[2][3] An interacting pair of two vigorous starburst galaxies separated by ~1300 ± 200 km s−1 in velocity,[4] 4C +72.26 is known to have tight locus following in the K-band Hubble diagram, suggesting it as a luminous (~3L*) galaxy with stellar populations forming rapidly at a very high redshift and such, evolved passively.

Energy that is released from the continued accretion of material, is then fueled towards its central supermassive black hole.

[6][7] The molecular gas is known to end up between two colliding galaxies[8] which displays absorption line profiles like P Cygni, while the active galactic nucleus host shows Lyα emission that indicative of a galaxy-wide "superwind".

Despite showing a strong massive starburst, the ultraviolet-mid-infrared spectral energy distribution in 4C +72.26 is found to have a pre-existing stellar population that comprises ~1012 Msolar of stellar mass, with further ~2 per cent contributed by the current burst.

[4] 4C +72.26 is classfied as a broad absorption-line radio galaxy with strong mid-infrared continua observed through spectrograph observations from Spitzer Telescope,[11][12] according to research conducted by Dey in 1999,[13] similar to those of broad absorption-line quasars with C IV trough extending bluewards to ~7000 km s−1.