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  • 1
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    Detection of the 267 GHz J = 1-0 rotational transition of PH3 in Saturn with a new Fourier transform spectrometer (1994)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: In recent observations at the Caltech Submillimeter Observatory, the highly pressure-broadened (FWHM = 11.2 GHz) J = 1-0 rotational transition of PH3 (phosphine) was detected on Saturn. By modeling the Saturnian atmosphere with a radiative transfer code, the observed line profile was consistent with a constant PH3 mole fraction of 3.0 plus or minus 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 approximately less than 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. PH3 in Jupiter was not detected, nor any other molecular lines between 195 and 295 GHz (1.54 mm and 1.02 mm, respectively) in either Jupiter or Saturn.
    Keywords: ASTRONOMY
    Type: NASA-CR-194364 , NAS 1.26:194364
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 2
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    High spectral and spatial resolution observations of the 12.28 micron emission from H2 in the Orion molecular cloud (1981)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The pure rotational S(2) line of molecular hydrogen at 12.28 microns was looked for in 44 positions in the Orion moleular cloud with 6 in. beams and 35 km/s spectral resolution; it was detected in 27 positions. Emission was observed over a velocity range of + or - 100 km/s. The lines are approximately symmetric, and have full widths at half maximum ranging from 100 km/s down to the resolution limit. The distribution of intensities and line shapes is largely consistent with that seen in the 2 micron hydrogen transitions. However, unexpectedly complex line profiles and point-to-point variations in linear shapes appear, particularly in the region near IRc9.
    Keywords: ASTRONOMY
    Type: NASA-CR-164889
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 3
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    Detection of the 267 GHz J = 1-0 rotational transition of PH3 in Saturn with a new fourier transfer spectrometer (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: 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.
    Keywords: ASTRONOMY
    Type: Icarus (ISSN 0019-1035); 109; 2; p. 367-381
    Format: text
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    NASA TECHNICAL REPORTS
  • 4
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    Vibrationally excited CS: A new probe of conditions in young protostellar systems (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Description: We present the first detection of vibrationally excited C(32)S J = 10-9 and J = 7-6 emission toward a young stellar object (YSO). Toward IRAS 16293-2422, the vibrationally excited C(32)S emission is redshifted approximately 3.9 km/s from the systemic velocity of the core. The emission must arise in warm (T greater than or approximately equal 1000 K), dense (n greater than or approximately equal to 10(exp 11)-10(exp 12) per cc) gas. The most plausible origin for the emission appears to be self-gravitating instabilities in a protostellar accretion disk, which produce waves and shocks.
    Keywords: ASTRONOMY
    Type: Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X); 437; 2; p. L127-L130
    Format: text
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    NASA TECHNICAL REPORTS
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