A spectroscopic study of the open cluster NGC 6475 (M 7) - Chemical abundances from stars in the range Teff = 4500–10 000 K

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Table 2:

Abundances for the Sun and Vega as obtained from the line lists used in this work.
El.	Sun	Sun $_{\rm GS98}$	Vega	Vega $_{\rm Qi01}$
HeI	-	10.99	-	-
CI	8.50	8.52	8.52	8.46
CI $_{\rm NLTE}$	-	-	8.57	-
NI	7.95	7.92	7.98	8.00
NI $_{\rm NLTE}$	-	-	7.58	-
OI	8.83	8.83	8.82	9.01
OI $_{\rm NLTE}$	-	-	8.74	-
NaI	6.37	6.33	6.63	6.45
NaI $_{\rm NLTE}$	6.32	6.33	6.33	-
MgI	7.54	7.58	7.14	6.81
MgI $_{\rm NLTE}$	7.56	7.58	-	-
AlI	6.43	6.47	-	-
SiI	7.61	7.55	-	-
CaI	6.39	6.36	5.65	5.41
ScII	3.12	3.17	2.56	2.33
TiI	4.94	5.02	-	-
TiII	4.96	5.02	4.52	4.58
VI $_{\rm Hyp}$	4.00	4.00	-	-
CrI	5.63	5.67	-	-
CrII	5.67	5.67	5.20	5.19
FeI	7.50	7.50	7.03	6.94
FeII	7.51	7.50	7.01	6.93
CoI	4.85	4.92	-	-
NiI	6.28	6.25	-	-
CuI	4.19	4.21	-	-
ZnI	4.61	4.60	-	-
YII	2.24	2.24	-	-
BaII $_{\rm Hyp}$	2.34	2.13	1.85	0.81
LaII	1.26	1.17	-	-
CeII	1.53	1.58	-	-
NdII	1.59	1.50	-	-

Abundances for the Sun are compared with Grevesse & Sauval (1998) (Sun $_{\rm GS98}$ ),
those for Vega with Qiu et al. (2001) (Vega $_{\rm Qi01}$ ).

Source LaTeX | All tables | In the text

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