Gas kinematics and the Dragged Magnetic Field in the High-mass Molecular
  Outflow Source G192.16$-$3.84: An SMA View
  We report the Submillimeter Array (SMA) observations of the polarized
0.88\,mm thermal dust emission and various molecular line transitions toward
the early B-type ($L_{*}\sim2\times10^{3}L_{\odot}$) star-forming region
G192.16$-$3.84 (IRAS 05553+1631). The peak of the continuum Stokes-I emission
coincides with a hot rotating disk/envelope (SO$_{2}$ rotational temperature
T$_{rot}^{SO_{2}}$$\sim84^{+18}_{-13}$\,K), with a north-south velocity
gradient. Joint analysis of the rotation curve traced by HCO$^{+}$ 4-3 and
SO$_{2}$ 19$_{1,19}-18_{0,18}$ suggests that the dense molecular gas is
undergoing a spinning-up rotation, marginally bound by the gravitational force
of \textbf{an} enclosed mass $M_{*+gas+dust}\sim$11.2-25.2\,$M_{\odot}$.
Perpendicular to the rotational plane a $\gtrsim100/\cos(i)$\,km\,s$^{-1}$
($i\sim63^{\circ}$) high velocity molecular jet, and the
$\sim$15-20\,km\,s$^{-1}$ expanding biconical cavity were revealed in the CO
3-2 emission. The polarization percentage of the 0.88\,mm continuum emission
decreases toward the central rotating disk/envelope. The polarization angle in
the inner $\sim2"$ (0.015\,pc) disk/envelope is perpendicular to the plane of
the rotation. The magnetic field lines, which are predominantly in the toroidal
direction along the disk plane, are likely to be dragged by the gravitationally
accelerated rotation.
