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The host galaxy of 3C 196.1 is a type-cDelliptical galaxy confirmed by near-infrared and optical imaging. It is described having an elongated structure from northeast and southwest direction with an estimated angular size of 3.16 kpc arcsec. According to optical color gradients of the host galaxy, 3C 196.1 exhibits periodic shells with the centroids of the optical isotopes having a directional shift towards southwest, indicating a merger stage. Furthermore, nucleus of the galaxy is partly obscured by interstellar dust and appears to be split in several patches of emission that is extended along the nucleus' direction.
Radio imaging of 3C 196.1 made by Very Large Array, shows a compact one-sided source within the host galaxy and a secondary nucleus on its side opposite its radio extension, measuring a total size of 16 kpc and an orientation along a position angle of 40°. The southwest side of the galaxy has an enshrouded radio lobe with the region displaying high recessional velocities that is exceeding 500 km s whereas the northwest side is more diffused with a small velocity dispersion.
According to X-ray and radio imaging analysis, 3C 196.1 has an butterfly-shaped X-ray cavity located 10 kpc from its nucleus with the inner and outer cavities having jet power of 1.9 x 10 erg s and 3.4 x 10 erg s respectively. The enthalpies of the inner and outer cavities are computed as 7 x 10 erg and 3 x 10 erg. Further evidence also shows presence of ionized gas filling up the cavity suggesting either the gas underwent numerous ionization events from AGN outbursts caused by the galaxy or the cooling of AGN outflows (10 < T ≤ 10 K) are causing the gas to form filaments.