THE MAGNETIC FIELD and POLARIZATION PROPERTIES of RADIO GALAXIES in DIFFERENT ACCRETION STATES

We use the integrated polarized radio emission at 1.4 GHz (P1.4 GHz) from a large sample of active galactic nuclei (AGN; 796 sources at redshifts z <0.7) to study the large-scale magnetic field properties of radio galaxies in relation to the host galaxy accretion state. We find a fundamental difference in P1.4 GHz between radiative-mode AGN (i.e., high-excitation radio galaxies (HERGs) and radio-loud QSOs) and jet-mode AGN (i.e., low-excitation radio galaxies (LERGs)). While LERGs can achieve a wide range of P1.4 GHz (up to ≈30%), the HERGs and adioloud QSOs are limited to P1.4 GHz ≲15%. A difference in P1.4 GHz is also seen when the sample is divided at 0.5% of the total Eddington-scaled accretion rate, where the weakly accreting sources can attain higher values of P1.4 GHz. We do not find any clear evidence that this is driven by intrinsic magnetic field differences of the different radio morphological classes. Instead, we attribute the differences in P1.4 GHz to the local environments of the radio sources, in terms of both the ambient gas density and the magnetoionic properties of this gas. Thus, not only are different large-scale gaseous environments potentially responsible for the different accretion states of HERGs and LERGs, we argue that the large-scale magnetized environments may also be important for the formation of powerful AGN jets. Upcoming high angular resolution and broadband radio polarization surveys will provide the high-precision Faraday rotation measure and depolarization data required to robustly test this claim.