The properties of the kinematically distinct components in NGC 448 and
  NGC 4365
  Aims. We study the kinematically distinct components in two early-type
galaxies NGC 448 and NGC 4365 aided by integral-field observations with the
Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope. We aim to
measure the brightness profiles, kinematics, and stellar population properties
of the peculiar kinematic structures in these galaxies and shed light on their
true nature and formation mechanism.
  Methods. We use a kinematic decomposition technique to separate the
individual contributions to the spectra of the two distinct kinematic
components observed at each spatial position in the field of view. By folding
back the outcome of a photometric decomposition we reduce the intrinsic
degeneracies in recovering the kinematics and the best-fitting stellar spectral
templates. Finally, by extracting the Lick line-strength indices for the
individual components and fitting them to single stellar population models we
derive their ages, metallicities, and {\alpha}/Fe overabundances.
  Results. The two kinematically decoupled stellar components in NGC 448 have
similar ages, but different chemical compositions. The distinct kinematic
feature in NGC 448 has a nearly exponential surface-brightness light profile,
dominates in the innermost ~ 10", is smaller in size, and is very likely an
embedded counter-rotating disk as also indicated by its kinematics. It has
higher metallicity than the main galaxy stellar body and lower {\alpha}/Fe
overabundance. By contrast, we do not find evidence for true decoupling in the
two distinct kinematic components in NGC 4365. This confirms earlier work
suggesting that the kinematically distinct core is likely not a separate
dynamical structure, but most certainly likely a projection effect stemming
from the orbital structure of this galaxy that was previously found to be
intrinsically triaxial in shape.
