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The time evolution of atmospheric dust at high southern latitudes on Mars hasbeen determined using observations of the south seasonal cap acquired in thenear infrared (1-2.65 {\mu}m) by OMEGA/Mars Express in 2005. Observations atdifferent solar zenith angles and one EPF sequence demonstrate that thereflectance in the 2.64 {\mu}m saturated absorption band of the surface CO2 iceis mainly due to the light scattered by aerosols above most places of theseasonal cap. We have mapped the total optical depth of dust aerosols in thenear-IR above the south seasonal cap of Mars from mid-spring to early summerwith a time resolution ranging from one day to one week and a spatialresolution of a few kilometers. The optical depth above the south perennial capis determined on a longer time range covering southern spring and summer. Aconstant set of optical properties of dust aerosols is consistent with OMEGAobservations during the analyzed period. Strong variations of the optical depthare observed over small horizontal and temporal scales, corresponding in partto moving dust clouds. The late summer peak in dust opacity observed byOpportunity in 2005 propagated to the south pole contrarily to that observed inmid spring. This may be linked to evidence for dust scavenging by waterice-rich clouds circulating at high southern latitudes at this season.

Dust aerosols above the south polar cap of Mars as seen by OMEGA