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  author = {{Farmer}, C.~B. and {Raper}, O.~F. and {Robbins}, B.~D. and 
	{Toth}, R.~A. and {Muller}, C.},
  title = {{Simultaneous spectroscopic measurements of stratospheric species: O$_{3}$, CH$_{4}$, CO, CO$_{2}$, N$_{2}$O, H$_{2}$O, HCl, and HF at northern and southern mid-latitudes}},
  journal = {\jgr},
  year = 1980,
  volume = 85,
  pages = {1621-1632},
  abstract = {{Near-infrared solar absorption spectra have been recorded in the course
of balloon flights from Palestine, Texas, (32{\deg}N latitude) in May
1976, and Broken Hill, Australia, (30{\deg}S latitude) in March 1977. The
northern flight was made at a float altitude of 37 km and covered the
spectral region from 1800 cm$^{-1}$ to 3600 cm$^{-1}$, which
encompasses infrared transitions of O$_{3}$, CH$_{4}$, CO,
CO$_{2}$, N$_{2}$O, H$_{2}$O and HCl. The flight in
the southern hemisphere, from a float altitude of 39km, covered the
spectra region from 2800 cm$^{-1}$ to 4500 cm$^{-1}$, which
includes useful transitions for all of the above gases (with the
exception of CO) and encompasses as well the 1-0 fundamental band for
HF. Both sets of spectra were acquired at sunset by using a
high-resolution (0.13 cm$^{-1}$) Michelson interferometer. The
simultaneous profiles of concentration derived from the spectra for the
individual gases covered in each flight are presented and discussed.
While the results show few differences between the profiles at the
northern and southern latitudes, there are several aspects of general
importance; these include lower values for stratospheric CO than had
previously been reported (i.e., \~{}10 ppbv), and water vapor profiles in
both hemispheres showing an increase with altitude considerably in
excess of that to be expected from CH$_{4}$ oxidation alone. The
shape of the profile for HF was found to be consistent with model
predictions, but the HF concentrations were lower by a factor of 3 or 4
than those predicted.
  doi = {10.1029/JC085iC03p01621},
  adsurl = {https://ui.adsabs.harvard.edu/abs/1980JGR....85.1621F},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}