Characterizing the turbulent properties of the starless molecular cloud MBM 16

We investigate turbulent properties of the non-star-forming, translucent molecular cloud MBM 16 by applying the statistical technique of a two-dimensional spatial power spectrum (SPS) on the neutral hydrogen (H I) observations obtained by the Galactic Arecibo L-Band Feed Array H I 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 MBM 16 for a fixed velocity channel thickness. However, the slope varies significantly with the velocity slice thickness, suggesting that both velocity and density contribute to H I intensity fluctuations. By using this variation, we estimate the slope of three-dimensional density fluctuations in MBM 16 to be –3.7 ± 0.2. This is significantly steeper than what has been found for H I in the Milky Way plane, the Small Magellanic Cloud, or the Magellanic Bridge, suggesting that interstellar turbulence in MBM 16 is driven on scales >17 pc and that the lack of stellar feedback could be responsible for the steep power spectrum.