  We show that the starburst-driven outflow in the peculiar galaxy NGC 2782
forms a well-defined collimated bubble which has an extent of $\sim$ 1 kpc and
a closed shell at its edge, as seen in H$\alpha$, [O III], and 5 GHz radio
continuum. The shell coincides with the maximum in intensity and linewidths of
[O III] lines in a blueshifted emission nebula which was previously detected
via optical spectroscopy by Boer et al. (1992). Such a remarkable outflow
morphology has not been observed to date in any other starburst galaxy of
comparable luminosity. The radio continuum map reveals a second bubble of
similar size on the opposite side of the nucleus, forming a striking
double-bubble outflow morphology. We argue from the morphology and short
timescale ($\sim$ $4 \times 10^6$ years) of the outflow that it is dynamically
younger than freely-expanding outflows seen in other galaxies which harbor
circumnuclear starbursts of comparable luminosity, e.g., M82. We suggest that
the outflow in NGC 2782 is in the early stage where thermal instabilities have
not yet completely ruptured the outflow bubble.We present evidence that the
outflow is driving warm and hot ionised gas, and possibly cold molecular gas,
out of the central kpc of the galaxy. We estimate the contribution of the hot,
warm, and cold phases of the ISM to the energetics of the outflow. This study
is based on our optical BVR, H$\alpha$, and [O III] observations from the WIYN
telescope and OVRO CO interferometric data, along with available 5 GHz radio
continuum and ROSAT X-ray maps.
