Fig. 15
Top: βphot vs. log(EW[OII]) rest-frame. We use the convention of positive EW for emission lines. The right axis converts βphot to AIRX using Eq. (11). Black points represent IR-detected galaxies, while grey points represent galaxies with no IR detection. The blue dashed line is a linear fit to the points. Bottom: average spectra in two bins of rest-frame EW[OII]. Lines of interest are labelled.
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