  Studying the earliest stages in the birth of stars is crucial for
understanding how they form. Brown dwarfs with masses between that of stars and
planets are not massive enough to maintain stable hydrogen-burning fusion
reactions during most of their lifetime. Their origins are subject to much
debate in recent literature because their masses are far below the typical mass
where core collapse is expected to occur. We present the first confirmed
evidence that brown dwarfs undergo a phase of molecular outflow that is typical
of young stars. Using the Submillimeter Array, we have obtained a map of a
bipolar molecular outflow from a young brown dwarf. We estimate an outflow mass
of 1.6 x 10^-4 M_Sun and a mass-loss rate of 1.4 x 10^-9 M_Sun. These values
are over two orders of magnitude smaller than the typical ones for T Tauri
stars. From our millimiter continuum data and our own analysis of Spitzer
infrared photometry, we estimate that the brown dwarf has a disk with a mass of
8 x 10^-3 M_Sun and an outer disk radius of 80 AU. Our results demonstrate that
the bipolar molecular outflow operates down to planetary masses, occurring in
brown dwarfs as a scaled-down version of the universal process seen in young
stars.
