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Fig. 9

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Bisectors of the FeI lines used in Löhner-Böttcher et al. (2019) and fitted model to account for the CB. Left: bisectors from the quiet Kitt Peak solar spectrum. Right: bisectors from the active Kitt Peak solar spectrum. We rejected the bottom part of the 6301.5008 Å bisector because it was significantly off by 2500 m s−1 due to strong contamination by other weak lines.

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