  Characterizing the Martian atmosphere is an essential objective to understand
its meteorology and its climate. The lower atmosphere (< 40 km) and middle
atmosphere (40-80 km) of Mars appear dynamically coupled at much higher levels
than in the case of the Earth. The vertical extension of the weather phenomena
is considerable with for example Hadley's cells reaching the top of the neutral
atmosphere (120 km). The circulation in the middle atmosphere modifies the
meteorology of the lower atmosphere, affecting the transport and climatic
processes Observations of the CO rotational lines at millimeter (mm)
wavelengths (Clancy et al 1990) have strongly contributed in the study of the
vertical distribution of this compound and the thermal profile in the
atmosphere of Mars over 0-70 km. Singledish observations of the CO Doppler
lineshift have allowed direct wind measurements in the martian middle
atmosphere near 50 km altitude (Lellouch et al 1991), but at a low spatial
resolution (12'') enabling only an essentially hemispheric resolution of the
martian disk. The use of mm interferometry has allowed us to better spatially
resolve the Martian disk, in order to obtain wind maps of the middle atmosphere
(Moreno et al 2001).
