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Volume 16, issue 8
Atmos. Chem. Phys., 16, 5021–5042, 2016
https://doi.org/10.5194/acp-16-5021-2016
© Author(s) 2016. This work is distributed under
the Creative Commons Attribution 3.0 License.
Atmos. Chem. Phys., 16, 5021–5042, 2016
https://doi.org/10.5194/acp-16-5021-2016
© Author(s) 2016. This work is distributed under
the Creative Commons Attribution 3.0 License.

Research article 22 Apr 2016

Research article | 22 Apr 2016

Comparison of VLT/X-shooter OH and O2 rotational temperatures with consideration of TIMED/SABER emission and temperature profiles

Stefan Noll1, Wolfgang Kausch2,1, Stefan Kimeswenger3,1, Stefanie Unterguggenberger1, and Amy M. Jones4 Stefan Noll et al.
  • 1Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria
  • 2Department of Astrophysics, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
  • 3Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile
  • 4Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany

Abstract. Rotational temperatures Trot derived from lines of the same OH band are an important method to study the dynamics and long-term trends in the mesopause region near 87 km. To measure realistic temperatures, the rotational level populations have to be in local thermodynamic equilibrium (LTE). However, this might not be fulfilled, especially at high emission altitudes. In order to quantify possible non-LTE contributions to the OH Trot as a function of the upper vibrational level v′, we studied a sample of 343 echelle spectra taken with the X-shooter spectrograph at the Very Large Telescope at Cerro Paranal in Chile. These data allowed us to analyse 25 OH bands in each spectrum. Moreover, we could measure lines of O2b(0-1), which peaks at about 94 to 95 km, and O2a(0-0) with an emission peak at about 90 km. The latter altitude is reached in the second half of the night after a rise of several km because of the decay of a daytime population of excited O2. Since the radiative lifetimes for the upper levels of the two O2 bands are relatively long, the derived Trot are not significantly affected by non-LTE contributions. These bands are well suited for a comparison with OH if the differences in the emission profiles are corrected. For different sample averages, we made these corrections by using OH emission, O2a(0-0) emission, and CO2-based temperature profile data from the multi-channel radiometer SABER on the TIMED satellite. The procedure relies on differences of profile-weighted SABER temperatures. For an O2a(0-0)-based reference profile at 90 km, we found a good agreement of the O2 with the SABER-related temperatures, whereas the OH temperatures, especially for the high and even v′, showed significant excesses with a maximum of more than 10 K for v′ = 8. The exact value depends on the selected lines and molecular parameters. We could also find a nocturnal trend towards higher non-LTE effects, particularly for high v′. The amplitude of these variations can be about 2 K or less, which tends to be significantly smaller than the total amount of the non-LTE contributions. The variations revealed may be important for dynamical studies based on Trot derived from OH bands with high v′.

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Short summary
We compare temperatures derived from simultaneous observations of 25 OH and two O2 mesospheric airglow bands taken with the X-shooter spectrograph at the Very Large Telescope in Chile. Considering emission and temperature profile data from the radiometer SABER on the TIMED satellite, we find significant time-dependent non-thermal contributions to the OH-based temperatures, especially for bands originating from high vibrational levels. Many studies of the mesopause region are affected.
We compare temperatures derived from simultaneous observations of 25 OH and two O2 mesospheric...
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