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Fig. 6


Upper panels: as in Fig. 4, but here, the color code indicates different wind parameters λ of the galaxies that reproduce the MZ relations. Lower panels: distribution of the predicted passive galaxies (red histogram) and star-forming galaxies (blue histogram) that reproduced the MZ relation in terms of the wind parameter λ of galaxies. In the left panel we adopt a Chabrier (2003) IMF, whereas in the right panel a Salpeter (1955) IMF is adopted.

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