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Table 2.

Atmospheric parameters and elemental abundances.

Teff log(g) v sin(i) ξ log(n(x))
(K) (cgs) (km s−1) He C N O Ne Mg Al Si S Ar Ca Fe
Value 15 840 4.86 18.4 (a) 2.0 −2.13 ≤ − 5.66 ≤ − 4.69 ≤ − 5.36 ≤ − 5.97 −5.71 ≤ − 7.08 ≤ − 7.00 ≤ − 6.60 ≤ − 5.75 −6.38 (b) −3.69
Stat. ... ... ... ... ... ... ... ...
Sys. ... ... ... ... ... ... ... ...
⊙ (c) −1.06 −3.57 −4.17 −3.31 −4.07 −4.40 −5.55 −4.49 −4.88 −5.60 −5.66 −4.50
Value −1.54 ≤ − 4.60 ≤ − 3.57 ≤ − 4.18 ≤ − 4.69 −4.34 ≤ − 5.67 ≤ − 5.57 ≤ − 5.11 ≤ − 4.17 −4.80 (b) −1.96
Stat. ... ... ... ... ... ... ... ...
Sys. ... ... ... ... ... ... ... ...
⊙ (c) −0.57 −2.60 −3.13 −2.22 −2.87 −3.12 −4.23 −3.15 −3.48 −4.11 −4.17 −2.86

Notes. The abundance n(x) is given either as a fractional particle number (upper four rows) or a mass fraction (lower four rows) of species x with respect to all elements. Statistical uncertainties (“Stat.”) are 1σ confidence limits based on χ2 statistics. Systematic uncertainties (“Sys.”) cover only the effects induced by additional variations of 1% in Teff and 0.04 in log(g) and are formally taken to be 1σ confidence limits (see Irrgang et al. 2014 for details). Abundances without uncertainties are upper limits because the respective chemical elements do not exhibit spectral lines that are strong enough to be measured.

(a)

Affected by orbital smearing and thus overestimated (see Sect. 2.4).

(b)

Abundance based on population numbers computed in LTE.

(c)

Proto-solar nebula values from Asplund et al. (2009) as reference.

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