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Cumulative number density matching of galaxies is a method to observationallyconnect descendent galaxies to their typical main progenitors at higherredshifts and thereby to assess the evolution of galaxy properties. Theaccuracy of this method is limited due to galaxy merging and scatter in thestellar mass growth history of individual galaxies. Behroozi et al. (2013) haveintroduced a refinement of the method, based on abundance matching of observedgalaxies to the Bolshoi dark-matter-only simulation. The EAGLE cosmologicalhydro-simulation is well suited to test this method, because it reproduces theobserved evolution of the galaxy stellar mass function and the passivefraction. We find agreement with the Behroozi et al. (2013) method for thecomplete sample of main progenitors of z = 0 galaxies, but we also find astrong dependence on the current star formation rate. Passive galaxies with astellar mass up to 10^10.75 Msun have a completely different median masshistory than active galaxies of the same mass. This difference persists if weonly select central galaxies. This means that the cumulative number densitymethod should be applied separately to active and passive galaxies. Even then,the typical main progenitor of a z = 0 galaxy already spans two orders ofmagnitude in stellar mass at z = 2.

A large difference in the progenitor masses of active and passive galaxies in the EAGLE simulation