3C 263 is classified as a Fanaroff-Riley Type II source.[5][6] It is also a steep spectrum[7] source with its radio structure best described as a double-lobed structure.[8] When imaged by Very Large Array, its lobes are asymmetrically placed and of unequal brightness. One lobe is described as jetted and the other as being relaxed. There is also a linear jet containing bright, elongated knots and a diffused emission region located 2 arcseconds from the hotspot region.[9] There is another weak component showing a flux density of 0.13 x 10-26 W m-2 Hz-1.[10]
Observations by Chandra X-ray Observatory, showed the compact component of the quasar is made up of several subcomponents; mainly an extended halo, a weak leading component and a bright central component with a flat two-point radio spectrum.[5] Parsec-scale observations showed the source as a core-jet structure with a bright nucleus. Based on results, its jet contains three knots which in turn projects out from the radio core by 2.5 mas.[11]
The nucleus of 3C 263 is found variable. It exhibits an variation amplitude that is greater than 40 mJy at 5 GHz. Superluminal motion was also detected inside its nucleus with evidence of parsec-scale jet components showing acceleration and nonradial motion. According to results, the inner jet component has a transverse velocity of 0.7h-1 c while the outer jet component has a velocity of 1.2-2.5 h-1 c.[3] Soft X-ray emission was also found surrounding the object with its luminosity calculated as 16.4 x 1043erg s-1.[12]
The host galaxy of 3C 263 is described as a flat-system according to Hubble Space Telescope. Based on observations, the host has an aligned major axis along the position angle of 350°. The absolute magnitude of the host is approximately 22.2.[13] Faint galaxies have also been found surrounding the object.[14] A multiphase absorption system was found at redshift (z) 0.32566 towards the object, showing detections of neon elements.[15][16]
^Porcas, R. W. (1986-01-01). "Compact Radio Structure of Quasars". Quasars; Proceedings of the IAU Symposium, Bangalore, India, Dec. 2-6, 1985. 119: 131.
