All Figures

	Figure 1: Geometry of the observations in a) 2001 and b) 2005. Positions of observed points are given in Tables 2 and 3. Their position on the disks are only approximative. The field of view (full width at half maximum of the beam) at 230 GHz is plotted in dashed lines for position 1. Celestial east/west directions.
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In the text

	Figure 2: Antenna temperature spectra of the 12CO(1-0) and (2-1) lines in 2001 for position 1 with the high spectral resolution mode. The absorption caused by terrestrial mesospheric CO can be seen at 1.5 MHz on the blue wing of the line center of the (1-0) line and 3 MHz on the blue wing of the line center of the (2-1) line.
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In the text

Figure 3: Contribution functions for the 12CO(2-1) line in 2005. From the highest peak to the lowest one, the frequencies at which the functions are computed are: 0, 0.5, 1, 2, 4, 6 and 10 MHz from the line center. These functions show that it is possible to retrieve the thermal profile between 15 and 70 km from the high resolution 12CO(2-1) line. The 12CO(1-0) line gives similar results. The gap from the surface to 15 km is filled in with the low resolution 12CO(2-1) spectrum because it gives access to the missing part of the spectrum, from 10 MHz from the line center to the continuum.

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In the text

	Figure 4: Contribution function for the central frequency of the 13CO(2-1) line in 2001.
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In the text

	Figure 5: 12CO(2-1) high resolution line in 2005 fitted with the best fit model (solid line). The dotted model corresponds to an increase of from to above 50 km (homopause level).
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In the text

	Figure 6: Relative comparison between the observed spectra of 2001 and MCD predictions (Warm scenario in solid lines, dust storm scenario in dotted lines and MY24 scenario in long-dashed lines) for: 12CO(1-0)  a) low and  b) high resolution, 12CO(2-1)  c) low and  d) high resolution, 13CO(2-1)  e) high resolution.
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In the text

	Figure 7: Same caption as Fig. 6 for 2005.
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In the text

	Figure 8: Mean atmospheric temperature profiles derived from the observations (solid lines) and the MCD predictions in 2001 and 2005. The temperature profile corresponding to the scenario 2 (MY24) and 7 (Warm) are in dashed and dotted lines, respectively.
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In the text

Figure 9: Best fit model for the 2001 dataset. The mean temperature profile derived from the observations is shown in Fig. 8. The 1-D surface temperature profile used is given in Eq. (10). The CO mixing ratio is . All spectra correspond to disk center observations. a) 12CO(2-1) line with 256 MHz bandwidth and a 1 MHz spectral resolution. b) Same line but with 128 MHz bandwidth and a 39 kHz spectral resolution. c) 12CO(1-0) line with the same parameters as  a). d) 12CO(1-0) line with the same parameters as  b). d) 13CO(2-1) line with a 78 kHz spectral resolution.

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In the text

	Figure 10: Same caption as Fig. 9 for the 2005 dataset. Mean temperature profile shown in Fig. 8b. The spectral resolution is 26.4 kHz for the  b), d) and  e) spectra.
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In the text

	Figure 11: 12CO(2-1) line computed with the MCD thermal profiles (black lines) taken from the  grid of 2005. The line is fitted with the mean thermal profile model (dashed lines).
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In the text

	Figure 12: Atmospheric temperature profile in 2005 derived from the observations (solid lines) and from Clancy et al. (2006) (dashed lines).
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In the text

	Figure 13: Contribution function of the 12CO(3-2) line at 0 and 6 MHz from the central frequency and contribution function of the 13CO(3-2) line at 0 MHz from the central frequency in 2005.
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In the text

	Figure 14: Atmospheric temperature profile in 2001 derived from the observations (solid lines) and measurements from Gurwell et al. (2005) (crosses).
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In the text

	Figure 15: 12CO(2-1) line cores in 2005 for five positions on the equator. Positions are: 90W, 30W, Central Meridian (CM), 30E and 90E and correspond to 6 pm, 2 pm, noon, 10 am and 6 am in local time.
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In the text

	Figure 16: LOS BI wind velocities for the a) 12CO(2-1) and  b) 13CO(2-1) observations in 2001. Celestial east/west directions. Parenthese: 1- fitting uncertainties. Additional uncertainty on each point: 20 m s-1 for 12CO(2-1) measurements and 30-40 m s-1 for 13CO(2-1) measurements.
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In the text

	Figure 17: LOS BI wind velocities for the a) 12CO(2-1) and  b) 13CO(2-1) observations in 2005. Celestial east/west directions. Parenthese: 1- fitting uncertainties. Additional uncertainty on each point: 20 m s-1 for 12CO(2-1) measurements and 30-40 m s-1 for 13CO(2-1) measurements.
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In the text

	Figure 18: Wind velocities predictions from the MCD MY24 scenario for a) the 12CO(2-1) and  b) the 13CO(2-1) in 2001. The numbers correspond to the velocities on the 13 points of the observed map. Celestial east/west directions.
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In the text

	Figure 19: Same caption as Fig. 18 for 2005. Celestial east/west directions. Taking a pointing error of 2 arcsec in the south-east direction into account would result in reducing the velocities of the western limb by 20 m s-1 and increasing the eastern limb velocities by 20 m s-1.
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In the text