Fig. 5
Voigt-profile fits to the host-galaxy metal lines. We label the intervening metal lines (see Sect. 3.5) that contaminate the host galaxy lines; their contribution to the observed profile is taken into account. In orange (light grey) we show an atmospheric transmission spectrum matching the observing conditions and spectral resolution of our observations, generated with ESO’s SkyCalc tool. Residuals such as those close to the Fe ii lines are due to subtracted telluric emission lines.
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