This might favor a sequence of several minor mergers, where, if the merger orbits are random, each new merger would tend to wash out the rotation signal left over from the previous merger. The stochastic behavior of possible multiple black hole systems, formed as a consequence of successive minor mergers, might further reduce core rotation in real galaxies. Constraints from galaxy scaling relations, however, limit the mass ratios of precursor galaxies as well [@KormendyBender13]. To put more quantitative constraints on the detailed formation histories of core galaxies, we need (1) numerical simulations that explore a wider range of initial conditions and (2) discussion of stellar population properties (something we plan for a forthcoming paper).

Non-core Galaxies
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The five non-core galaxies of our sample are not consistent with simple models of an adiabatic black hole growth into an originally isotropic stellar distribution: the relative overpopulation of tangential orbits with stars is stronger and spread over a spatially more extended region than expected from these models.

They are, however, compatible with the idea that these galaxies form in gas-rich mergers, where any pre-existing core is “refilled” by gas that falls in during/after the merger, settles into a rotating configuration, and then 