Radio Polarimetry of 3C119, 3C318, and 3C343 at milliarcsecond resolution

TL;DR

This study presents VLBA polarimetric observations of CSS sources 3C119, 3C318, and 3C343 at 5 and 8.4 GHz, revealing high and complex rotation measure values indicating dense gas interactions and magnetic field structures near their cores.

Contribution

It provides detailed milliarcsecond-scale RM measurements of CSS sources, highlighting the extreme and variable magnetic environments close to their cores and jets.

Findings

3C119 has RM up to ~10200 rad/m² near jet changes.

3C318's brightest component shows RM ~3030 rad/m².

3C343 exhibits complex RM > 6000 rad/m² near emission peaks.

Abstract

We report VLBA polarimetric observations of the CSS sources 3C119, 3C318, and 3C343 at 5 and 8.4 GHz. The CSS source 3C119 has source rest-frame RM values up to ~10200 rad/m**2 in a region which coincides with a change in the direction of the inner jet. This component is located ~325 pc from the core, which is variable and has a peaked radio spectrum. In the case of 3C318, a rest-frame RM of ~3030 rad/m**2 has been estimated for the brightest component which contributes almost all of the polarised emission. Further, two more extended components have been detected, clearly showing "wiggles" in the jet towards the southern side of the source. The CSS source 3C343 contains two peaks of emission and a curved jet embedded in more diffuse emission. It exhibits complex field directions near the emission peaks, which indicate rest-frame RM values in excess of ~6000 rad/m**2. The locations of the cores in 3C318 and 3C343 are not clear. The available data on mas-scale rest-frame RM estimates for CSS sources show that these have a wide range of values extending up to ~40000 rad/m**2 in the central region of OQ172, and could be located at projected distances from the core of up to ~1600 pc, as in 3C43 where this feature has a rest-frame RM of ~14000 rad/m**2. RM estimates for cores in core-dominated radio sources indicate that in addition to responding to an overall density gradient of the magneto-ionic medium, geometry, orientation and modes of fuelling may also play a significant role. In addition to these effects, the high values of RM in CSS sources are possibly due to dense clouds of gas interacting with the radio jets. The observed distortions in the radio structures of many CSS sources are consistent with this interpretation.