  We have mapped the pre-planetary nebula IRAS 17150-3224 in 350 GHz continuum
and CO J=3-2 line at an angular resolution of about 0".09 using the Atacama
Large Millimeter/submillimeter Array. A continuum source is detected at the
center of the nebula, elongated along the equatorial plane, likely tracing a
dusty torus around the central source. Continuum emission is also detected on
both sides of the central continuum source in the equatorial plane, probably
resulting from interactions of collimated fast winds with envelope material in
the equator. CO emission is detected along the optical lobe. Although the
optical lobe appears as bipolar, CO map shows that it is actually a quadrupolar
outflow consisting of two overlapping bipolar outflows. Two additional younger
bipolar outflows are also detected in CO, one at lower latitude and the other
along the equatorial plane. In the CO position-velocity maps, blueshifted
absorption stripes are detected in the outflow emissions, due to absorption by
a series of shells produced by a series of asymptotic giant branch (AGB) wind
ejections. By modeling the morphology and kinematics of the AGB wind and
outflows, we find that the AGB wind could end about 1300 yr ago, the
quadrupolar outflow was ejected about 350 yr ago, and the two additional
bipolar outflows were ejected about 280 and 200 ago, respectively. The outflows
could be produced either by bullets coming from an explosion, or by a
precessing collimated fast wind with a time-dependent ejection velocity.
