We re-investigate the Fornax cusp-core problem using observational results on the spatial and mass distributions of globular clusters ( GCs ) in order to put constraints on the dark matter profile .
We model Fornax using high resolution N-body simulations with entirely live systems , i.e .
self-gravitating systems composed of stars and dark matter , which account correctly for dynamical friction and tidal effects between Fornax and the globular clusters .
We test two alternative hypotheses , which are a cored and a cuspy halo for Fornax by exploring a reasonable range of initial conditions on globular clusters .
For Fornax cored dark matter halo , we derive a lower limit on the core size of r _ { c } \gtrsim 0.5 kpc .
Contrary to many previous works , we show also that for different initial conditions , a cuspy halo is not ruled out in our simulations based on observations of Fornax globular clusters .