The globular cluster system of NGC1316. III. Kinematic complexity
  The merger remnant NGC 1316 (Fornax A) is one of the most important objects
regarding the investigation of merger-related processes. We use kinematical
data of globular clusters (GCs) and the diffuse stellar light to investigate
the global structure of NGC 1316 and to constrain the dark matter content. We
perform multi-object-spectroscopy with VLT/FORS2 and MXU. Out of 562 slits, we
extract radial velocities for 177 GCs. Moreover, we measure radial velocities
of the integrated galaxy light, using slits with a sufficiently bright "sky".
To these data, we add 20 cluster velocities from Goudfrooij et al. (2001). In
an appendix, we identify new morphological features of NGC 1316 and its
companion galaxy NGC 1317. The GC sample based on radial velocities confirms
the colour peaks already found in our photometric study. The bright clusters,
which probably have their origin in a 2 Gyr-old starburst and younger star
formation events, avoid the systemic velocity. A Gaussian velocity distribution
is found only for clusters fainter than about m_R=22 mag. The velocity
distribution of clusters shows a pronounced peak at 1600 km/s. These clusters
populate a wide area in the south-western region which we suspect to be a disk
population. Globular clusters or subsamples of them do not show a clear
rotation signal. This is different from the galaxy light, where rotation along
the major axis is discernable out to 3 arcmin radius. A simple spherical model
like that suggested by dynamical analyses of planetary nebulae reproduces also
the velocity dispersions of the faint GCs. The central dark matter density of
the present model resembles a giant elliptical galaxy. This contradicts
population properties which indicate spiral galaxies as pre-merger components.
MOND would provide a solution, but the kinematical complexity of NGC 1316 does
not allow a really firm conclusion. (abridged)
