We present the first entirely ground-based astrometric determination of the proper motion for the Fornax Local Group Dwarf Spheroidal satellite galaxy of the Milky Way , using CCD data acquired with the ESO 3.5 m NTT telescope at La Silla Observatory in Chile .
Our unweighted mean from five Quasar fields in the background of Fornax , used as fiducial reference points , leads to \mu _ { \alpha } \cos \delta = 0.62 \pm 0.16 mas y ^ { -1 } , and \mu _ { \delta } = -0.53 \pm 0.15 mas y ^ { -1 } .
A detailed comparison with all previous measurements of this quantity seems to imply that there is still no convincing convergence to a single value , perhaps indicating the existence of unnacounted systematic effects in ( some of ) these measurements .
From all available proper motion and radial velocity measurements for Fornax , we compute Fornax ’ s orbital parameters and their uncertainty using a realistic Galactic potential and a Monte Carlo simulation .
Properties of the derived orbits are then compared to main star formation episodes in the history of Fornax .

All published proper motion values imply that Fornax has recently ( 200-300 Myr ago ) approached perigalacticon at a distance of \sim 150 kpc .
However , the derived period exhibits a large scatter , as does the apogalacticon .
Our orbit , being the most energetic , implies a very large apogalactic distance of \sim 950 kpc .
If this were the case , then Fornax would be a representative of an hypervelocity MW satellite in late infall .