Galactic and magellanic evolution with the SKA

Naomi M. McClure-Griffiths*, Snežana Stanimirovíc, Claire E. Murray, Di Li, John M. Dickey, Enrique Vázquez-Semadeni, Josh E.G. Peek, Mary Putman, Susan E. Clark, Marc Antoine Miville-Deschênes, Joss Bland-Hawthorn, Lister Staveley-Smith

*Corresponding author for this work

Research output: Contribution to journalConference articlepeer-review


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 l21-cm line of atomic hydrogen (H I) 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.

Original languageEnglish
Article number130
JournalProceedings of Science
Publication statusPublished - 2014
Externally publishedYes
EventAdvancing Astrophysics with the Square Kilometre Array, AASKA 2014 - Giardini Naxos, Italy
Duration: 9 Jun 201413 Jun 2014


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