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Errors in the retrieved VMR profiles can result from the following: (I) The instrumental response function. This function was measured during the 1999-2000 cruise by cell measurements with a gas of known pressure, and the resulting instrumental line shape has been taken into account in the analysis. (ii) The assumed atmospheric pressure and temperature. These variables were measured daily on board the ship by balloon sondes during both cruises. (iii) Initial VMR profiles. Sensitivity tests (scaling the whole profile or shifting the profile with respect to altitude) gave similar results. (iv) The spectroscopic data: The most likely problems are the air-broadening half-widths and their temperature dependence. We analyzed spectra recorded with the same instrument in Spitsbergen in the high Arctic (79°N, 12°E, 20 m above sea level) and at Potsdam (S2°N, 80 m above sea level) in exactly the same way that we analyzed the cruise spectra. At both locations, the atmospheric temperatures show strong seasonal variabilities. The high-latitude VMR profiles derived yield relatively constant CO5 mixing ratios in the whole troposphere, in agreement with the available balloon observations, and do not indicate erroneous spectroscopic data. In addition to the spectroscopic remote-sensing observations, CO was also measured on board the ship during the 1999-2000 cruise by an in situ monitor, measuring the ultraviolet resonance fluorescence of CO at 150 nm (34). The instrument has an accuracy of ±1.3 ppbv and a detection limit of 3 ppbv (2σ) for an integration time of 1 s. The in situ and spectrometric data for the lower troposphere are in excellent agreement, confirming our spectroscopic observations.
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The backward trajectories were calculated on isentropic levels with HYSPLIT4 (HYbrid 5ingle-Particle Lagrangian Integrated Trajectory) Model, 1997 (www. arl.noaa.gov/ready/hysplit4.html); National Oceanic and Atmospheric Administration, Air Resources Laboratory, Silver Spring, MD.
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0242654147
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note
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We acknowledge the ATMOS team, who acquired and processed the shuttle spectra and made them available for analysis. We also thank the Polarstern crew for their assistance.
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