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Galaxy evolution can be studied observationally by linking progenitor anddescendant galaxies through an evolving cumulative number density selection.This procedure can reproduce the expected evolution of the median stellar massfrom abundance matching. However, models predict an increasing scatter in mainprogenitor masses at higher redshifts, which makes galaxy selection at themedian mass unrepresentative. Consequently, there is no guarantee that theevolution of other galaxy properties deduced from this selection are reliable.Despite this concern, we show that this procedure approximately reproduces theevolution of the average stellar density profile of main progenitors of M =10^11.5 Msun galaxies, when applied to the EAGLE hydrodynamical simulation. Atz > 3.5 the aperture masses disagree by about a factor two, but thisdiscrepancy disappears when we include the expected scatter in cumulativenumber densities. The evolution of the average density profile in EAGLE broadlyagrees with observations from UltraVISTA and CANDELS, suggesting an inside-outgrowth history for these massive galaxies over 0 < z < 5. However, for z < 2the inside-out growth trend is stronger in EAGLE. We conclude that cumulativenumber density matching gives reasonably accurate results when applied to theevolution of the mean density profile of massive galaxies.

The average structural evolution of massive galaxies can be reliably estimated using cumulative galaxy number densities