  The Local Group galaxy Phoenix has the properties of a dwarf spheroidal
galaxy, but an adjacent HI cloud has been found to be at the same radial
velocity as the stars. The proximity suggests that this cloud is associated
with the most recent ($\le 100$ Myr) star formation in Phoenix. We have
obtained relatively high sensitivity and high resolution HI imaging with the
VLA with the goal of distinguishing between different processes for displacing
the gas from the galaxy. Due to the outer curvature of the HI cloud, it appears
that expulsion from the galaxy by winds from supernovae is more likely than
ram-pressure stripping. The isolation of the galaxy makes tidal stripping
highly unlikely. Using a star formation history constructed from HST imaging,
we construct a simple kinematic model which implies that the HI cloud is still
gravitationally bound to the galaxy. Gas which is expelled from the centers of
dwarf galaxies but which remains gravitationally bound may explain the episodic
star formation observed in several dwarfs. In the specific case of Phoenix,
there may be future star formation in this currently dSph-like galaxy.
