A Stratification in Magnetic Field Structures: The Radio Outflow in NGC 4151

The nature of radio outflows in radio-quiet AGN remains poorly understood. In this study, we present kpc-scale polarization observations of the Seyfert galaxy NGC,4151 using the Karl G. Jansky Very Large Array (VLA) in B-array at 3 and 10 GHz. We find that the inferred magnetic (B-) field structures show a stratification: a spine-sheath'-like structure, with fields perpendicular to the jet direction in the spine’ and parallel in the sheath', is observed in the higher resolution (0.5 arcsec) image at 10 GHz. In addition, a wind’-like component with B-fields perpendicular to the radio outflow is observed in the 3 GHz image (resolution 2 arcsec); this feature is prominent along the receding' (eastern) jet direction. Rotation measure (RM) ranges from $-230$ to 250 rad m$^{-2}$ over the polarized regions, indicating a low-electron-density ($10^{-2}-10^{-3}$ cm$^{-3}$) tenuous medium surrounding the source causing Faraday rotation. A {tentative} RM gradient of $+75$ to $-25$ rad m$^{-2}$ is observed transverse to the northern wind’ component, while a similar gradient with opposite sign is seen across the southern wind' component, suggestive of a helical magnetic field threading the outflow. Based on an analysis of the available radio and X-ray data, we conclude that the stratified radio outflow in NGC 4151 is magnetically-driven. The bi-conical radio wind’ is found to be massive ($1050-3200M_{\odot }$) with a high mass outflow rate ($0.01-0.03$ M${}_{\odot }$ yr${}^{-1}$) but low in kinetic power ($<0.01$% of L${}_{\mathrm{b}\mathrm{o}\mathrm{l}}$), making it less impactful for galactic-scale feedback. Our study suggests that radio-quiet AGN may also host magnetically dominant jets and winds, even while their jets are smaller and weaker compared to radio-loud AGN.