Table 2: Changes ( $\Delta$ ) in the derived N abundance caused by errors in model atmosphere parameters for HD 122563, a cool star, and CS 22948-066 (hotter). A is the adopted model; B, C, and D vary log g, v_t, and $T_{{\rm eff}}$ individually as shown, while in model E, log g and v_t have been re-adjusted for consistency with the lower $T_{{\rm eff}}$ (see also Paper V, Tables 6 and 7).
HD 122563

A: $T_{{\rm eff}}$ = 4600 K, log g = 1.0 dex, vt = 2.0 km s^-1

B: $T_{{\rm eff}}$ = 4600 K, log g = 0.9 dex, vt = 2.0 km s^-1

C: $T_{{\rm eff}}$ = 4600 K, log g = 1.0 dex, vt = 1.8 km s^-1

D: $T_{{\rm eff}}$ = 4500 K, log g = 1.0 dex, vt = 2.0 km s^-1

E: $T_{{\rm eff}}$ = 4500 K, log g = 0.6 dex, vt = 1.8 km s^-1

$\Delta_{{\rm B-A}}$ $\Delta_{{\rm C-A}}$ $\Delta_{{\rm D-A}}$ $\Delta_{{\rm E-A}}$

$\rm [Fe/H]$ 0.03 0.03 -0.11 0.03

logN(Li) 0.01 0.00 -0.12 -0.06

logN(C) 0.04 0.00 -0.23 -0.08

$\rm [C/Fe~I]$ 0.02 -0.09 -0.03 -0.05

logN(N) 0.05 0.00 -0.30 -0.05

$\rm [N/Fe~I]$ 0.05 -0.13 -0.14 -0.06

$\rm [C/N]$ -0.01 0.00 0.10 0.00

$\rm [(C+N)/Fe~I]$ 0.07 -0.02 -0.24 0.05

CS 22948-066

A: $T_{{\rm eff}}$ = 5100 K, log g = 1.8 dex, vt = 2.0 km s^-1

B: $T_{{\rm eff}}$ = 5100 K, log g = 1.7 dex, vt = 2.0 km s^-1

C: $T_{{\rm eff}}$ = 5100 K, log g = 1.8 dex, vt = 1.8 km s^-1

D: $T_{{\rm eff}}$ = 5000 K, log g = 1.8 dex, vt = 2.0 km s^-1

E: $T_{{\rm eff}}$ = 5000 K, log g = 1.5 dex, vt = 2.0 km s^-1

$\Delta_{{\rm B-A}}$ $\Delta_{{\rm C-A}}$ $\Delta_{{\rm D-A}}$ $\Delta_{{\rm E-A}}$

$\rm [Fe/H]$ -0.02 +0.02 -0.05 -0.11

logN(Li) 0.01 0.00 -0.11 -0.10

logN(C) +0.04 0.00 -0.20 -0.10

$\rm [C/Fe~I]$ +0.04 -0.05 -0.09 +0.00

logN(N) +0.05 0.00 -0.30 -0.10

$\rm [N/Fe~I]$ +0.05 -0.05 -0.19 -0.01

$\rm [C/N]$ -0.01 0.00 0.07 -0.03

$\rm [(C+N)/Fe~I]$ 0.07 -0.02 -0.24 0.01

**Table 2:** Changes ( $\Delta$ ) in the derived N abundance caused by errors in model atmosphere parameters for HD 122563, a cool star, and CS 22948-066 (hotter). A is the adopted model; B, C, and D vary log g, v_t, and $T_{{\rm eff}}$ individually as shown, while in model E, log g and v_t have been re-adjusted for consistency with the lower $T_{{\rm eff}}$ (see also Paper V, Tables 6 and 7).
HD 122563
A: $T_{{\rm eff}}$ = 4600 K, log g = 1.0 dex, vt = 2.0 km s^-1
B: $T_{{\rm eff}}$ = 4600 K, log g = 0.9 dex, vt = 2.0 km s^-1
C: $T_{{\rm eff}}$ = 4600 K, log g = 1.0 dex, vt = 1.8 km s^-1
D: $T_{{\rm eff}}$ = 4500 K, log g = 1.0 dex, vt = 2.0 km s^-1
E: $T_{{\rm eff}}$ = 4500 K, log g = 0.6 dex, vt = 1.8 km s^-1
	$\Delta_{{\rm B-A}}$	$\Delta_{{\rm C-A}}$	$\Delta_{{\rm D-A}}$	$\Delta_{{\rm E-A}}$
$\rm [Fe/H]$	0.03	0.03	-0.11	0.03

logN(Li)	0.01	0.00	-0.12	-0.06

logN(C)	0.04	0.00	-0.23	-0.08
$\rm [C/Fe~I]$	0.02	-0.09	-0.03	-0.05

logN(N)	0.05	0.00	-0.30	-0.05
$\rm [N/Fe~I]$	0.05	-0.13	-0.14	-0.06

$\rm [C/N]$	-0.01	0.00	0.10	0.00

$\rm [(C+N)/Fe~I]$	0.07	-0.02	-0.24	0.05
CS 22948-066
A: $T_{{\rm eff}}$ = 5100 K, log g = 1.8 dex, vt = 2.0 km s^-1
B: $T_{{\rm eff}}$ = 5100 K, log g = 1.7 dex, vt = 2.0 km s^-1
C: $T_{{\rm eff}}$ = 5100 K, log g = 1.8 dex, vt = 1.8 km s^-1
D: $T_{{\rm eff}}$ = 5000 K, log g = 1.8 dex, vt = 2.0 km s^-1
E: $T_{{\rm eff}}$ = 5000 K, log g = 1.5 dex, vt = 2.0 km s^-1
	$\Delta_{{\rm B-A}}$	$\Delta_{{\rm C-A}}$	$\Delta_{{\rm D-A}}$	$\Delta_{{\rm E-A}}$
$\rm [Fe/H]$	-0.02	+0.02	-0.05	-0.11

logN(Li)	0.01	0.00	-0.11	-0.10

logN(C)	+0.04	0.00	-0.20	-0.10
$\rm [C/Fe~I]$	+0.04	-0.05	-0.09	+0.00

logN(N)	+0.05	0.00	-0.30	-0.10
$\rm [N/Fe~I]$	+0.05	-0.05	-0.19	-0.01

$\rm [C/N]$	-0.01	0.00	0.07	-0.03

$\rm [(C+N)/Fe~I]$	0.07	-0.02	-0.24	0.01

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and reductions
	3 Abundance analysis
	4 Mixing in metal-poor giants
	5 CNO elements in the early Galaxy
	6 Conclusions
	References