Using eight dark matter haloes extracted from fully-self consistent cosmological N -body simulations , we perform microlensing experiments .
A hypothetical observer is placed at a distance of 8.5 kpc from the centre of the halo measuring optical depths , event durations and event rates towards the direction of the Large Magellanic Cloud .
We simulate 1600 microlensing experiments for each halo .
Assuming that the whole halo consists of MACHOs , f = 1.0 , and a single MACHO mass is m _ { M } = 1.0 { M _ { \odot } } , the simulations yield mean values of \tau = 4.7 ^ { +5.0 } _ { -2.2 } \times 10 ^ { -7 } and \Gamma = 1.6 ^ { +1.3 } _ { -0.6 } \times 10 ^ { -6 } events star ^ { -1 } yr ^ { -1 } .
We find that triaxiality and substructure can have major effects on the measured values so that \tau and \Gamma values of up to three times the mean can be found .
If we fit our values of \tau and \Gamma to the MACHO collaboration observations ( 1 ) , we find f = 0.23 ^ { +0.15 } _ { -0.13 } and m _ { M } = 0.44 ^ { +0.24 } _ { -0.16 } .
Five out of the eight haloes under investigation produce f and m _ { M } values mainly concentrated within these bounds .