Journal
ASTROPHYSICAL JOURNAL
Volume 779, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/779/1/36
Keywords
ISM: clouds; ISM: structure; magnetohydrodynamics (MHD); turbulence
Categories
Funding
- NSF [AST-0707597, 0917810, 0707679, 0709347]
- Research Corporation for Science Advancement
- NASA through a Hubble Fellowship grant from STScI [HST-HF-51295.01A]
- NASA [NAS5-26555]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0707679] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0917810, 0709347] Funding Source: National Science Foundation
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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.
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