Magnetic Field Morphology in Interstellar Clouds with the Velocity
  Gradient Technique
  Magnetic fields, while ubiquitous in many astrophysical environments, are
challenging to measure observationally. Based on the properties of anisotropy
of eddies in magnetized turbulence, the Velocity Gradient Technique is a method
synergistic to dust polarimetry that is capable of tracing plane-of-the-sky
magnetic field, measuring the magnetization of interstellar media and
estimating the fraction of gravitational collapsing gas in molecular clouds
using spectral line observations. In this paper, we apply this technique to
five low-mass star-forming molecular clouds in the Gould Belt and compare the
results to the magnetic-field orientation obtained from polarized dust
emission. We find the estimates of magnetic field orientations and
magnetization for both methods are statistically similar. We estimate the
fraction of collapsing gas in the selected clouds. By means of the Velocity
Gradient Technique, we also present the plane-of-the-sky magnetic field
orientation and magnetization of the Smith cloud, for which dust polarimetry
data are unavailable.
