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Galactic and magellanic evolution with the SKA


McClure-Griffiths, NM and Stanimirovic, S and Murray, CE and Li, D and Dickey, JM and Vazquez-Semadeni, E and Peek, JEG and Putman, M and Clark, SE and Miville-Deschenes, M-A and Bland-Hawthorn, J and Staveley-Smith, L, Galactic and magellanic evolution with the SKA, Advancing Astrophysics with the Square Kilometre Array, 09-13 June 2014, Giardini Naxos, Italy, pp. 655-677. ISBN 978-1-909204-70-6 (2015) [Refereed Conference Paper]



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Copyright 2015 the Author Licensed under Creative Commons Attribution-ShareAlike 4.0 International (CC BY-SA 4.0)

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As we strive to understand how galaxies evolve it is crucial that we resolve physical processes and test emerging theories in nearby systems that we can observe in great detail. Our own Galaxy, the Milky Way, and the nearby Magellanic Clouds provide unique windows into the evolution of galaxies, each with its own metallicity and star formation rate. These laboratories allow us to study with more detail than anywhere else in the Universe how galaxies acquire fresh gas to fuel their continuing star formation, how they exchange gas with the surrounding intergalactic medium, and turn warm, diffuse gas into molecular clouds and ultimately stars. The λ21-cm line of atomic hydrogen (H ɪ) is an excellent tracer of these physical processes. With the SKA we will finally have the combination of surface brightness sensitivity, point source sensitivity and angular resolution to transform our understanding of the evolution of gas in the Milky Way, all the way from the halo down to the formation of individual molecular clouds.

Item Details

Item Type:Refereed Conference Paper
Keywords:radio astronomy, square kilometre array, galactic structure, interstellar medium
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Dickey, JM (Professor John Dickey)
ID Code:102297
Year Published:2015
Funding Support:Australian Research Council (DP110104101)
Deposited By:Mathematics and Physics
Deposited On:2015-08-11
Last Modified:2017-11-06
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