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Fig. 6.


Ratio of the fraction of stars forming at low metallicity (ZO/H <  ZO/H⊙) in different mass ranges using the environment-dependent IMF to that using the universal IMF, as a function of redshift. The shaded area spans between the ratios obtained for the low- (solid lines) and high-metallicity (dashed lines) extreme fSFR(Z, z) distributions from ChN19. Thus, at redshift z = 1, about 2.5 times more stars with M* <  1 M form in the considered non-universal IMF scenario than in the universal IMF case.

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