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Shock-induced H2O masers are important magnetic field tracers at very highdensity gas. Water masers are found in both high- and low-mass star-formingregions, acting as a powerful tool to compare magnetic field morphologies inboth mass regimes. In this paper, we show one of the first magnetic fielddeterminations in the low-mass protostellar core IRAS 16293-2422 at volumedensities as high as 10^(8-10) cm^-3. Our goal is to discern if the collapsingregime of this source is controlled by magnetic fields or other factors liketurbulence. We used the Very Large Array (VLA) to carry outspectro-polarimetric observations in the 22 GHz Zeeman emission of H2O masers.From the Stokes V line profile, we can estimate the magnetic field strength inthe dense regions around the protostar. A blend of at least three maserfeatures can be inferred from our relatively high spatial resolution data set(~ 0.1"), which is reproduced in a clear non-Gaussian line profile. Theemission is very stable in polarization fraction and position angle across thechannels. The maser spots are aligned with some components of the complexoutflow configuration of IRAS 16293-2422, and they are excited in zones ofcompressed gas produced by shocks. The post-shock particle density is in therange of 1-3 x 10^9 cm^-3, consistent with typical water masers pumpingdensities. Zeeman emission is produced by a very strong line-of-sight magneticfield (B ~ 113 mG). The magnetic field pressure derived from our data iscomparable to the ram pressure of the outflow dynamics. This indicates that themagnetic field is energetically important in the dynamical evolution of IRAS16293-2422.

The magnetic field of IRAS 16293-2422 as traced by shock-induced H2O masers