Abstract: The magnetic fields (B-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 formation of filamentary structures, their fragmentation into dense cores, and the overall outcome of star formation in the molecular clouds. Investigating how each agent interacts with others and how their pressures vary as a function of gas density and spatial scale is crucial to fully understanding B-fields' role. The wide-field and sensitive polarimeters enable us to trace B-field morphology and strength across the cloud, encompassing a range of densities and spatial scales. Based on the multi-wavelength dust polarization observations, I will present results from two textbook examples for low- and high-mass star-forming regions, such as the Taurus B213 filament and Cep A clump, respectively. I will discuss the key metrics and their implications for the formation and evolution of molecular clouds and star formation. Finally, I will briefly shed light on the results obtained from HINSA Zeeman observations towards Planck Galactic Cold Clumps (PGCCs) and future goals.

Meeting ID: 971 9800 9537
Passcode: 601756