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Fig. 3.


Intensity spectrum of the solar centre around the S I triplet at 1045 nm and the moved S I line. No further adjustments to the line strengths in the line lists from VALD have been made. Solar abundances (Grevesse et al. 2007) are assumed, and the log gf values of the S I lines are those that are listed in NIST, i.e. Zerne et al. (1997) and Zatsarinny & Bartschat (2006). The Fe I and Si I lines obviously have incorrect log gf values and can be adjusted to solar astrophysical values if required.

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