Table 4: Sensitivities of abundance ratios to variations in the atmospheric parameters and to errors in the equivalent widths, as computed for a typical program star with $T_{\rm eff} = 4500$ K. The total error is computed as the quadratic sum of the three dominant sources of error, $T_{\rm eff}$ , v_t, and errors in the ${\it EW}$ s (Col. 8: tot.1) or as the sum of all contributions (Col. 9: tot.2).
Ratio $\Delta T_{\rm eff}$ $\Delta$ $\log g$ $\Delta$ [A/H] $\Delta v_t$ $\langle N_{lines}\rangle$ $\Delta$ EW tot.1 tot.2

(+50 K) (+0.2 dex) (+0.10 dex) (+0.20 km s^-1) (dex) (dex)

(1) (2) (3) (4) (5) (6) (7) (8) (9)

[Fe/H] I +0.047 +0.001 -0.001 -0.029 38 +0.021 0.059 0.059

[Fe/H] II -0.040 +0.010 +0.017 -0.011 3 +0.076 0.087 0.089

[O/Fe] I +0.046 -0.001 +0.004 +0.009 2 +0.093 0.104 0.104

[Na/Fe] II -0.006 -0.006 -0.020 +0.005 4 +0.066 0.066 0.070

**Table 4:** Sensitivities of abundance ratios to variations in the atmospheric parameters and to errors in the equivalent widths, as computed for a typical program star with $T_{\rm eff} = 4500$ K. The total error is computed as the quadratic sum of the three dominant sources of error, $T_{\rm eff}$ , v_t, and errors in the ${\it EW}$ s (Col. 8: tot.1) or as the sum of all contributions (Col. 9: tot.2).
Ratio	$\Delta T_{\rm eff}$	$\Delta$ $\log g$	$\Delta$ [A/H]	$\Delta v_t$	$\langle N_{lines}\rangle$	$\Delta$ EW	tot.1	tot.2
	(+50 K)	(+0.2 dex)	(+0.10 dex)	(+0.20 km s^-1)			(dex)	(dex)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
[Fe/H] I	+0.047	+0.001	-0.001	-0.029	38	+0.021	0.059	0.059
[Fe/H] II	-0.040	+0.010	+0.017	-0.011	3	+0.076	0.087	0.089
[O/Fe] I	+0.046	-0.001	+0.004	+0.009	2	+0.093	0.104	0.104
[Na/Fe] II	-0.006	-0.006	-0.020	+0.005	4	+0.066	0.066	0.070

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