On the origin of radio-loudness in active galactic nuclei using far-infrared polarimetric observations

TL;DR

This study provides the first evidence linking magnetic field strength and structure in AGN dust cores to their radio-loudness, suggesting magnetic fields play a key role in jet production and AGN classification.

Contribution

It demonstrates a clear difference in polarized dust emission between RL and RQ AGN and links magnetic field properties to jet power and radio-loudness.

Findings

RL AGN show significant polarized dust emission (5-11%), RQ AGN do not (<1%).

RL AGN have a toroidal magnetic field offset from the jet axis by ~65 degrees.

Magnetic fields are intrinsically related to jet power and AGN radio-loudness.

Abstract

The dichotomy between radio-loud (RL) and radio-quiet (RQ) active galactic nuclei (AGN) is thought to be intrinsically related to radio jet production. This difference may be explained by the presence of a strong magnetic field (B-field) that enhances, or is the cause of, the accretion activity and the jet power. Here, we report the first evidence of an intrinsic difference in the dust polarized emission cores of four RL and five RQ obscured AGN using 89 $\mu$m polarization with HAWC+/SOFIA. We find that the thermal polarized emission increases with the nuclear radio-loudness, $R_{20} = L_{\rm 5GHz}/ L_{\rm 20\mu m}$. The dust emission cores of RL AGN are measured to be polarized, $\sim5-11$%, while RQ AGN are unpolarized, $<1$%. For RQ AGN, our results are consistent with the observed region being filled with an unmagnetized or highly turbulent, disk and/or expanding outflow at scales of $5-130$ pc from the AGN. For RL AGN, the measured $89$ $\mu$m polarization arises primarily from magnetically aligned dust grains associated with a $5-130$ pc-scale dusty obscuring structure with a toroidal B-field orientation highly offset, $65\pm22^{\circ}$, with respect to the jet axis. Our results indicate that the size and strength of the B-fields surrounding the AGN are intrinsically related to the strength of the jet power -- the stronger the jet power is, the larger and stronger the toroidal B-field is. The detection of a $\le130$ pc-scale ordered toroidal B-field suggests that a) the infalling gas that fuels RL AGN is magnetized, b) there is a magnetohydrodynamic wind that collimates the jet, and/or c) the jet is able to magnetize its surroundings.