0.02}$ $1.85^{+0.02}_{-0.02}$
4590	12.17 ± 0.51	−2.27 ± 0.04	0.350 ± 0.100 (2)	−2.02 ± 0.09	0.06 (P16)	$2 . 07_{- 0.01}^{+ 0.01}$ $2.07^{+0.01}_{-0.01}$
5053	12.68 ± 0.47	−2.30 ± 0.08	0.340 ± 0.070 (3)	−2.06 ± 0.10	0.01 (P16)	–
5466	13.02 ± 0.48	−2.31 ± 0.09	0.330 ± 0.100 (2)	−2.07 ± 0.12	0.02 (P16)	$2 . 11_{- 0.02}^{+ 0.02}$ $2.11^{+0.02}_{-0.02}$
6101	12.60 ± 0.53	−1.98 ± 0.07	0.400 ± 0.100 (4)	−1.69 ± 0.11	0.13 (P16)	$2 . 00_{- 0.01}^{+ 0.01}$ $2.00^{+0.01}_{-0.01}$
6121	12.18 ± 0.45	−1.18 ± 0.02	0.510 ± 0.100 (2)	−0.80 ± 0.09	0.44 (G19)	$1 . 69_{- 0.01}^{+ 0.01}$ $1.69^{+0.01}_{-0.01}$
6144	13.36 ± 0.54	−1.82 ± 0.05	0.400 ± 0.100 (4)	−1.53 ± 0.10	0.41 (G19)	$1 . 88_{- 0.02}^{+ 0.02}$ $1.88^{+0.02}_{-0.02}$
6218	12.97 ± 0.47	−1.33 ± 0.02	0.410 ± 0.100 (2)	−1.03 ± 0.08	0.19 (P16)	$1 . 77_{- 0.01}^{+ 0.01}$ $1.77^{+0.01}_{-0.01}$
6362	12.86 ± 0.44	−1.07 ± 0.05	0.370 ± 0.120 (5)	−0.80 ± 0.11	0.07 (P16)	$1 . 68_{- 0.01}^{+ 0.01}$ $1.68^{+0.01}_{-0.01}$
6397	13.06 ± 0.42	−1.99 ± 0.02	0.360 ± 0.100 (2)	−1.73 ± 0.08	0.19 (P16)	$2 . 00_{- 0.01}^{+ 0.01}$ $2.00^{+0.01}_{-0.01}$
6535	12.17 ± 0.63	−1.79 ± 0.07	0.320 ± 0.110 (6)	−1.56 ± 0.11	0.42 (G19)	–
6584	11.75 ± 0.47	−1.50 ± 0.09	0.410 ± 0.080 (7)	−1.20 ± 0.11	0.10 (P16)	$1 . 85_{- 0.01}^{+ 0.01}$ $1.85^{+0.01}_{-0.01}$
6637	12.19 ± 0.53	−0.59 ± 0.07	0.310 ± 0.100 (2)	−0.37 ± 0.10	0.15 (P16)	$1 . 55_{- 0.01}^{+ 0.01}$ $1.55^{+0.01}_{-0.01}$
6652	12.48 ± 0.46	−0.76 ± 0.14	0.200 ± 0.200 (8)	−0.62 ± 0.20	0.12 (P16)	$1 . 57_{- 0.02}^{+ 0.02}$ $1.57^{+0.02}_{-0.02}$
6717	12.89 ± 0.50	−1.26 ± 0.07	0.400 ± 0.100 (4)	−0.97 ± 0.11	0.26 (G19)	$1 . 77_{- 0.02}^{+ 0.02}$ $1.77^{+0.02}_{-0.02}$
6934	11.63 ± 0.46	−1.56 ± 0.09	0.400 ± 0.100 (1)	−1.27 ± 0.12	0.10 (G19)	$1 . 88_{- 0.01}^{+ 0.01}$ $1.88^{+0.01}_{-0.01}$
6791	8.30 ± 0.30	+0.29 ± 0.09	0.092 ± 0.007 (9)	+0.35 ± 0.09	0.14 (B12)	$1 . 37_{- 0.04}^{+ 0.04}$ $1.37^{+0.04}_{-0.04}$

Notes. The references for age and [Fe/H] are Kruijssen et al. (2019) and Carretta et al. (2010), respectively, for all the clusters except NGC 6791, for which we took quantities from Brogaard et al. (2012) and Brogaard et al. (2011), respectively. References for [α/Fe] are listed below, and [M/H] is computed with Eq. (3) from Salaris et al. (1993). The references for the reddening values are labelled as follows: P16 for Planck Collaboration Int. XLVIII (2016), G19 for Green et al. (2019), and B12 for Brogaard et al. (2012). Finally, the RGBb luminosities were derived with the methods described in Sect. 3.2 (for NGC 5053 and NGC 6535, no RGBb luminosity is provided since there are not enough stars on the RGB). The errors on log L_RGBb include the random error from the fit, the systematic error due the number of stars (see Appendix B), and the error on the distance modulus (Baumgardt & Hilker 2018). References. (1) Marino et al. (2021); (2) Carretta et al. (2010); (3) Sbordone et al. (2015); (4) Tailo et al. (2020); (5) Massari et al. (2017); (6) Bragaglia et al. (2017); (7) O’Malley & Chaboyer (2018); (8) Sharina & Shimansky (2020); (9) Linden et al. (2017).

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