Detection of solid methanol toward W33A

Details Detection of solid methanol toward W33A Detection of solid methanol toward W33A

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...243..473g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 243, no. 2, March 1991, p. 473-477.

Astronomy and Astrophysics

Astrophysics

91

Absorption Spectra, Early Stars, Interstellar Matter, Methyl Alcohol, Abundance, Astronomical Spectroscopy, Infrared Spectra, Photochemical Reactions

Scientific paper

A recently detected absorption feature at 3.53 microns in the spectrum of W33A has been assigned to methanol (CH3OH). Its optical depth implies that methanol is the second most abundant molecule (7 percent relative to H2O) in the grain mantles in the line of sight toward W33A observed to date. Laboratory experiments have shown that the implied abundance is difficult to explain by UV irradiation of the dust grains alone. Grain surface reactions or condensation directly out of the gas phase must also play roles, but the relative contributions of the various processes are difficult to estimate. The optical depth of the 3.53-micron feature constrains the contribution of methanol to the 6.8-micron feature in W33A to be 10 percent or less, requiring the contribution of at least one other compound to this feature, while the estimated contribution to the 4.9-micron absorption band is even smaller. Only a small contribution of formaldehyde (H2CO) is consistent with the observed 3.53-micron band profile. In contrast to methanol, formaldehyde can be produced readily by photochemical reactions within the ice mantle.

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