Complex Organic Molecules in Taurus Molecular Cloud-1

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<jats:title>Abstract</jats:title> <jats:p>We have observed the millimeter-wave rotational spectral lines of CH<jats:sub>3</jats:sub>CHO, H<jats:sub>2</jats:sub>CCO, cyclopropenone, and H<jats:sub>2</jats:sub>CO toward the cyanoployyne peak of Taurus Molecular Cloud-1 (TMC-1 CP). The spectral line profile of CH<jats:sub>3</jats:sub>CHO is found to reveal a well-separated double peak. It is similar to the line profile of CH<jats:sub>3</jats:sub>OH, but is much different from those of carbon-chain molecules and C<jats:sup>34</jats:sup>S. The different line profiles mean different distributions along the line of sight. The similarity of the spectral line profiles between CH<jats:sub>3</jats:sub>CHO and CH<jats:sub>3</jats:sub>OH suggests that CH<jats:sub>3</jats:sub>CHO is mainly formed on dust grains as CH<jats:sub>3</jats:sub>OH or through gas-phase reactions starting from CH<jats:sub>3</jats:sub>OH. On the other hand, the spectral line profiles of H<jats:sub>2</jats:sub>CCO and cyclopropenone are rather similar to those of carbon-chain molecules and C<jats:sup>34</jats:sup>S, implying their gas-phase productions. H<jats:sub>2</jats:sub>CO shows a composite spectral line profile reflecting the contributions of both gas-phase and grain-surface productions. In addition, we have detected the spectral lines of CH<jats:sub>3</jats:sub>CHO and HCOOCH<jats:sub>3</jats:sub> toward the methanol peak near TMC-1 CP. We have also tentatively detected one line of (CH<jats:sub>3</jats:sub>)<jats:sub>2</jats:sub>O. Considering the chemical youth of TMC-1, the present results indicate that fairly complex organic species have already been formed in the early evolutionary phase of starless cores. TMC-1 is thus recognized as a novel source where formation processes of complex organic molecules can be studied on the basis of the line profiles.</jats:p>

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