Discovery of solid formaldehyde toward the protostar GL 2136: observations and laboratory simulation.

Details Discovery of solid formaldehyde toward the protostar GL 2136: observations and laboratory simulation. Discovery of solid formaldehyde toward the protostar GL 2136: observations and laboratory simulation.

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...309..633s&link_type=abstract

Astronomy and Astrophysics, v.309, p.633-647

Astronomy and Astrophysics

Astrophysics

64

Ism: Clouds, Ism: Dust, Extinction, Ism: Molecules, Stars: Individual: Gl 2136, Methods: Laboratory, Infrared: Ism: Lines And Bands

Scientific paper

A search for the ν_5_ band of solid formaldehyde toward the protostellar source GL 2136 has resulted in the detection of absorption features near 3.47 and 3.54μm. A good match of the 3.47μm feature exists with solid H_2_CO features in laboratory analogs of interstellar ice condensates. The abundance of H_2_CO and the composition of the ice in which it is found are constrained by the precise wavelength of the 3.47μm absorption, the profile of the 3.54μm absorption feature, and the previously observed 9.75 (CH_3_OH), 6.0, and 6.8μm features. From comparison with laboratory spectra, we conclude that the H_2_CO and CH_3_OH are intimately mixed and that both contribute to the 3.54μm absorption, while the profiles of the 6.0 and 6.8μm bands indicate a contribution of the solid H_2_CO ν_2_ and ν_3_ features at 5.8 and 6.7μm. We estimate that the abundance of H_2_CO is ~7% of that of H_2_O seen along the same line of sight, but that only a small fraction of the H_2_O is intimately mixed with the H_2_CO. There appear to be at least two types of ice mantles present along the line of sight, one consisting of almost pure H_2_O (type I ice) and the other rich in, if not dominated by H_2_CO and CH_3_OH (type II ice). The possible origin of solid H_2_CO and the implication of our results for the physical and chemical conditions in the cloud are discussed

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