The observed galaxy presents a flattened, disk-like morphology, indicative of a spiral or lenticular type. The galaxy is oriented approximately edge-on with respect to our line of sight. A bright, somewhat centrally concentrated bulge region is evident, appearing nearly spherical and containing a concentrated population of stars. The stellar population in the bulge appears older, as indicated by its relatively brighter emission in the redder bands of the spectrum.

Extending outwards from the bulge is a fainter, more diffuse disk. Traces of spiral arm structure may be present, although the near edge-on orientation makes it difficult to fully resolve them. The disk exhibits a bluer color compared to the bulge, suggesting a more active star formation. This color gradient could mean this disk contains younger stellar populations, particularly in the outer regions.

A slight asymmetry in the outer regions of the disk may indicate a potential interaction or tidal disturbance. Further investigation would be needed to confirm this hypothesis. Dust lanes appear to be present within the disk, absorbing and scattering light, which appear as darker patches superimposed against the stellar emission.
