| Abstract : | The magnetic fields contribute a significant amount of pressure—as much as turbulence does—and more than thermal energy to the diffuse interstellar medium. These factors and gravity collaborate in a complex way to govern the rate and efficiency of star formation. Stars form due to the gravitational collapse of fragmented, dense cores that lie along the ridges of the molecular cloud filaments. Investigating how each agent's contribution varies as a function of density and spatial scale is crucial to fully understand magnetic fields' role. Thanks to the wide-field and sensitive polarimeters, which enable us to shed light on this. In this presentation, I'll talk about how to make a detailed map of a magnetic field, how to estimate the strength of a magnetic field, and how to compare the importance of magnetic fields to that of turbulence, gravity, and stellar feedback. I will talk about the results of the multi-wavelength polarization observations of a wide range of sources, such as low-mass star-forming filamentary clouds, massive dense cores in and around bipolar HII regions, massive clumps with energetic outflows, dark globules, etc. I will also briefly discuss the HINSA Zeeman experiment with the FAST telescope and JCMT's BISTRO project. |
