  Galactic winds are essential to regulation of star formation in galaxies. To
study the distribution and dynamics of molecular gas in a wind, we imaged the
nearby starburst galaxy NGC 1482 in CO ($J=1\rightarrow0$) at a resolution of
1'' ($\approx100$ pc) using the Atacama Large Millimeter/submillimeter Array.
Molecular gas is detected in a nearly edge-on disk with a radius of 3 kpc and a
biconical outflow emerging from the central 1 kpc starburst and extending to at
least 1.5 kpc perpendicular to the disk. In the outflow, CO gas is distributed
approximately as a cylindrically symmetrical envelope surrounding the warm and
hot ionized gas traced by H$\alpha$ and soft X-rays. The velocity, mass outflow
rate, and kinetic energy of the molecular outflow are
$v_\mathrm{w}\sim100~\mathrm{km~s^{-1}}$,
$\dot{M}_\mathrm{w}\sim7~M_\odot~\mathrm{yr}^{-1}$, and
$E_\mathrm{w}\sim7\times10^{54}~\mathrm{erg}$, respectively.
$\dot{M}_\mathrm{w}$ is comparable to the star formation rate
($\dot{M}_\mathrm{w}/\mathrm{SFR}\sim2$) and $E_\mathrm{w}$ is $\sim1\%$ of the
total energy released by stellar feedback in the past
$1\times10^7~\mathrm{yr}$, which is the dynamical timescale of the outflow. The
results indicate that the wind is starburst driven.
