  In this work we build a detailed dynamic model for a S0 galaxy possibly
hosting a central massive dark object (MDO). We show that the photometric
profiles and the kinematics along the major and minor axes, including the h3
and h4 profiles, imply the presence of a central MDO of mass M = 1.5 - 9.7 10^8
solar masses, i.e. 0.3-2.8% of the mass derived for the stellar spheroidal
component. Models without MDO are unable to reproduce the kinematic properties
of the inner stars and of the rapidly rotating nuclear gas.
  The stellar population comprise of an exponential disc (27% of the light) and
a diffuse spheroidal component (73% of the light) that cannot be represented by
a simple de Vaucouleurs profile at any radius. The M/L ratios we found for the
stellar components (respectively 3.3 and 6.6) are typical of those of disc and
elliptical galaxies.
