The galaxy presents a complex morphology, appearing to be in a state of interaction or merger. A dominant, relatively smooth central component is visible, elongated in shape, suggestive of either an elliptical galaxy or a disk galaxy viewed at a high inclination angle. There is evidence of tidal tails or other distortions emanating from the central body, indicating gravitational interaction with another object. 

The light distribution within the galaxy is not uniform. There is a distinct colour gradient, with the central regions appearing more yellow-red and the outer regions exhibiting a bluer hue. This suggests differences in stellar populations or dust content, potentially related to ongoing star formation in the outer regions triggered by the interaction. The light is highly concentrated in two distinct bright regions. 

The overall structure appears perturbed. It lacks a clear spiral arm structure, hinting that any pre-existing disk morphology has been disrupted. It is difficult to precisely assess the types of galaxies involved, but the disturbed morphology indicates a significant gravitational interaction. Further spectroscopic analysis will provide more details regarding the specific properties of the constituent stellar populations and gas dynamics, therefore giving insight into the merger history.
