Molecular Gas Outflow in the Starburst Galaxy NGC 1482

Galactic winds are essential to the regulation of star formation in galaxies. To study the distribution and dynamics of molecular gas in wind, we imaged the nearby starburst galaxy NGC 1482 in CO (J = 1 -> 0) at a resolution of 1 " (approximate to 100 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 Ha and soft X-rays. The velocity, mass outflow rate, and kinetic energy of the molecular outflow are v(w) similar to 100 km s(-1),. (M) over dot(w) similar to 7M(circle dot) yr(-1), and E-w similar to 7 x 10 erg(54), respectively. (M) over dot (w) is comparable to the star formation rate ((M) over dot(w)/SFR similar to 2) and Ew is similar to 1% of the total energy released by stellar feedback in the past 1 x 10(7) yr, which is the dynamical timescale of the outflow. The results indicate that the wind is starburst driven.