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  Our limited sample measurement doesn't allow us to robustly
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  We start by illustrating the variety in Hi column densities and lots throughout our
  suite of simulated faint dwarf galaxies in Figure 1.
  We show the evolution of the central Hi mass (bottom panel) for
  example objects in our three lessons of dwarf galaxies, and plot Hi column density maps (prime to third row) at three different snapshot occasions in the final billion years of evolution (left
  to right). Specifically, we use three genetically-modified mass growths targeting the early mass meeting of a low-mass host (Halo 1459 in Table 1; see Rey et al.
  In low-mass haloes, retaining gasoline is at first order determined by
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