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We have compared the halo kinematics traced by globular clusters (GCs) andplanetary nebulae (PNe) for two elliptical galaxies in the Fornax and Virgoclusters NGC 1399 and NGC 4649, and for the merger remnant NGC 5128 (CentaurusA). We find differences in the rotational properties of the PN, red GC, andblue GC systems in all these three galaxies. NGC 1399 PNe and GCs show line ofsight velocity distributions in specific regions that are significantlydifferent, based on Kolmogorov-Smirnov tests. The PN system shows multi-spincomponents, with nearly opposite direction of rotation in the inner and theouter parts. The GCs velocity field is not point-symmetric in the outer regionsof the galaxy, indicating that the system has not reached dynamical equilibriumyet. In NGC 4649 PNe, red and blue GCs have different rotation axes androtational velocities. Finally, in NGC 5128 both PNe and GCs deviate fromequilibrium in the outer regions of the galaxy, and in the inner regions the PNsystem is rotationally supported, whereas the GC system is dominated byvelocity dispersion. The observed different kinematic properties, includingdeviations from point-symmetry, between PNe and GCs suggest that these systemsare accreted at different times by the host galaxy, and the most recentaccretion took place only few Gyr ago.We discuss two scenarios which mayexplain some of these differences: i) tidal stripping of loosely-bound GCs, andii) multiple accretion of low luminosity and dwarf galaxies. Because these twomechanisms affect mostly the GC system, differences with the PNe kinematics canbe expected.

Signatures of accretion events in the halos of early-type galaxies from comparing PNe and GCs kinematics