Not –So-Dense Gas in Not-So-Distant Galaxies
Andrew Baker (Rutgers University)
To understand how
galaxies evolve across cosmic time, we must
understand not only
their dark matter and their stars, but also the
properties of their
interstellar gas, from which new stars form and
into which old stars
release the products of their nucleosynthesis.
In normal galaxies like
the Milky Way, a majority of this gas lies at
temperatures that are
neither hot enough to ionize hydrogen atoms
nor cold enough to
permit the formation of hydrogen molecules. Such
material is best
traced at radio wavelengths using the 21cm spin-flip
transition of neutral
atomic hydrogen (HI). I will describe what we
can learn from
observations of HI emission in galaxies, and how we
will use a powerful
new array of 64 radio telescopes in South Africa
to observe a single
position on the sky for thousands of hours,
thereby probing the
evolution of galaxies' HI reservoirs over the
last nine billion
years. This effort, constituting the LADUMA (Looking
At the Distant
Universe with the MeerKAT Array) survey, will
benefit
from close
connections with optical-wavelength observations and
theoretical modeling.