The galaxy presents as a slightly inclined spiral, displaying a centrally concentrated morphology with a prominent bulge. The bulge appears relatively smooth, and emits strongly across the observed color bands, indicating a population of older stars. Fainter spiral arms emanate from the bulge, exhibiting a moderately wound structure. These spiral arms are relatively diffuse, but suggest active star formation. There is no obvious bar structure. The overall color of the disk is somewhat bluer than the bulge, suggesting the presence of younger stellar populations in the outer regions. The light distribution indicates that the stellar density decreases gradually from the center outwards. There is no visible evidence of any major tidal disturbances or ongoing merger activity, but minor disturbances cannot be ruled out.
