Origin and Evolution of the $\Omega$ Structure in the Head-Tail Radio Galaxy of Abell 3322

TL;DR

This study investigates the unique Omega-shaped head-tail galaxy in Abell 3322, revealing insights into jet dynamics, cosmic-ray aging, and shock interactions using multi-telescope radio observations.

Contribution

It provides the first detailed analysis of the Omega structure in a head-tail galaxy, linking jet morphology to shock waves and vortex formation.

Findings

Southern jet is brighter, likely due to Doppler boosting.

Radio spectrum steepens along the jet, indicating cosmic-ray aging.

Spectral index gradient suggests shock wave presence.

Abstract

A head-tail galaxy is thought to be a radio galaxy with bent active galactic nuclei (AGN) jets interacting with the intracluster medium (ICM). Study of head-tail galaxies provides us with fruitful insights into the mechanisms of shock waves and turbulence, as well as magnetic-field amplification and cosmic-ray acceleration. A recent MeerKAT observation revealed that a head-tail galaxy in the galaxy cluster, Abell 3322, exhibits a peculiar ``Omega" structure in its shape. In this paper, we investigated this Omega-tail galaxy using the upgraded Giant Meterwave Radio Telescope (GMRT) and the Australia Telescope Compact Array (ATCA). We found that the southern jet tends to be brighter than the northern jet, with a brightness ratio of about 2. This can be attributed to Doppler boost and the inclination of the jets. Our broadband data suggest that the radio spectrum becomes steeper along the jet propagation direction, and the cosmic-ray aging model with a weak reacceleration of cosmic rays is preferable to explain the index profile. We further found a gradient of the spectral index perpendicular to the jet propagation. We discussed the origin of the gradient and suggested that a shock wave along one side of the jets is present. The resultant ram pressure as well as the backflow made at the early stage of the jet may produce the tail component of this Omega-tail galaxy, while the observed Omega-shape structure is more likely due to a twin vortex seen in the low Reynolds number flow.