  I have combined the Emsellem et al. ATLAS3D rotation measures of a large
sample of early-type galaxies with HST-based classifications of their central
structure to characterize the rotation velocities of galaxies with cores. "Core
galaxies" rotate slowly, while "power-law galaxies" (galaxies that lack cores)
rotate rapidly, confirming the analysis of Faber et al. Significantly, the
amplitude of rotation sharply discriminates between the two types in the -19 >
Mv > -22 domain over which the two types coexist. The slow rotation in the
small set of core galaxies with Mv > -20, in particular, brings them into
concordance with the more massive core galaxies. The ATLAS3D "fast-rotating"
and "slow-rotating" early-type galaxies are essentially the same as power-law
and core galaxies, respectively, or the Kormendy & Bender two families of
elliptical galaxies based on rotation, isophote shape, and central structure.
The ATLAS3D fast rotators do include roughly half of the core galaxies, but
their rotation-amplitudes are always at the lower boundary of that subset.
Essentially all core galaxies have ATLAS3D rotation-amplitudes lambda_(R_e/2)
<= 0.25, while all galaxies with lambda_(R_e/2) > 0.25 and figure eccentricity
> 0.2 lack cores. Both figure rotation and the central structure of early-type
galaxies should be used together to separate systems that appear to have formed
from "wet" versus "dry" mergers.
