Turbulent velocity structure in interstellar clouds

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Abstract
The feasibility of directly measuring a spatially correlated turbulent velocity spectrum in interstellar clouds is investigated. It is argued on a number of grounds that relations between line width and scale size are unsuitable for this purpose. A more direct method is suggested for the determination of the turbulent velocity structure using well-sampled observations of mean velocities, to estimate the accuracy with which mean velocities must be measured for this purpose, and to point out the difficulties in the interpretation of this approach and of the line width-size relation. A preliminary C18O velocity autocorrelation function for the dense core of the ρ Oph cloud is presented as an example.

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