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 3

Average abundances based on the individual spectra based in turn on the different temperature scales.

T_eff-scale	ΔT_eff	Δ log g	Δξ	Δlog ε(Ca) ^a	Δlog ε(Fe) ^b
	(K)	(cgs)	(km s^-1)	NLTE	NLTE

Victoria	1282 ± 86	1.59 ± 0.13	0.34 ± 0.06	0.05 ± 0.71	−0.33 ± 0.35
Al96+99	1299 ± 106	1.60 ± 0.21	0.32 ± 0.06	0.07 ± 0.39	−0.37 ± 0.39
RM05+Cas10	1375 ± 135	1.60 ± 0.22	0.39 ± 0.09	0.03 ± 0.60	−0.39 ± 0.43
Hα	1259 ± 128	1.61 ± 0.18	0.30 ± 0.08	0.05 ± 0.27	−0.43 ± 0.33

Notes. The differences were calculated based on the mean values derived from individual stars on the TOP (T_eff> 6200 K) and the middle of the RGB (5100 K <T_eff< 4900 K) and include the 1σ uncertainties.

^(a)

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

^(b)

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

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