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Table A.1.

Observed line fluxes and modeled abundances.

Atomic species Line Fint S/N FX/FPaγ X/H [(X/H)]
[μm] [erg s−1 cm2]
H0 (Paγ) 1.09381 7.0 × 10−9 187
H0 (Paβ) 1.28181 2.0 × 10−8 1090.5 2.857 ± 0.016 log (nH) = 14.74 ± 0.02

C0 1.06831 3.8 × 10−10 18.3 0.0543 ± 0.0030 1.26 ± 0.54 × 10−2
N0 (blend) 1.04072 <2.5 × 10−10 <3 <0.0073 <2.35 × 10−1
O0 (blend) 0.84464 1.7 × 10−9 58.7 0.2429 ± 0.0043 3.27 ± 2.09 × 10−2
Na0 1.70311 <4.7 × 10−11 <3 <0.0067 <2.67 × 10−3
Mg0 1.71087 <4.7 × 10−11 <3 <0.0067 <1.12 × 10−4
Al0 1.67189 <1.1 × 10−10 <3 <0.0157 <1.68 × 10−1
Si0 1.58884 <9.8 × 10−11 <3 <0.0140 <1.83 × 10−4
S0 (blend) 1.04568 5.6 × 10−10 39.8 0.0800 ± 0.0021 8.70 ± 4.06 × 10−3
K0 1.51631 <4.7 × 10−11 <3 <0.0067 <6.33 × 10−3
Ca+1 0.86621 8.7 × 10−10 93.1 0.1240 ± 0.0015 1.39 ± 1.15 × 10−5
Fe+1 1.64355 <4.0 × 10−11 <3 <0.0057 <2.72 × 10−2

Notes. The uncertainties on the modeled abundances are dominated by a systematic 20% uncertainty on the synthetic line fluxes, which results from a factor of ∼2−4 uncertainty on the charge exchange rate coefficients, as is discussed in Sect. 3.3.4 of Hazy, the Cloudy users’ manual. Abundances are with respect to the Asplund et al. (2009) solar values.

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