In this laboratory investigation, Mars dust analogues have been mobilized by wind flow under Martian conditions of low density CO₂. Various laser based techniques have been employed to quantify dust mobilization and suspension; these include 2D laser Doppler velocimetry, optical opacity and optical reflectance. Direct mobilization of dust has been observed with a threshold shear stress as low as around 0.036 ​± ​0.007 ​Pa though only for dust layers of >1 monolayer and at a flux as high as 220 ​± ​100 ​mg/m²/s at around 20% above threshold. The dust resuspension fluxes for this direct process have been measured to be significantly lower (order of magnitude) than the mobilization rate, typically around 10 ​mg/m²/s at a shear stress of 0.15 ​Pa. This mechanism involved the removal, transport and breakup of dust aggregates. In another mechanism, saltating sand was seen to remobilize deposited dust layers <1 monolayer at a similar mobilization flux of around 50 ​± ​20 ​mg/m²/s and with a threshold of around 0.08 ​± ​0.008 ​Pa. At the high wind speeds used in these studies a significant fraction of the saltating sand grains become transported at relatively high elevation (>10 ​cm) and to high velocity. These essentially suspended grains were seen to generate a large flux of dust through impact abrasion. This constitutes a potential mechanism for dust generation on Mars, though is beyond the scope of this study to isolate and investigate.