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Fig. A.16


Top panels: FEROS or UVES Ca ii K (3933 Å) and Na i D1 (5889 Å) profiles towards Galactic and Magellenic stars, showing the observed spectrum in the LSR, Voigt model fit and data-model residual. Bottom panel: corresponding H i data from the GASS (black line) and LABS (dotted red line) surveys.

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