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  • 2000-2004
  • 1985-1989  (3)
  • 1989  (3)
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  • 2000-2004
  • 1985-1989  (3)
Year
  • 1
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    Unknown
    Interferometric molecular line observations of W51 (1989)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Observations are presented of the H II region complex in W51 made with a mm interferometer. W51 is a region of massive star formation approx. 7 kpc distant from the sun. This region has been well studied in both the IR and submillimeter, the radio, as well as the maser transitions. These previous observations have revealed three regions of interest: (1) W51MAIN, a know of bright maser emission near two compact H II regions W51e1 and W51e2 (W51MAIN is also the peak of the 400 micron emission indicating that the bulk of the mass is centered there; (2) W51IRS1 is a long curving structure seen at 20 micron and at 2 and 6 cm but not at 400 micron; (3) W51IRS2 (also known as W51NORTH) is another compact H II region slightly offset from an 8 and a 20 micron peak and a collection of masers. Some conclusions are as follows: (1) SO and H(13)CN emission are similar and coincide with outflow activity; (2) HCO+ spectra show evidence for overall collapse of the W51 cloud toward W51MAIN; (3) A previously undetected continuum peak, W51DUST, coincides with the molecular peak H(13)CN-4; and (4) Dust emission at 3.4 mm reveals that about half of the 400 micron emission comes from the ultracompact H II region e2, and the rest from W51e1 and W51DUST.
    Keywords: ASTRONOMY
    Type: NASA, Ames Research Center, Interstellar Dust: Contributed Papers; p 221-226
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 2
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    Radio detection of formaldehyde emission from Comet Halley (1989)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: The J(K-1 K1) = -1(11) -10(10) transition of H2CO was detected in emission at 4829.659 MHz from Comet Halley. The H2CO emission line had a peak intensity of 2.66 + or - 0.78 mJy/beam with a small blueshift of -0.76 + or - 0.40 km/s, which is consistent with the anisotropic outgassing of the nucleus in the solar direction found for other cometary species. Data analysis suggests that cometary H2CO was produced from an extended source in the coma as well as directly from the nucleus and that it was not refrigerated as in interstellar dark nebulae. The derived H2CO production rate of 1.5 x 10 to the 28th molecules/s is obtained which is consistent with observational and theoretical findings.
    Keywords: ASTROPHYSICS
    Type: Astronomical Journal (ISSN 0004-6256); 97; 246-253
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    VLA observations of the OH emission from Comet Wilson (1986) - The value of high resolution in both spatial and velocity coordinates (1989)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: In comparison with Comet Halley, the radio OH emission from Comet Wilson behaved very erratically, changing rapidly in position as well as in velocity, while the emission and brightness distribution from Comet Halley displayed apparent stability. A few months later, nearer perihelion, just the opposite behavior was observed at UV wavelengths. Another difference between the two comets is that the OH emission from Comet Halley seemed confined to a region a few times 100.000 km in size, while the emission from Comet Wilson showed up in sporadic blobs, with variable intensities and velocities, at distances as far as 10 to the 6th km from the nucleus. This behavior in Comet Wilson may be associated with the disintegration of the outer frosting associated with new comets and possibly with the fragmentation and ejection of cometesimals from the nucleus. As part of the data analysis, it is demonstrated that lengthening the integration time and lowering the velocity resolution affects the symmetry of the OH images and spectral-line profiles. As a consequence, asymmetric cometary OH line profiles may be more common than previously thought.
    Keywords: ASTROPHYSICS
    Type: Astronomical Journal (ISSN 0004-6256); 97; 1791-179
    Format: text
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    NASA TECHNICAL REPORTS
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