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Zeeman Splitting in the Diffuse ISM

Published online by Cambridge University Press:  21 October 2010

Carl Heiles
Carl Heiles*
Affiliation:
Astronomy Department, University of California, Berkeley CA 94720-3422, USA email: heiles@astro.berkeley.edu
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Abstract

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Many Zeeman-spitting measurements in the diffuse Galactic Interstellar Medium have been made of the 21-cm line in both absorption and emission. Typical field strength is about 6 μG, with enhancement in shocked regions; the magnetic, turbulent, and cosmic-ray pressures are comparable and considerably larger than the thermal gas pressure. For PhotoDissociation Regions, Carbon recombination lines show intriguing results for single-dish measurements. OH Megamasers in Ultra-Luminous Infrared Galaxies show easily detectable fields whose strength ranges up to at least 20 mG. Upper limits for several damped Ly-α systems range down to a few μG. The z=0.692 system against 3C286 was reported in the literature to have a large field strength, but this result is wrong.

Keywords

ISM: magnetic fieldsgalaxies: magnetic fieldsmaserspolarization
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 428 - 429
Copyright
Copyright © International Astronomical Union 2010

References

Ferrière, K. 2001, RevModPhyss, 73, 1031Google Scholar
Heiles, C. 1988, ApJ, 324, 321CrossRefGoogle Scholar
Heiles, C. 1989, ApJ, 336, 808CrossRefGoogle Scholar
Heiles, C. 1994, ApJ, 424, 208Google Scholar
Heiles, C. 1996, ApJ 466, 224CrossRefGoogle Scholar
Heiles, C. 1997, ApJS 111, 245CrossRefGoogle Scholar
Heiles, C. 1998, Astrophys. Lett. and Comm. 37, 85Google Scholar
Heiles, C. & Troland, T. H. 2005, ApJ 624, 773CrossRefGoogle Scholar
Myers, P. C., Goodman, A. A., Rüsten, R., & Heiles, C. 1995, ApJ, 442, 177CrossRefGoogle Scholar
Robishaw, T. 2008, Ph.D. Thesis, University of California, Berkeley (AAT 3331778)Google Scholar
Robishaw, T. & Heiles, C. 2009, PASP, 121, 272CrossRefGoogle Scholar
Robishaw, T., Quataert, E., & Heiles, C. 2008, ApJ, 680, 981CrossRefGoogle Scholar
Verschuur, G. L. 1969, ApJ, 156, 861CrossRefGoogle Scholar
Verschuur, G. L. 1989, ApJ, 339, 163CrossRefGoogle Scholar
Verschuur, G. L. 1995a, ApJ, 451, 624CrossRefGoogle Scholar
Verschuur, G. L. 1995b, ApJ, 451, 645CrossRefGoogle Scholar
Wolfe, A. M., Jorgenson, R. A., Robishaw, T., Heiles, C., & Prochaska, J. X. 2008, Nature, 455, 638CrossRefGoogle Scholar