Table 2: Elemental abundances of Balloon 090100001. Average values with standard deviations are given, if more than one line was fitted. Single line measurements are given without errors. Upper limits are only given, if they constrain the abundances in a reasonable way. $\log~\epsilon=12-\log(n(M)/n(H))$. [M/H] abundances relative to solar values are taken from Grevesse & Sauval (1998). The abundances of the comparison star Feige 48 are derived from optical spectra using mostly the same line data as well as line lists, and are taken from Heber et al. (2000).
        Feige 48
Ion $N_{\rm lines}$ $\log~\epsilon$ [M/H] $\log~\epsilon$
C  II 2 6.60 $\pm$ 0.14 -1.92  
C  III 1 7.10 -1.42 7.36 $\pm$ 0.03
N  II 11 7.55 $\pm$ 0.12 -0.37 7.47 $\pm$ 0.17
N  III   <7.90 <-0.02 7.80 $\pm$ 0.11
O  II 10 7.78 $\pm$ 0.08 -1.05 7.79 $\pm$ 0.12
Mg  II 1 6.80 -0.78 6.91
Al  III   <5.66 <-0.81 5.50 $\pm$ 0.18
Si  III 3 6.83 $\pm$ 0.15 -0.72 6.39 $\pm$ 0.32
Si  IV   <6.98 <-0.57 6.17
P  III   <4.94 <-0.51  
S  II   <6.50 <-0.83  
S  III 1 6.60 -0.73 6.15
Ar  II   <6.80 <0.40  
Ti  III   <5.68 <0.66  
Fe  III 8 7.38 $\pm$ 0.23 -0.12 7.55 $\pm$ 0.19


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