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Although, from a theoretical point of view, magnetic fields are believed tohave a significant role during the early stages of star formation, especiallyduring the main accretion phase, the magnetic field strength and topology ispoorly constrained in the youngest accreting Class 0 protostars that lead tothe formation of solar-type stars. We carried out observations of the polarizeddust continuum emission with the SMA interferometer at 0.87mm, in order toprobe the structure of the magnetic field in a sample of 12 low-mass Class 0envelopes, including both single protostars and multiple systems, in nearbyclouds. Our SMA observations probe the envelope emission at scales of 600-5000au with a spatial resolution ranging from 600 to 1500 au depending on thesource distance. We report the detection of linearly polarized dust continuumemission in all of our targets, with average polarization fractions rangingfrom 2% to 10% in these protostellar envelopes. The polarization fractiondecreases with the continuum flux density, which translates into a decreasewith the H2 column density within an individual envelope. Our analysis showthat the envelope-scale magnetic field is preferentially observed eitheraligned or perpendicular to the outflow direction. Interestingly, our resultssuggest for the first time a relation between the orientation of the magneticfield and the rotational energy of envelopes, with a larger occurrence ofmisalignment in sources where strong rotational motions are detected athundreds to thousands of au scales. We also show that the best agreementbetween the magnetic field and outflow orientation is found in sources showingno small-scale multiplicity and no large disks at about 100 au scales.

SMA observations of the polarized dust emission in solar-type Class 0 protostars: the magnetic field properties at envelope scales