Whether magnetic fields or turbulence play a critical role in the star formation processes has been one of the most important unresolved questions in star formation.   Classical low mass star formation theory claims that ambipolar diffusion is essential to remove magnetic flux for gravitational collapse; however, many MHD simulations shows that molecular clouds can fragment and form stars under the influence of turbulence without much assistance from the magnetic fields.   Recent ALMA observations of magnetic fields have revealed much more structure that cannot be seen before with lower resolution data.   In addition, some recent ALMA observations at disk scales show that scattering cannot be ignored which would challenge the reliability of the magnetic field measurement but also could provide critical information on dust growths for the formation of planetesimals. Therefore, carefully modeling the magnetic fields from large to small structure is necessary to understand the full picture of the magnetic field structure and their influence on star formation.   Here we would like to combine the ALMA archival data with JCMT/SMA/CARMA data for magnetic field structure analysis.