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Deep exposure imaging of early-type galaxies (ETGs) are revealing thesecond-order complexity of these objects, which have been long considereduniform, dispersion-supported spheroidals. "Fine structure" features (e.g.ripples, plumes, tidal tails, rings) as well as depleted stellar cores (i.e.central light deficits) characterize a number of massive ETG galaxies, and canbe interpreted as the result of galaxy-galaxy interactions. We discuss how thetimescale for the evolution of cores and fine structures are comparable, andhence it is expected that they develop in parallel after the major interactionevent which shaped the ETG. Using archival data, we compare the "depletedstellar mass" (i.e. the mass missing from the depleted stellar core) againstthe prominence of the fine structure features, and observe that they correlateinversely. This result confirms our expectation that, while the Super MassiveBlack Hole (SMBH) binary (constituted by the SMBHs of the merger progenitors)excavates the core via three-body interactions, the gravitational potential ofthe newborn galaxy relaxes, and the fine structures fade below detectionlevels. We expect the inverse correlation to hold at least within the first Gyrfrom the merger which created the SMBH binary; after then, the fine structureevolves independently.

Connecting traces of galaxy evolution: the missing core mass -- morphological fine structure relation