Effects of magnetic field orientations in dense cores on gas kinematics
  in protostellar envelopes
  Theoretically, misalignment between the magnetic field and rotational axis in
a dense core is considered to be dynamically important in the star formation
process, however, extent of this influence remains observationally unclear. For
a sample of 32 Class 0 and I protostars in the Perseus Molecular Cloud, we
analyzed gas motions using C$^{18}$O data from the SMA MASSES survey and the
magnetic field structures using 850 $\mu$m polarimetric data from the JCMT
BISTRO-1 survey and archive. We do not find any significant correlation between
the velocity gradients in the C$^{18}$O emission in the protostellar envelopes
at a 1,000 au scale and the misalignment between the outflows and magnetic
field orientations in the dense cores at a 4,000 au scale, and there is also no
correlation between the velocity gradients and the angular dispersions of the
magnetic fields. However, a significant dependence on the misalignment angles
emerges after we normalize the rotational motion by the infalling motion, where
the ratios increase from $\lesssim1$ to $\gtrsim1$ with increasing misalignment
angles. This suggests that the misalignment could prompt angular momentum
transportation to the envelope scale but is not a dominant factor in
determining the envelope rotation, and other parameters, like mass accretion in
protostellar sources, also play an important role. These results remain valid
after taking into account projection effects. The comparison between our
estimated angular momentum in the protostellar envelopes and the sizes of the
known protostellar disks suggests that significant angular momentum is likely
lost between radii of $\sim$1,000-100 au in protostellar envelopes.
