| Abstract |
While studies of galaxy evolution generally focus on extensive HI
surveys at large redshifts, we argue in this paper that the
understanding of detailed physical processes that drive HI evolution in
galaxies is equally important. Specifically, we focus on three open
questions regarding the very first step in the star-formation cycle in
galaxies: How much do galaxy halos flavor and tax the accretion flows
that are postulated to bring fresh star-formation fuel to galaxy disks?
What are the basic properties of the warm neutral gas, the progenitor of
cold star-forming clouds? And, what are the origin and level of
interstellar inhomogeneities as seeding agents for molecule and star
formation? The very local Universe (The Milky Way and nearby galaxies)
offers an unparalleled high-resolution view for answering these
questions and the upcoming radio telescopes (e.g. EVLA, ASKAP, MeerKAT,
ATA-256) promise great advances. |