Infalling motions were detected and modeled toward this source. A mean infall velocity of 0.5 km/s with an infall mass rate of 5x10^-3 Solar masses per year was obtained. Also, a previously estimated value for the magnetic field strength in the plane
of the sky was refined to be 855 micro Gauss which we used to calculate a mass-to-magnetic flux ratio of 1.9, or super-critical. The virial mass from turbulent motions was also calculated finding Mvir=563 solar masses, which gives a ratio of Msubmm/Mvir=5.9. Both values strongly suggest that this clump must be in a state of gravitational collapse.
We report millimeter interferometric observations of polarized continuum and line emission from the massive star forming region G34.4. Polarized thermal dust emission at 3 mm wavelength and CO $J=1 to 0$ line emission were observed using the Berkeley
-Illinois-Maryland Association (BIMA) array. Our results show a remarkably uniform polarization pattern in both dust and in CO J=$1 to 0$ emission. In addition, the line emission presents a consistent uniform polarization pattern over most of the velocity channel maps. These uniform polarization patterns are aligned with the north-south main axis of the filament between the main millimeter source (MM) and the ultra-compact H {scriptsize II} region, which are the central sources in G34.4, suggesting a magnetic field orthogonal to this axis. This morphology is consistent with a magnetically supported disk seen roughly edge-on.
