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Angular power spectra of Galactic HI

Published online by Cambridge University Press:  01 August 2006

D. A. Green
D. A. Green*
Affiliation:
Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Avenue, Cambridge, CB4 3PT, UK email: dag@mrao.cam.ac.uk
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Abstract

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As an alternative to identifying and then studying particular features seen in Galactic HI 21-cm images, studies of the angular power spectra of the emission provide a concise, statistical description of HI emission. The angular power spectra of several fields near l = 140°, from the Canadian Galactic Plane Survey, as observed with the DRAO Synthesis Telescope, have been analysed in this way. The derived power spectra, which typically cover angular scales from about 0 · 15 to 0 · 9 degree, are generally well-fitted by a simple power-law dependence on angular scale.

Keywords

ISM: structureturbulencetechniques: interferometricradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 413
Copyright
Copyright © International Astronomical Union 2007

References

Dickey, J. M., McClure-Griffiths, N. M.Stanimirović, S., Gaensler, B. M. & Green, A. J. 2001, ApJ 561, 264CrossRefGoogle Scholar
Green, D. A. 1993, MNRAS 262, 327CrossRefGoogle Scholar
Taylor, A. R., et al. 2003, AJ 125, 3145CrossRefGoogle Scholar