Characterizing the turbulent properties of the starless molecular cloud MBM 16
Journal Article
·
· Astrophysical Journal
- Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706 (United States)
- Department of Astronomy, Columbia University, New York, NY 10027 (United States)
- Indian Institute of Science Education and Research, ITI Campus (Gas Rahat) Building, Govindpura, Bhopal- 23 (India)
- University of Calgary/Dominion Radio Astrophysical Observatory, P.O. Box 248, Penticton, BC V2A6J9 (Canada)
- Astronomy Department and Space Science Laboratory, University of California, Berkeley, CA 94703 (United States)
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.
- OSTI ID:
- 22348549
- Journal Information:
- Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 779; ISSN ASJOAB; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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