Abstract:

Star formation occurs through the collapse of dense cores embedded within molecular clouds. However, during this process, a significant fraction of the core material is dispersed by outflows and jets rather than incorporated into the protostars. Magnetic fields within dense cores may regulate the transfer of angular momentum from envelope to disk scales, thereby influencing the formation and evolution of protostellar disks. Class 0 protostars are particularly informative for studying the role of magnetic fields in star formation because they are in the earliest stages of stellar evolution, when most of the stellar mass is accumulated, and the protostar interacts most vigorously with its natal envelope through powerful outflows. The high angular resolution of the Atacama Large Millimeter/submillimeter Array (ALMA) has opened new opportunities to investigate magnetic fields in dense envelopes in unprecedented detail. I will talk about the ALMA Perseus Polarization Survey (ALPPS), which comprises 870 μm polarimetric observations toward 38 Class 0/I protostars in the Perseus molecular cloud at an angular resolution of ∼0′′.4. ALPPS reveals a diverse range of magnetic field morphologies across the observed sources. I will also show velocity distributions and protostellar outflows of the same sources, traced by C17O (3-2) and 12CO (3-2) lines, respectively. Although mostly Class 0, our results suggest that a few of the targets are relatively more evolved and show evidence of polarization due to self-scattering. In this talk, I will present summary results obtained from the ALPPS.