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Fig. A.1
Theoretical [S I]/[S II] flux ratios vs. xe obtained assuming S = S I + S II + S III. Noticeably, both the [S I] lines are predicted to be brighter than the [S II]1032 line in the range of Te and ne that we fit (see Sect. 4). The horizontal line is the typical 3σ upper limit measured on our objects.
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