The galaxy presents as an elongated structure with a prominent central bulge. The bulge appears to be composed of older stellar populations as indicated by its yellowish-orange color. Extending outwards from the bulge, we observe fainter, bluer regions suggesting the presence of ongoing star formation. These regions are not well-defined spiral arms, but rather irregular patches distributed asymmetrically around the central bulge. The overall shape can be approximated as a distorted disk, possibly exhibiting signs of tidal interactions or past mergers due to the asymmetric light distribution and disturbed morphology. The galaxy does not exhibit a strong degree of rotational symmetry. The edges of the galaxy fade into the background sky, indicative of a relatively large but diffuse halo of stars and gas. There may be possible evidence of disturbances that indicate the presence of merger activity.
