Table 3: Averaged absolute abundances (in the scale where $\log \epsilon$ (H) = 12) and normalized abundances [X/Fe] for HD 148897 (relative to the Sun; Grevesse & Sauval 1998). The standard deviations $\sigma$ and the number of lines used in the analysis (n) are also given. Two sets of abundances from Luck (1991) are given: one is based on a "photometric $\log g$ '' (derived from the absolute magnitude, the effective temperature and an estimate for the stellar mass) and the other on the "spectroscopic $\log g$ '' (Fe I/Fe II ionization balance).
This work Kiröläinen et al. (1986) Luck (1991) Luck (1991)

$T_{\rm eff}$ = 4350 K $T_{\rm eff}$ = 4360 K $T_{\rm eff}$ = 4100 K $T_{\rm eff}$ = 4100 K

$\log g = 1.0$ $\log g = 1.5$ phot. $\log g = 1.6$ spec. $\log g = 0.1$

$v_{\rm t} = 2.0$ km s^-1 $v_{\rm t} = 2.6$ km s^-1 $v_{\rm t} = 1.7$ km s^-1 $v_{\rm t} = 1.7$ km s^-1

X $\log \epsilon$ (X) $\sigma$ n [X/H] $_\odot$ $\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$ [X/H] $_\odot$ [X/Fe] $_\odot$ [X/H] $_\odot$ $\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$ [X/H] $_\odot$ $\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$

O I 8.22 0.20 4 -0.61 +0.41 -0.58 +0.04 -0.50 +0.50 -1.10 +0.06

Na I 5.10 0.08 6 -1.23 -0.21 -1.11 -0.49 -1.36 -0.36 -1.26 -0.10

Mg I 6.92 0.09 6 -0.66 +0.36 -0.59 +0.03 -0.54 +0.46 -0.62 +0.54

Al I 5.61 0.23 4 -0.86 +0.16 -0.70 -0.08 -1.28 -0.28 -1.20 -0.04

Si I 6.91 0.11 23 -0.77 +0.25 -0.56 +0.06 -0.24 +0.76 -0.59 +0.57

K I 4.17 1 -0.95 +0.07 - - - - - -

Ca I 5.65 0.11 21 -0.71 +0.31 -0.54 +0.08 -1.09 -0.09 -0.97 +0.19

Ca II 5.48 1 -0.88 +0.09 - - - - - -

Sc II 2.08 0.12 13 -1.09 -0.12 -0.86 -0.24 -0.75 -0.40 -1.37 -0.21

Ti I 4.20 0.07 56 -0.82 +0.20 -0.48 +0.14 -1.20 -0.20 -1.19 -0.03

Ti II 4.22 0.14 8 -0.80 +0.17 - - -0.51 -0.16 -1.16 0.00

V I 3.11 0.09 23 -0.89 +0.13 -0.56 +0.06 -1.24 -0.24 -1.24 -0.08

V II 3.01 1 -0.99 -0.02 - - - - - -

Cr I 4.59 0.12 27 -1.08 -0.06 -0.82 -0.20 -1.19 -0.19 -1.08 +0.08

Cr II 4.85 0.08 6 -0.82 +0.15 - - - - - -

Mn I 4.24 0.10 11 -1.15 -0.13 -1.00 -0.38 - - - -

Fe I 6.48 0.07 180 -1.02 - -0.62 - -1.00 - -1.16 -

Fe II 6.53 0.07 17 -0.97 - - - -0.35 - -1.16 -

Co I 4.11 0.12 21 -0.81 +0.21 -0.70 -0.08 -0.84 +0.16 -1.10 +0.06

Ni I 5.15 0.11 54 -1.10 -0.08 -0.62 0.00 -0.84 +0.16 -1.12 +0.04

Cu I 3.31 0.17 3 -0.90 +0.12 - - -0.64 +0.36 -0.80 +0.36

Zn I 3.78 1 -0.82 +0.20 - - -0.39 +0.61 -0.92 +0.24

Y II 1.21 0.12 6 -1.03 -0.06 -0.73 -0.11 -0.62 -0.27 -1.14 +0.02

Zr I -1.43 -0.43 -1.43 -0.27

Zr II 1.91 0.13 3 -0.69 +0.28 -0.37 +0.25 - - - -

Ba II 0.97 0.05 3 -1.16 -0.19 -0.66 -0.04 - - - -

La II 0.24 0.25 3 -0.93 +0.04 -0.52 +0.10 - - - -

Ce II
0.26 0.16 5 -1.32 -0.35 -0.65 -0.03 -0.68 -0.33 -1.21 -0.05

Pr II -0.20 0.13 2 -0.91 +0.06 - - - - - -

Nd II 0.56 0.13 8 -0.94 +0.03 - - -0.61 -0.26 -1.15 +0.01

Eu II 0.17 1 -0.34 +0.63 - - -0.40 -0.05 -1.01 +0.15

**Table 3:** Averaged absolute abundances (in the scale where $\log \epsilon$ (H) = 12) and normalized abundances [X/Fe] for HD 148897 (relative to the Sun; Grevesse & Sauval 1998). The standard deviations $\sigma$ and the number of lines used in the analysis (n) are also given. Two sets of abundances from Luck (1991) are given: one is based on a "photometric $\log g$ '' (derived from the absolute magnitude, the effective temperature and an estimate for the stellar mass) and the other on the "spectroscopic $\log g$ '' (Fe I/Fe II ionization balance).
	This work		Kiröläinen et al. (1986)	Luck (1991)	Luck (1991)
	$T_{\rm eff}$ = 4350 K		$T_{\rm eff}$ = 4360 K	$T_{\rm eff}$ = 4100 K	$T_{\rm eff}$ = 4100 K
	$\log g = 1.0$		$\log g = 1.5$	phot. $\log g = 1.6$	spec. $\log g = 0.1$
	$v_{\rm t} = 2.0$ km s^-1		$v_{\rm t} = 2.6$ km s^-1	$v_{\rm t} = 1.7$ km s^-1	$v_{\rm t} = 1.7$ km s^-1
X	$\log \epsilon$ (X)	$\sigma$	n	[X/H] $_\odot$	$\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$	[X/H] $_\odot$	[X/Fe] $_\odot$	[X/H] $_\odot$	$\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$	[X/H] $_\odot$	$\left[\frac{{X}_{{\rm I,II}}}{{\rm Fe}_{{\rm I,II}}}\right]_\odot$
O I	8.22	0.20	4	-0.61	+0.41	-0.58	+0.04	-0.50	+0.50	-1.10	+0.06
Na I	5.10	0.08	6	-1.23	-0.21	-1.11	-0.49	-1.36	-0.36	-1.26	-0.10
Mg I	6.92	0.09	6	-0.66	+0.36	-0.59	+0.03	-0.54	+0.46	-0.62	+0.54
Al I	5.61	0.23	4	-0.86	+0.16	-0.70	-0.08	-1.28	-0.28	-1.20	-0.04
Si I	6.91	0.11	23	-0.77	+0.25	-0.56	+0.06	-0.24	+0.76	-0.59	+0.57
K I	4.17		1	-0.95	+0.07	-	-	-	-	-	-
Ca I	5.65	0.11	21	-0.71	+0.31	-0.54	+0.08	-1.09	-0.09	-0.97	+0.19
Ca II	5.48		1	-0.88	+0.09	-	-	-	-	-	-
Sc II	2.08	0.12	13	-1.09	-0.12	-0.86	-0.24	-0.75	-0.40	-1.37	-0.21
Ti I	4.20	0.07	56	-0.82	+0.20	-0.48	+0.14	-1.20	-0.20	-1.19	-0.03
Ti II	4.22	0.14	8	-0.80	+0.17	-	-	-0.51	-0.16	-1.16	0.00
V I	3.11	0.09	23	-0.89	+0.13	-0.56	+0.06	-1.24	-0.24	-1.24	-0.08
V II	3.01		1	-0.99	-0.02	-	-	-	-	-	-
Cr I	4.59	0.12	27	-1.08	-0.06	-0.82	-0.20	-1.19	-0.19	-1.08	+0.08
Cr II	4.85	0.08	6	-0.82	+0.15	-	-	-	-	-	-
Mn I	4.24	0.10	11	-1.15	-0.13	-1.00	-0.38	-	-	-	-
Fe I	6.48	0.07	180	-1.02	-	-0.62	-	-1.00	-	-1.16	-
Fe II	6.53	0.07	17	-0.97	-	-	-	-0.35	-	-1.16	-
Co I	4.11	0.12	21	-0.81	+0.21	-0.70	-0.08	-0.84	+0.16	-1.10	+0.06
Ni I	5.15	0.11	54	-1.10	-0.08	-0.62	0.00	-0.84	+0.16	-1.12	+0.04
Cu I	3.31	0.17	3	-0.90	+0.12	-	-	-0.64	+0.36	-0.80	+0.36
Zn I	3.78		1	-0.82	+0.20	-	-	-0.39	+0.61	-0.92	+0.24
Y II	1.21	0.12	6	-1.03	-0.06	-0.73	-0.11	-0.62	-0.27	-1.14	+0.02
Zr I								-1.43	-0.43	-1.43	-0.27
Zr II	1.91	0.13	3	-0.69	+0.28	-0.37	+0.25	-	-	-	-
Ba II	0.97	0.05	3	-1.16	-0.19	-0.66	-0.04	-	-	-	-
La II	0.24	0.25	3	-0.93	+0.04	-0.52	+0.10	-	-	-	-
Ce II	0.26	0.16	5	-1.32	-0.35	-0.65	-0.03	-0.68	-0.33	-1.21	-0.05
Pr II	-0.20	0.13	2	-0.91	+0.06	-	-	-	-	-	-
Nd II	0.56	0.13	8	-0.94	+0.03	-	-	-0.61	-0.26	-1.15	+0.01
Eu II	0.17		1	-0.34	+0.63	-	-	-0.40	-0.05	-1.01	+0.15

Source LaTeX | All tables | In the text

	1 The problem
	2 The samples
	3 Abundances
	4 Statistics of binarity among metal-deficient Ba stars
	5 Summary of the binary criteria and discussion
	References
	Online Material