  Aims:We have studied the bulge and the disk kinematics of the giant low
surface brightness galaxy ESO 323-G064 in order to investigate its dynamical
properties and the radial mass profile of the dark matter (DM) halo.
  Methods:We observed the galaxy with integral field spectroscopy (VLT/VIMOS,
in IFU configuration), measured the positions of the ionized gas by fitting
Gaussian functions to the O[III] and Hbeta emission lines, and fit stellar
templates to the galaxy spectra to determine velocity and velocity dispersions.
We modeled the stellar kinematics in the bulge with spherical isotropic Jeans
models and explored the implications of self consistent and dark matter
scenarios for NFW and pseudo isothermal halos.
  Results:In the bulge-dominated region, r<5", the emission lines show
multi-peaked profiles. The disk dominated region of the galaxy, 13"<r<30",
exhibits regular rotation, with a flat rotation curve that reaches 248 +/- 6
km/sec. From this we estimate the total barionic mass to be M_bar ~ 1.9 10^11
M_sun and the total DM halo mass to be M_DM ~ 4.8 10^12 M_sun. The stellar
velocity and velocity dispersion have been measured only in the innermost ~5"
of the bulge, and reveal a regular rotation with an observed amplitude of 140
km/sec and a central dispersion of sigma=180 km/sec. Our simple Jeans modeling
shows that dark matter is needed in the central 5" to explain the kinematics of
the bulge, for which we estimate a mass of (7 +/- 3) 10^10 M_sun. However, we
are not able to disentangle different DM scenarios. The computed central mass
density of the bulge of ESO 323-G064 resembles the central mass density of some
high surface brightness galaxies, rather than that of low surface brightness
galaxies.
