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The degree to which the formation and evolution of clouds and filaments inthe interstellar medium is regulated by magnetic fields remains an openquestion. Yet the fundamental properties of the fields (strength and 3Dmorphology) are not readily observable. We investigate the potential forrecovering magnetic field information from dust polarization, the Zeemaneffect, and the Faraday rotation measure ($RM$) in a SILCC-Zoommagnetohydrodynamic (MHD) filament simulation. The object is analyzed at theonset of star formation, and it is characterized by a line-mass of about M/L$\sim 63\ M_{\odot}\ pc^{-1}$ out to a radius of $1\,$pc and a kinked 3Dmagnetic field morphology. We generate synthetic observations via POLARISradiative transfer (RT) post-processing, and compare with an analytical modelof helical or kinked field morphology to help interpreting the inferredobservational signatures. We show that the tracer signals originate close tothe filament spine. We find regions along the filament where theangular-dependency with the line-of-sight (LOS) is the dominant factor and dustpolarization may trace the underlying kinked magnetic field morphology. We alsofind that reversals in the recovered magnetic field direction are notunambiguously associated to any particular morphology. Other physicalparameters, such as density or temperature, are relevant and sometimes dominantcompared to the magnetic field structure in modulating the observed signal. Wedemonstrate that the Zeeman effect and the $RM$ recover the line-of-sightmagnetic field strength to within a factor 2.1 - 3.4. We conclude that themagnetic field morphology may not be unambiguously determined in low-masssystems by observations of dust polarization, Zeeman effect, or $RM$, whereasthe field strengths can be reliably recovered.

monthly notices of the royal astronomical society

Magnetic fields in star-forming systems (II): examining dust  polarization, the Zeeman effect, and the Faraday rotation measure as magnetic  field tracers