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Fig. 10


EW([O iii]+Hβ) vs. redshift for different studies that empirically derived EW from the photometry (Shim et al. 2011; Labbé et al. 2013; Stark et al. 2013; Smit et al. 2014; Faisst et al. 2016; Mármol-Queraltó et al. 2016; Rasappu et al. 2016; Castellano et al. 2017) and the results obtained for the three SFHs used in the present work (rising, constant, and declining) assuming an SMC attenuation curve (alternative curves do not affect the results) and BC03 templates. We also show the result using BPASS templates (Sect. 4.4). For the studies deriving EW(Hα), we assume the typical ratio between this line and [O iii]+Hβ from Anders & Fritze-v. Alvensleben (2003) for a metallicity Z = 0.2 Z. We show the relation between EW and redshift derived in Fumagalli et al. (2012), extrapolated to high redshift and for two different stellar masses (Smit et al. 2014).

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