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Interstellar Chemistry in Orion KL

Published online by Cambridge University Press:  12 April 2016

Satoshi Yamamoto ,
Hitomi Mikami  and
Shuji Saito
Satoshi Yamamoto
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa, Nagoya 464-01, Japan
Hitomi Mikami
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa, Nagoya 464-01, Japan
Shuji Saito
Affiliation:
Institute for Molecular Science, Okazaki444, Japan

Abstract

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A map of SiO (J = 2 − 1) in Ori KL has been obtained with 2.8” spatial resolution by using Nobeyama Millimeter Array. The distribution of SiO evidences an interaction between outflow and dense gas around IRc4 and IRc5; these infrared sources are thus considered to be shock-heated regions. Since distributions of (CH3)2O and HCOOCH3 have a peak at the IRc5 position, such shock heating seems to play an important role in production of these molecules. Detection of CH3OD around the interacting region most likely suggests that CH3OH is evaporating from dust grains. (CH3)2O and HCOOCH3 may be produced by gas-phase reactions starting from injected CH3OH, or they might be evaporated from dust grains.

Type
3. Astronomical Results and Prospects
Information
International Astronomical Union Colloquium , Volume 140: Astronomy with Millimeter and Submillimeter Wave Interferometry , 1994 , pp. 190 - 194
Copyright
Copyright © Astronomical Society of the Pacific 1994

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