The chemical abundance analysis of normal early A- and late B-type stars

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Volume 503 / No 3 (September I 2009)

A&A, 503 3 (2009) 945-962

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Table 5:

Error sources for the abundances of the chemical elements of 21 Peg.
Ion	Abundance	$\sigma_{\rm abn}$ (scatt.)	$\sigma_{\rm abn}$ ( $T_{{\rm eff}}$ )	$\sigma_{\rm abn}$ ( $\ensuremath{\log~g}$ )	$\sigma_{\rm abn}$ ( $\upsilon_{{\rm mic}}$ )	$\sigma_{\rm abn}$ (syst.)
	$\log (N/N_{\rm tot})$	(dex)	(dex)	(dex)	(dex)	(dex)
He I	-1.11	0.04	-0.08	0.03	0.00	0.09
C I	-3.66	0.14	-0.05	-0.13	-0.10	0.17
C II	-3.65	0.05	-0.17	-0.02	-0.08	0.19
N I	-3.95	0.12	-0.05	-0.07	-0.05	0.10
N II	-3.90:		-0.09	0.05	0.00	0.10
O I	-3.28	0.11	0.00	-0.02	-0.02	0.03
Ne I	-3.76	0.05	-0.18	-0.03	-0.06	0.19
Na I	-5.60		0.04	-0.04	-0.01	0.06
Mg I	-4.42	0.12	0.10	-0.06	-0.05	0.13
Mg II	-4.56	0.03	-0.02	-0.01	-0.02	0.03
Al I	-5.89		0.10	-0.03	0.00	0.10
Al II	-5.68	0.10	-0.09	0.01	-0.03	0.10
Si I	-4.95		0.10	-0.02	0.00	0.10
Si II	-4.49	0.13	-0.07	0.01	-0.03	0.08
Si III	-4.26	0.18	-0.16	0.04	-0.03	0.17
P II	-6.37	0.06	-0.08	0.02	-0.02	0.08
S II	-4.86	0.13	-0.14	0.00	-0.05	0.15
Ca I	-5.84	0.11	0.20	-0.07	0.00	0.21
Ca II	-5.98	0.08	0.03	-0.05	-0.04	0.07
Sc II	-9.37	0.10	0.12	-0.01	0.00	0.12
Ti II	-7.23	0.09	0.08	0.00	-0.02	0.08
V II	-7.98	0.06	0.06	0.02	0.00	0.06
Cr I	-6.29	0.09	0.13	-0.03	0.00	0.13
Cr II	-6.20	0.10	0.03	0.02	-0.01	0.04
Mn I	-6.54	0.21	0.14	-0.03	0.00	0.14
Mn II	-6.51	0.17	0.01	0.01	-0.01	0.01
Fe I	-4.52	0.13	0.11	-0.03	0.00	0.11
Fe II	-4.50	0.12	-0.02	0.02	-0.02	0.03
Fe III	-4.60	0.06	-0.10	0.06	-0.01	0.12
Co II	-6.75	0.18	0.01	0.03	0.00	0.03
Ni I	-5.71	0.05	0.09	-0.03	-0.01	0.10
Ni II	-5.61	0.09	-0.04	0.03	-0.01	0.05
Zn I	-6.86		0.10	-0.02	0.00	0.10
Sr II	-9.10	0.01	0.13	-0.03	-0.06	0.15
Y II	-9.76	0.15	0.13	-0.02	-0.01	0.13
Zr II	-9.48	0.28	0.11	0.00	0.00	0.11
Ba II	-9.19	0.06	0.14	-0.02	-0.01	0.14
Nd III	-10.09	0.07	0.04	0.04	0.00	0.06

Column 3 standard deviation $\sigma_{\rm abn}$ (scatt.) of the mean abundance obtained from different spectral lines (internal scattering); a blank means that the number of spectral lines is <3, hence no internal scattering could be estimated. (Note that these values are identical to those given in Table 4.) Columns 4-6 give the variation in abundance estimated by increasing $T_{{\rm eff}}$ by 200 K, $\ensuremath{\log~g}$ by 0.1 dex, and $\upsilon_{{\rm mic}}$ by 0.4 km s^-1, respectively. Column 7 gives the the mean error calculated applying the standard error propagation theory on the systematic uncertainties given in Col. 4-6, i.e., $\sigma_{\rm abn}^2$ (syst.) = $\sigma_{\rm abn}^2$ ( $T_{{\rm eff}}$ ) + $\sigma_{\rm abn}^2$ ( $\ensuremath{\log~g}$ ) + $\sigma_{\rm abn}^2$ ( $\upsilon_{{\rm mic}}$ ).

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