The Winds from HL Tau
  Outflowing motions, whether a wind launched from the disk, a jet launched
from the protostar, or the entrained molecular outflow, appear to be an
ubiquitous feature of star formation. These outwards motions have a number of
root causes, and how they manifest is intricately linked to their environment
as well as the process of star formation itself.
  Using the ALMA Science Verification data of HL Tau, we investigate the high
velocity molecular gas being removed from the system as a result of the star
formation process. We aim to place these motions in context with the optically
detected jet, and the disk. With these high resolution ($\sim 1"$) ALMA
observations of CO (J=1-0), we quantify the outwards motions of the molecular
gas. We find evidence for a bipolar outwards flow, with an opening angle, as
measured in the red-shifted lobe, starting off at 90$^\circ$, and narrowing to
60$^\circ$ further from the disk, likely because of magnetic collimation. Its
outwards velocity, corrected for inclination angle is of order 2.4 km s$^{-1}$.
