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Galaxy formation in the Planck cosmology II Star formation histories and post processing magnitude reconstruction

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Figure

Fig. 1).
Figure 2. The difference between photometric properties calculated using full resolution and binned SFHs at z = 0 (left) and z = 2 (right)
Figure 3. The average SFH from VESPA (black lines), the GWB11 model(magenta, dash–dotted lines) and the HWT14 model (dashed, green lines)within the indicated mass range
Figure 4. The average SFH from VESPA (black lines), the GWB11 model(magenta, dash–dotted lines) and the HWT14 model (dashed, green lines)within two different stellar mass bins, as shown
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