Galactic and Magellanic Evolution with the SKA
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.