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High resolution (sub-)millimeter polarization observations have opened a newera in the understanding of how B-fields are organized in star forming regions,unveiling an intricate interplay between the B-fields and the gas inprotostellar cores. However, to assess the role of the B-field in the processof solar-type star formation, it is key to be able to understand to what extentthese polarized dust emissions are good tracers of the B-field in the youngestprotostellar objects. We present a thorough investigation of the fidelity andlimitations of using dust polarized emission to map the B-field topologies inlow-mass protostars. To assess the importance of these effects, we performedthe analysis of B-field properties in 27 realizations of MHD models ofstar-forming cores. Assuming a uniform population of dust grains whose sizesfollow the standard MRN, we analyze the synthetic polarized dust emission mapsproduced if these grains align with the local B-field thanks to B-RATs. We findthat (sub-)millimeter polarized dust emission is a robust tracer of the B-fieldtopologies in inner protostellar envelopes and is successful at capturing thedetails of the B-field spatial distribution down to radii ~100 au. Measurementsof the los averaged B-field orientation using the polarized dust emission areprecise to < 15{\deg} in about 75 - 95% of the independent lines of sightpeering through protostellar envelopes. Large discrepancies between theintegrated B-field mean orientation and the orientation reconstructed from thepolarized dust emission are mostly observed in (i) lines of sight where theB-field is highly disorganized and (ii) lines of sight probing large columndensities. Our analysis shows that high opacity of the thermal dust emissionand low polarization fractions could be used to avoid utilizing the smallfraction of measurements affected by large errors.

Is the mm/submm dust polarization a robust tracer of the magnetic field topology in protostellar envelopes? A model exploration