Fig. A.1.
Observed solar spectrum from HARPS around each Mg I spectral line. The abundance estimation window is delimited by blue vertical lines (ΔλAbund ∼ 0.5 Å for non-saturated lines and ΔλAbund ∼ 2.5 Å for strong saturated ones). The different local normalisation intervals applied in the analysis are shown with red dashed vertical lines. Left: non-saturated lines: 4730.04, 5711.09, 6318.7, 6319.24, and 6319.49 Å. Right: strong saturated lines: 5167.3, 5172.7, 5183.6, and 5528.4 Å (from top to bottom).
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