The galaxy presents a distinct morphology, characterized by a disk-like structure viewed at an oblique angle. The spiral arms are well-defined, exhibiting a flocculent pattern with a loose winding. Two main spiral arms emanate from the central region.

The central bulge appears relatively small and indistinct, suggesting a lower concentration of older stars compared to the disk component.  No clear bar structure is observed within the galactic nucleus.

Evidence suggests a possible interaction or disturbance affecting the galaxy's morphology. The presence of irregularities in the spiral arm structure and potential tidal features, with the material being ejected, indicates a recent or ongoing gravitational interaction. This could be a minor merger with a smaller object, or a close encounter with a nearby galaxy.
