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Table 3

Detailed abundances.

Ion A(X)⊙ N A(X) [X/H] σ [X/Fe] σ N A(X) [X/H] σ [X/Fe] σ
J113613-105227 J113615-105244
Na i 6.30 2 4.35 −1.95 0.20 −0.22 0.36 2 4.35 −1.95 0.20 −0.28 0.36
Mg i 7.54 2 6.12 −1.42 0.03 0.31 0.26 2 6.22 −1.32 0.42 0.35 0.51
Ca i 6.33 4 4.96 −1.37 0.23 0.36 0.35 4 5.10 −1.23 0.11 0.44 0.30
Ti ii 4.90 3 3.36 −1.54 0.19 0.19 0.20 2 3.21 −1.69 0.20 −0.02 0.34
V i 4.00 1 2.11 −1.89 −0.16 1 2.23 −1.77 −0.10
Cr ii 5.64 2 3.82 −1.82 0.03 −0.09 0.26 1 4.40 −1.24 0.43
Mn i 5.37 2 3.74 −1.63 0.09 0.10 0.28
Fe i 7.52 58 5.79 −1.73 0.26 0.00 32 5.85 −1.67 0.28 0.00
Fe ii 7.52 2 5.67 −1.85 0.05 0.00 1 5.97 −1.55 0.00
Ni i 6.23 2 4.55 −1.68 0.18 0.05 0.31 1 4.62 −1.61 0.05
Ba ii 2.17 1 0.49 −1.68 −0.01 2 0.43 −1.74 0.20 −0.07 0.34

Notes. For elements for which several lines are measured, the quoted error is the line-to-line scatter, except for Na i. For Crater J113613-105227 the two lines of the doublet where fitted together, and for Crater J113615-105244 only the D2 line was fitted. The quoted errors are estimated from the goodness-of-fit. For the elements for which only one line was measured, we provide no estimate of the error, but recommend to take the error estimate provided for Fe i, since for both stars this is the element with the largest number of measured lines, and the line-to-line scatter can be interpreted as mainly due to the noise in the spectrum.

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