Atomic diffusion and mixing in old stars - V. A deeper look into the globular cluster NGC 6752

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Table 5

Abundance sensitivity to stellar parameters.

Ion	T_eff + 100 K		log g + 0.1 dex		v_mic + 0.1 km s^-1
	TOP	bRGB	TOP	bRGB	TOP	bRGB


Li I	0.073	0.078	−0.002	−0.002	−0.001	0.006
Na I	0.032	0.046	0.002	0.000	0.000	−0.001
Mg I	0.080	0.116	−0.030	−0.050	−0.014	−0.007
Al I	...	0.037	...	0.001	...	0.004
Si I	0.025	0.036	0.004	0.008	0.009	−0.001
Ca I	0.048	0.065	0.000	−0.002	−0.007	−0.015
Sc II	...	0.043	...	0.035	...	−0.006
Ti II	0.038	0.050	0.032	0.026	−0.010	−0.025
Cr I	...	0.132	...	−0.020	...	−0.038
Fe I	0.075	0.109	−0.006	−0.014	−0.014	−0.027
Fe II	0.040	0.058	0.022	0.013	−0.019	−0.031
Ni I	...	0.073	...	0.004	...	−0.004

Notes. Effects on the averaged abundances are shown for the hot and cool ends of our sample, as defined in Table 6.

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