A holistic perspective on the dynamics of G035.39-00.33: the interplay
  between gas and magnetic fields
  Magnetic field is one of the key agents that play a crucial role in shaping
molecular clouds and regulating star formation, yet the complete information on
the magnetic field is not well constrained due to the limitations in
observations. We study the magnetic field in the massive infrared dark cloud
G035.39-00.33 from dust continuum polarization observations at 850 $\micron$
with SCUBA-2/POL-2 at JCMT. The magnetic field tends to be perpendicular to the
densest part of the main filament (F$_{M}$), whereas it has a less defined
relative orientation in the rest of the structure, where it tends to be
parallel to some diffuse regions. A mean plane-of-the-sky magnetic field
strength of $\sim$50 $\mu$G for F$_{M}$ is obtained using
Davis-Chandrasekhar-Fermi method. Based on $^{13}$CO (1-0) line observations,
we suggest a formation scenario of F$_{M}$ due to large-scale ($\sim$10 pc)
cloud-cloud collision. Using additional NH$_3$ line data, we estimate that
F$_{M}$ will be gravitationally unstable if it is only supported by thermal
pressure and turbulence. The northern part of F$_{M}$, however, can be
stabilized by a modest additional support from the local magnetic field. The
middle and southern parts of F$_{M}$ are likely unstable even if the magnetic
field support is taken into account. We claim that the clumps in F$_{M}$ may be
supported by turbulence and magnetic fields against gravitational collapse.
Finally, we identified for the first time a massive ($\sim$200 M$_{\sun}$),
collapsing starless clump candidate, "c8", in G035.39-00.33. The magnetic field
surrounding "c8" is likely pinched, hinting at an accretion flow along the
filament.
