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Fig. B.1.


Galaxy-wide IMFs computed using IGIMF2 as a function of stellar mass plotted for several values of SFR (10−3, 1.0, 103M yr−1) and metallicity (−3, 0 2). The galaxy-wide IMFs are normalised by their values for 1 M to show the slope changes. We note the main difference between the IGIMF2 and IGIMF3 (Fig. 1) models is the variation for the low-mass part of the galaxy-wide IMF.

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