Possible identifications of the 3.4 micrometer feature

Details Possible identifications of the 3.4 micrometer feature Possible identifications of the 3.4 micrometer feature

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ioch.rept...86d&link_type=abstract

In NASA, Washington, Infrared Observations of Comets Halley and Wilson and Properties of the Grains p 86-90 (SEE N89-13330 04-89

Computer Science

Atmospheric Chemistry, Cometary Atmospheres, Emission Spectra, Halley'S Comet, Molecular Structure, Absorption Spectra, Infrared Spectra, Interstellar Chemistry, Interstellar Matter, Spectrum Analysis

Scientific paper

A feature at 3.4 micrometer was first detected in Comet Halley by the IKS spectrometer on board the Vega 1 probe; and subsequently from the ground. The feature has since been reported in Comet Wilson. The presence of the feature is of considerable interest for a number of reasons. First, it may represent the detection of a new parent molecule, and when combined with data from Giotto and Vega yield new information on cometary chemistry and the early solar system composition. Secondly, it may represent a link to the interstellar medium, the feature corresponds in wavelength and shape with an interstellar feature seen in absorption in a luminous star, towards the Galactic center known as GC-IRS7. The feature in turn is thought to be related with a growing family of unidentified infrared emission features seen in stellar objects, planetary nebulae, reflection nebulae, HII regions and extra galactic sources. These features occur at wavelengths 3.3, 3.4, 3.5, 6.2, 7.7, 8.6, and 11.25 micrometers. Further identification theory is given.

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