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Home All issues Volume 503 / No 3 (September I 2009) A&A, 503 3 (2009) 945-962 Full HTML
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Table 4:

LTE atmospheric abundances in programme stars with the error estimates based on the internal scattering from the number of analysed lines, n.
Ion HD 145788 21 Peg $\pi $ Cet Sun (*)
  $\log (N/N_{\rm tot})$ n $\log (N/N_{\rm tot})$ n $\log (N/N_{\rm tot})$ n $\log (N/N_{\rm tot})$
He I   -1.10 $\pm$ 0.05 4   -1.09 $\pm$ 0.03 7   -0.97 $\pm$ 0.04 6   -1.12 
C I   -3.60 $\pm$ 0.14 5   -3.66 $\pm$ 0.14 9       -3.65 
C II   -3.63: 2   -3.65 $\pm$ 0.05 4   -3.58 $\pm$ 0.07 7   -3.65 
N I       -3.95 $\pm$ 0.12 4   -4.03 $\pm$ 0.13 10   -4.26 
N II       -3.90: 1   -3.74 $\pm$ 0.07 9   -4.26 
O I   -3.12 $\pm$ 0.09 7   -3.28 $\pm$ 0.11 18   -3.06 $\pm$ 0.14 9   -3.38 
O II           -3.04: 2   -3.38 
Ne I       -3.76 $\pm$ 0.05 7   -3.66 $\pm$ 0.09 20   -4.20 
Na I       -5.60: 1   -5.23 $\pm$ 0.07 3   -5.87 
Mg I   -4.17 $\pm$ 0.24 5   -4.42 $\pm$ 0.12 5   -4.27: 2   -4.51 
Mg II   -4.29 $\pm$ 0.06 4   -4.56 $\pm$ 0.03 7   -4.47 $\pm$ 0.16 10   -4.51 
Al I   -5.70: 2   -5.89: 2   -5.57: 2   -5.67 
Al II   -5.11 $\pm$ 0.10 3   -5.70 $\pm$ 0.10 4   -5.73 $\pm$ 0.27 8   -5.67 
Al III           -5.30 $\pm$ 0.02 3   -5.67 
Si I   -4.75: 1   -4.95: 1   -4.80: 1   -4.53 
Si II   -4.27 $\pm$ 0.14 11   -4.49 $\pm$ 0.13 22   -4.41 $\pm$ 0.20 31   -4.53 
Si III       -4.26 $\pm$ 0.18 2   -4.16: 2   -4.53 
P II       -6.37 $\pm$ 0.06 3   -6.38 $\pm$ 0.19 9   -6.68 
P III           -6.19: 1   -6.68 
S II   -4.36: 2   -4.86 $\pm$ 0.13 26   -4.78 $\pm$ 0.16 31   -4.90 
Cl II           -6.95: 2   -6.54 
Ar I           -4.86 $\pm$ 0.24: 2   -5.86 
Ar II           -5.24 $\pm$ 0.19 6   -5.86 
Ca I   -5.46 $\pm$ 0.11 5   -5.84 $\pm$ 0.11 3       -5.73 
Ca II   -5.54 $\pm$ 0.16 6   -5.98 $\pm$ 0.08 5   -5.77: 2   -5.73 
Sc II   -8.90 $\pm$ 0.03 5   -9.37 $\pm$ 0.10 7   -9.31: 1   -8.99 
Ti II   -6.80 $\pm$ 0.15 47   -7.23 $\pm$ 0.09 59   -7.42 $\pm$ 0.08 11   -7.14 
V II   -7.55 $\pm$ 0.20 4   -7.98 $\pm$ 0.06 9       -8.04 
Cr I   -6.15 $\pm$ 0.09 4   -6.29 $\pm$ 0.09 5       -6.40 
Cr II   -5.86 $\pm$ 0.11 31   -6.20 $\pm$ 0.10 68   -6.41 $\pm$ 0.10 21   -6.40 
Mn I   -6.43: 2   -6.54 $\pm$ 0.21 5       -6.65 
Mn II   -6.15 $\pm$ 0.08 4   -6.51 $\pm$ 0.17 19   -6.50 $\pm$ 0.09 3   -6.65 
Fe I   -4.23 $\pm$ 0.16 88   -4.52 $\pm$ 0.13 108   -4.53 $\pm$ 0.22 7   -4.59 
Fe II   -4.13 $\pm$ 0.15 147   -4.50 $\pm$ 0.12 406   -4.58 $\pm$ 0.14 186   -4.59 
Fe III       -4.60 $\pm$ 0.06 3   -4.52 $\pm$ 0.10 4   -4.59 
Co II       -6.75 $\pm$ 0.18 3   -6.93: 1   -7.12 
Ni I   -5.32 $\pm$ 0.13 8   -5.71 $\pm$ 0.05 10       -5.81 
Ni II   -5.12 $\pm$ 0.05 3   -5.61 $\pm$ 0.09 23   -5.76 $\pm$ 0.19 17   -5.81 
Zn I       -6.86: 1       -7.44 
Sr II   -8.45: 2   -9.10: 2   -9.15: 2   -9.12 
Y II   -9.06: 1   -9.76 $\pm$ 0.15 4       -9.83 
Zr II   -8.75 $\pm$ 0.32 3   -9.48 $\pm$ 0.28 4       -9.45 
Ba II   -8.96 $\pm$ 0.11 3   -9.19 $\pm$ 0.06 3       -9.87 
Nd III      -10.09 $\pm$ 0.07 3      -10.59 
$T_{{\rm eff}}$ 9750 K 10 400 K 12 800 K 5777 K
\ensuremath{\log~g} 3.7      3.55     3.75     4.44    
Internal scattering was not estimated when n<3, in which case the derived abundance if flagged with a colon (:). (*) The abundances of the solar atmosphere calculated by Asplund et al. (2005).

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