Detection of the 267 GHz J = 1-0 rotational transition of PH3 in Saturn with a new fourier transfer spectrometer

Details Detection of the 267 GHz J = 1-0 rotational transition of PH3 in Saturn with a new fourier transfer spectrometer Detection of the 267 GHz J = 1-0 rotational transition of PH3 in Saturn with a new fourier transfer spectrometer

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994icar..109..367w&link_type=abstract

Icarus (ISSN 0019-1035), vol. 109, no. 2, p. 367-381

Other

21

Atmospheric Models, Line Spectra, Phosphines, Rotational States, Saturn Atmosphere, Absorption Spectra, Atmospheric Composition, Fourier Transformation, Infrared Spectrometers, Radiative Transfer, Rotational Spectra

Scientific paper

In recent observations with the Fourier transform spectrometer at the Caltech Submillimeter Observatory (CSO), we have detected the highly pressure-broadened (Full width at half maximum (FWHM) = 11.2 GHz) J = 1-0 rotational transition of PH3 (phosphine) on Saturn. By modeling the saturnian atmosphere with a radiative transfer code, we find that the observed line profile is consistent with a constant PH3 mole fraction of 0.3 +/- 1.0 ppm in the upper troposphere. A best fit to the depth of the line implies a cutoff at high altitudes, with no PH3 present at pressures less than and about 100 mbar. The observed line depth, combined with the lack of a detectable emission core, implies that a cutoff in the PH3 abundance occurs at a pressure between 13 and 140 mbar. We did not detect PH3 in Jupiter or any other molecular lines between 195 and 295 GHz (1.54 mm and 2.02 mm, respectively) in either Jupiter or Saturn.

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