Context : 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 ] \lambda \lambda 4959 , 5007 and H \beta 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 ^ { \prime \prime } , the emission lines show multi-peaked profiles . The disk dominated region of the galaxy , 13 ^ { \prime \prime } < r < 30 ^ { \prime \prime } , exhibits regular rotation , with a flat rotation curve that reaches 248 \pm 6 km s ^ { -1 } . From this we estimate the total barionic mass to be M _ { bar } \sim 1.9 \cdot 10 ^ { 11 } M _ { \odot } and the total DM halo mass to be M _ { DM } \sim 4.8 \cdot 10 ^ { 12 } M _ { \odot } . The stellar velocity and velocity dispersion have been measured only in the innermost \approx 5 ^ { \prime \prime } of the bulge , and reveal a regular rotation with an observed amplitude of 140 km s ^ { -1 } and a central dispersion of \sigma = 180 km s ^ { -1 } . Our simple Jeans modeling shows that dark matter is needed in the central 5 ^ { \prime \prime } to explain the kinematics of the bulge , for which we estimate a mass of \approx ( 7 \pm 3 ) \cdot 10 ^ { 10 } M _ { \odot } . 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 . Conclusions :