  Detailed studies of the photometric and kinematical properties of compact
groups of galaxies are crucial to understand the physics of galaxy interactions
and to shed light on some aspects of galaxy formation and evolution. In this
paper we present a kinematical and photometrical study of a member, NGC4778, of
the nearest (z=0.0137) compact group: Hickson 62.
  Aims: The aim of this work was to investigate the existence of kinematical
anomalies in the brightest group member, NGC4778 in order to constrain the
dynamical status and the formation history of the group.
  Methods: We used long-slit spectra obtained with FORS1 at VLT, to measure
line-of-sight velocity distributions by means of the Fourier Correlation
Quotient method, and to derive the galaxy rotation curve and velocity
dispersion profile.
  Results: Our analysis reveals that Hickson 62a, also known as NGC4778, is an
S0 galaxy with kinematical and morphological peculiarities, both in its central
regions (r < 5'') and in the outer halo. In the central regions, the rotation
curve shows the existence of a kinematically decoupled stellar component,
offset with respect to the photometric center. In the outer halo we find an
asymmetric rotation curve and a velocity dispersion profile showing a rise on
the SW side, in direction of the galaxy NGC4776.
  Conclusions: The nuclear counterrotation, the distorted kinematics in the
outer halo and the X-ray properties of the group suggest that NGC4778 may be
the product of a recent minor merger, more reliable with a small late-type
galaxy.
