Atomic diffusion and mixing in old stars - VI. The lithium content of M30

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Volume 589 (May 2016)

A&A, 589 (2016) A61

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Table A.1

Derived elemental abundances for the coadded group-averaged spectra.

Group	T_eff (K)	log g (cgs)	log ε(Li)	log ε(Ca)	log ε(Fe)

Tip-RGB1	4288	0.80	−0.51 ± 0.03	4.33 ± 0.01	5.18 ± 0.03
Tip-RGB2	4525	1.16	0.06 ± 0.05	4.33 ± 0.02	5.16 ± 0.05
RGB1	4711	1.76	0.46 ± 0.11	4.35 ± 0.03	5.17 ± 0.04
RGB2	5031	2.35	1.00 ± 0.02	4.36 ± 0.02	5.17 ± 0.02
bRGB1	5175	2.76	1.04 ± 0.04	4.33 ± 0.03	5.16 ± 0.04
bRGB2	5337	3.19	1.17 ± 0.03	4.30 ± 0.02	5.16 ± 0.03
bRGB3	5418	3.38	1.30 ± 0.06	4.29 ± 0.05	5.11 ± 0.05
SGB1	5537	3.46	1.69 ± 0.05	4.29 ± 0.06	5.07 ± 0.07
SGB2	5676	3.62	1.98 ± 0.03	4.26 ± 0.06	5.03 ± 0.06
SGB3	5822	3.72	2.06 ± 0.03	4.23 ± 0.07	5.04 ± 0.07
TOP1	5970	3.78	2.00 ± 0.04	4.27 ± 0.07	5.03 ± 0.07
TOP2	6069	3.87	2.00 ± 0.02	4.27 ± 0.04	4.96 ± 0.04
TOP3	6316	3.99	2.15 ± 0.03	4.37 ± 0.05	4.87 ± 0.06

Δ log ϵ(X) ^a	1247	1.83	1.05 ± 0.04 ^b	−0.05 ± 0.06	−0.22 ± 0.06

Notes. Abundance uncertainties are based on the statistical error as calculated by SME.

^(a)

The abundance difference between TOP and RGB. The TOP and RGB abundances are the averages of results for the respective coadded group-averaged spectra. The uncertainty on the trends is based on the standard deviation of the two averages.

^(b)

For the Li trend we take the RGB2 abundance as the cooler RGB group-averaged abundances are affected by the deep-mixing episode occurring on the RGB.

^(Li)

Based on Li I λ6707.8, assuming NLTE.

^(Ca)

Based on three Ca I λλ6493.9, 6499.7 and 6717.7, all assuming NLTE.

^(Fe)

Based on five Fe I and one Fe II lines λλ6495.0, 6518.4, 6592.9, 6593.9, and 6678, and λ6516.1, assuming NLTE.

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