Impact of the convective mixing-length parameter α on stellar metallicity

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Table 3

Stellar parameters and iron abundances with different models of the open cluster sample.

Object	T_eff	log g	α^(a)	Ion	N^(b)	[Fe/H] with error, LTE			[Fe/H] with error, NLTE

	(K)					Old	New	Δ[Fe∕H] ^(c)	Old	New	Δ[Fe∕H] ^(c)
Tr 183	8225	3.87	1.50	Fe I	13	−0.004 ± 0.071	−0.030 ± 0.067	−0.026	0.007 ± 0.067	−0.018 ± 0.062	−0.025
				Fe II	5	0.064 ± 0.079	0.042 ± 0.076	−0.022	0.064 ± 0.079	0.042 ± 0.076	−0.022
Tr 118	6460	4.30	1.97	Fe I	19	−0.010 ± 0.069	−0.026 ± 0.065	−0.016	−0.002 ± 0.069	−0.016 ± 0.064	−0.014
				Fe II	6	0.040 ± 0.057	0.020 ± 0.075	−0.020	0.040 ± 0.057	0.020 ± 0.075	−0.020
Tr 114	6370	4.34	2.00	Fe I	16	−0.046 ± 0.052	−0.059 ± 0.048	−0.013	−0.039 ± 0.052	−0.052 ± 0.050	−0.013
				Fe II	7	−0.026 ± 0.048	−0.041 ± 0.053	−0.015	−0.026 ± 0.048	−0.041 ± 0.053	−0.015
Tr 53	6220	4.39	2.04	Fe I	37	−0.032 ± 0.056	−0.041 ± 0.054	−0.009	−0.024 ± 0.056	−0.035 ± 0.055	−0.011
				Fe II	12	−0.095 ± 0.032	−0.106 ± 0.033	−0.011	−0.096 ± 0.033	−0.106 ± 0.033	−0.010
Tr 65	5980	4.44	2.06	Fe I	35	−0.051 ± 0.068	−0.054 ± 0.066	−0.003	−0.043 ± 0.066	−0.046 ± 0.064	−0.003
				Fe II	13	−0.018 ± 0.025	−0.024 ± 0.035	−0.006	−0.018 ± 0.025	−0.024 ± 0.035	−0.006
Tr 85	5890	4.45	2.04	Fe I	35	−0.038 ± 0.062	−0.040 ± 0.059	−0.002	−0.033 ± 0.065	−0.035 ± 0.062	−0.002
				Fe II	11	0.010 ± 0.026	0.009 ± 0.037	−0.001	0.010 ± 0.026	0.009 ± 0.037	−0.001
Tr 12	5790	4.49	2.08	Fe I	29	−0.051 ± 0.058	−0.052 ± 0.058	−0.001	−0.048 ± 0.055	−0.049 ± 0.056	−0.001
				Fe II	16	0.000 ± 0.060	0.001 ± 0.067	0.001	−0.001 ± 0.061	0.000 ± 0.066	0.001
Tr A13	5360	4.53	2.14	Fe I	27	−0.003 ± 0.047	−0.001 ± 0.045	0.002	−0.017 ± 0.051	−0.015 ± 0.049	0.002
				Fe II	10	0.011 ± 0.055	0.019 ± 0.055	0.008	0.011 ± 0.055	0.019 ± 0.055	0.008
Tr 39	4930	2.76	1.96	Fe I	31	−0.063 ± 0.047	−0.082 ± 0.047	−0.019	−0.074 ± 0.050	−0.094 ± 0.050	−0.020
				Fe II	13	−0.020 ± 0.079	−0.039 ± 0.081	−0.019	−0.030 ± 0.074	−0.048 ± 0.076	−0.018

Notes. ^(a) New α value derived from M15. ^(b) Number of lines used to calculate the abundances.^(c)Abundance derived from new α value model minus abundance derived from old (fixed) α value.

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