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We investigate turbulent properties of the non-star-forming, translucentmolecular cloud, MBM16 by applying the statistical technique of atwo-dimensional spatial power spectrum (SPS) on the neutral hydrogen (HI)observations obtained by the Galactic Arecibo L-Band Feed Array HI (GALFA-HI)survey. The SPS, calculated over the range of spatial scales from 0.1 to 17 pc,is well represented with a single power-law function, with a slope ranging from-3.3 to -3.7 and being consistent over the velocity range of MBM16 for a fixedvelocity channel thickness. However, the slope varies significantly with thevelocity slice thickness, suggesting that both velocity and density contributeto HI intensity fluctuations. By using this variation we estimate the slope of3D density fluctuations in MBM16 to be -3.7\pm0.2. This is significantlysteeper than what has been found for HI in the Milky Way plane, the SmallMagellanic Cloud, or the Magellanic Bridge, suggesting that interstellarturbulence in MBM16 is driven on scales >17 pc and that the lack of stellarfeedback could be responsible for the steep power spectrum.

Characterizing the Turbulent Properties of the Starless Molecular Cloud MBM16