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We present high angular resolution dust polarization and molecular lineobservations carried out with the Atacama Large Millimeter/submillimeter Array(ALMA) toward the Class 0 protostar Serpens SMM1. By complementing theseobservations with new polarization observations from the Submillimeter Array(SMA) and archival data from the Combined Array for Research in Millimeter-waveAstronomy (CARMA) and the James Clerk Maxwell Telescopes (JCMT), we can comparethe magnetic field orientations at different spatial scales. We find majorchanges in the magnetic field orientation between large (~0.1 pc) scales --where the magnetic field is oriented E-W, perpendicular to the major axis ofthe dusty filament where SMM1 is embedded -- and the intermediate and smallscales probed by CARMA (~1000 AU resolution), the SMA (~350 AU resolution), andALMA (~140 AU resolution). The ALMA maps reveal that the redshifted lobe of thebipolar outflow is shaping the magnetic field in SMM1 on the southeast side ofthe source; however, on the northwestern side and elsewhere in the source, lowvelocity shocks may be causing the observed chaotic magnetic field pattern.High-spatial-resolution continuum and spectral-line observations also reveal atight (~130 AU) protobinary system in SMM1-b, the eastern component of which islaunching an extremely high-velocity, one-sided jet visible in both CO(2-1) andSiO(5-4); however, that jet does not appear to be shaping the magnetic field.These observations show that with the sensitivity and resolution of ALMA, wecan now begin to understand the role that feedback (e.g., from protostellaroutflows) plays in shaping the magnetic field in very young, star-formingsources like SMM1.

ALMA observations of dust polarization and molecular line emission from the Class 0 protostellar source Serpens SMM1