The nuclei are clearly visible in radiowaves and mid infrared, but the southern nucleus is hidden by dust lanes at the optical spectrum.

[8] There is evidence of an outflow of ionised gas from the northern nucleus[8] with shocks which is attributed to a superwind powered by the starburst.

[7] Based on observations by Spitzer Space Telescope, and Chandra X-ray Observatory, Ohyana et al. suggested that the southern nucleus of NGC 3256 is a heavily absorbed low luminosity active galactic nucleus, with X-ray spectrum consistent with a typical Compton-thin Seyfert 2 galaxy.

[7] Although NGC 3256 has seven large H II regions, a number small in comparison with other interacting galaxies, they are very luminous, with a total flux 85 times that of the Tarantula Nebula and they could host super star clusters.

In the eastern tail were also detected several young (< 10 Myr), low mass objects with strong nebular emission, indicating a small, recent burst of star formation.

The mean stellar population of the western tail was estimated to be 288+11−54 Myr and its light is dominated by stars formed after the interaction.