Observations of chemical differentiation in clumpy molecular clouds

Abstract

We have extensively mapped a sample of dense molecular clouds (L1512, TMC-1C, L1262, Per 7, L1389, L1251E) in lines of HC3N, CH3OH, SO and C^{18}O. We demonstrate that a high degree of chemical differentiation is present in all of the observed clouds. We analyse the molecular maps for each cloud, demonstrating a systematic chemical differentiation across the sample, which we relate to the evolutionary state of the cloud. We relate our observations to the cloud physical, kinematical and evolutionary properties, and also compare them to the predictions of simple chemical models. The implications of this work for understanding the origin of the clumpy structures and chemical differentiation observed in dense clouds are discussed.

20 pages, 7 figures. Higher quality figures appear in the published journal article

References in corpus (4)

• An atomic and molecular database for analysis of submillimetre line observations
• Molecular Evolution in Collapsing Prestellar Cores III: Contraction of A Bonnor-Ebert Sphere
• Spitzer Mid-infrared Spectroscopy of Ices Toward Extincted Background Stars
• Turbulence driven by outflow-blown cavities in the molecular cloud of NGC 1333

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