2003/12/18 by Th. Encrenaz, E. Lellouch, P. Drossart +3 · 1 citation
Physics and Astronomy · Earth and Planetary Sciences · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Physics #Uranus #Astrophysics #Emission spectrum #Tropopause #Mixing ratio #Spectral line #Astronomy #Troposphere #Atmospheric sciences
paper · pdf · doi:10.1051/0004-6361:20034637
openalex publication_date 2003/12/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
The spectrum of Uranus has been recorded in Oct.–Nov. 2002, between 4.6 and 5.0 μm, using the ISAAC imaging spectrometer at the VLT-UT1 (ANTU) 8-m telescope of ESO. The spectral resolving power was 1500. In addition to a few strong H3+ emission lines, the spectrum of Uranus distinctly shows the emission lines of the CO(1–0) band from R7 to P8. The relative intensity distribution of the observed CO emission is not compatible with a thermal distribution, for any value of the rotational temperature. The most likely emission mechanism is fluorescence, and a good fit is obtained assuming a constant CO mixing ratio of at the tropopause and above. The tropospheric continuum of Uranus is also detected beween 4.7 and 5.0 μm. The observed continuum can be fitted assuming reflected sunlight above a cloud level at 3.1 bars, presumably attributed to H2S. Upper limits of and are inferred for the CO and PH3 tropospheric mixing ratios above this level. The low CO tropospheric upper limit might suggest that the CO vertical distribution is not uniform.